2742:, moving from WNL to WNE as more of the outer layers are lost, possibly reaching the WC or WO spectral class as carbon and oxygen from the triple alpha process reach the surface. This process would continue with heavier elements being fused until an iron core develops, at which point the core collapses and the star is destroyed. Subtle differences in initial conditions, in the models themselves, and most especially in the rates of mass loss, produce different predictions for the final state of the most massive stars. They may survive to become a helium-stripped star or they may collapse at an earlier stage while they retain more of their outer layers. The lack of sufficiently luminous WN stars and the discovery of apparent LBV supernova progenitors has also prompted the suggestion that certain types of LBVs explode as a supernova without evolving further.
2679:
1069:
1282:
1927:. The nebula is a prominent naked-eye object in the southern skies showing a complex mix of emission, reflection and dark nebulosity. Eta Carinae is known to be at the same distance as the Carina Nebula and its spectrum can be seen reflected off various star clouds in the nebula. The appearance of the Carina Nebula, and particularly of the Keyhole region, has changed significantly since it was described by John Herschel over 160 years ago. This is thought to be due to the reduction in ionising radiation from Eta Carinae since the Great Eruption. Prior to the Great Eruption the Eta Carinae system contributed up to 20% of the total ionising flux for the whole Carina Nebula, but that is now mostly blocked by the surrounding gas and dust.
1764:
1703:
1586:
2755:
2127:
1359:
2858:
1972:
2298:
2445:
1814:. There are multiple sources at various wavelengths right across the high energy electromagnetic spectrum: hard X-rays and gamma rays within 1 light-month of the Eta Carinae; hard X-rays from a central region about 3 light-months wide; a distinct partial ring "horse-shoe" structure in low-energy X-rays 0.67 parsec (2.2 light-years) across corresponding to the main shockfront from the Great Eruption; diffuse X-ray emission across the whole area of the Homunculus; and numerous condensations and arcs outside the main ring.
1908:
2666:
during the 19th century, light echoes observed in the 21st century give further information about the progression of the eruption, showing a brightening with multiple peaks for approximately 20 years, followed by a plateau period in the 1850s. The light echoes show that the outflow of material during the plateau phase was much higher than before the peak of the eruption. Possible explanations for the eruptions include: a binary merger in what was then a triple system; mass transfer from Eta
Carinae B during periastron passages; or a
2148:
2618:, suggesting strong accretion near periastron leading to a collapse of the secondary wind. It has been proposed that the initial brightening from 4th magnitude to 1st at relatively constant bolometric luminosity was a normal LBV outburst, albeit from an extreme example of the class. Then the companion star passing through the expanded photosphere of the primary at periastron triggered the further brightening, increase in luminosity, and extreme mass loss of the Great Eruption.
1297:
1230:
1511:
10783:
10831:
30:
2636:
10855:
2204:âand in a handful of other possible LBVs in other galaxies. None of them seem to be quite as violent as Eta Carinae's. It is unclear if this is something that only a very few of the most massive LBVs undergo, something that is caused by a close companion star, or a very brief but common phase for massive stars. Some similar events in external galaxies have been mistaken for supernovae and have been called
2212:
or spectral type of the underlying star actually is, and during its Great
Eruption it was much cooler than a typical LBV outburst, with a middle-G spectral type. The 1890 eruption may have been fairly typical of LBV eruptions, with an early F spectral type, and it has been estimated that the star may currently have an opaque stellar wind, forming a pseudo-photosphere with a temperature of 9,000â
10807:
10843:
10819:
1273:. Using direct focussing observations of the non-thermal source in the extremely hard X-ray band that is spatially coincident with the star, they showed that the source of non-thermal X-rays varies with the orbital phase of the binary star system and that the photon index of the emission is similar to that derived through analysis of the Îł-ray (gamma) spectrum.
2160:
still, possibly between 4.8 and 5.4 years. The orbital separation is only known approximately, with a semi-major axis of 15â16 AU. The orbit is highly eccentric, e = 0.9. This means that the separation of the stars varies from around 1.6 AU, similar to the distance of Mars from the Sun, to 30 AU, similar to the distance of
Neptune.
1091:, before fading slightly over the following three months. Herschel did not observe the star after this, but received correspondence from the Reverend W.S. Mackay in Calcutta, who wrote in 1843, "To my great surprise I observed this March last (1843), that the star Eta Argus had become a star of the first magnitude fully as bright as
2460:
the Eta
Carinae system consists of at least two stars, both with strong stellar winds and a shocked colliding wind (wind-wind collision or WWC) zone, embedded within a dusty nebula that reprocesses 90% of the electromagnetic radiation into the mid and far infrared. All of these features have different temperatures.
1493:, often multiple velocity components within the same line. The spectral lines also show variation over time, most strongly with a 5.5-year period but also less dramatic changes over shorter and longer periods, as well as ongoing secular development of the entire spectrum. The spectrum of light reflected from the
1217:
extinction due to the gas and dust ejected in the Great
Eruption. An unobscured brightness would have been magnitude 1.5â1.9, significantly brighter than the historical magnitude. Despite this, it was similar to the first one, even almost matching its brightness, but not the amount of material expelled.
3984:
Gull, Theodore R.; Hillier, D. John; Hartman, Henrik; Corcoran, Michael F.; Damineli, Augusto; Espinoza-Galeas, David; Hamaguchi, Kenji; Navarete, Felipe; Nielsen, Krister; Madura, Thomas; Moffat, Anthony F. J.; Morris, Patrick; Richardson, Noel D.; Russell, Christopher M. P.; Stevens, Ian R. (1 July
2651:
that the material indicating this eruption is actually from the Great
Eruption slowed down by colliding with older nebulosity. The mechanism producing these eruptions is unknown. It is not even clear whether the eruptions involve explosive events or so-called super-Eddington winds, an extreme form of
2650:
Two eruptions have been observed from Eta
Carinae, the Great Eruption of the mid-19th century and the Lesser Eruption of 1890. In addition, studies of outlying nebulosity suggest at least one earlier eruption around 1250 AD. A further eruption may have occurred around 1550 AD, although it is possible
2320:
Eta
Carinae A is losing a lot of mass due to its extreme luminosity and relatively low surface gravity. Its stellar wind is entirely opaque and appears as a pseudo-photosphere; this optically dense surface hides any true physical surface of the star that may be present. (At extreme rates of radiative
2211:
Eta Carinae A is not a typical LBV. It is more luminous than any other LBV in the Milky Way although possibly comparable to other supernova impostors detected in external galaxies. It does not currently lie on the S Doradus instability strip, although it is unclear what the temperature
1892:
and recombination lines vary very strongly, with continuum emission (electromagnetic radiation across a broad band of wavelengths) less affected. This shows a dramatic reduction in the ionisation level of the hydrogen for a short period in each cycle, coinciding with the spectroscopic events at other
1564:
In the second half of the 20th century, much higher-resolution visual spectra became available. The spectrum continued to show complex and baffling features, with much of the energy from the central star being recycled into the infrared by surrounding dust, some reflection of light from the star
1080:, who was in South Africa at the time, made a detailed series of accurate measurements in the 1830s showing that Eta Carinae consistently shone around magnitude 1.4 until November 1837. On the evening of 16 December 1837, Herschel was astonished to see that it had brightened to slightly outshine
6522:
Abdo, A.A.; Ackermann, M.; Ajello, M.; Allafort, A.; Baldini, L.; Ballet, J.; Barbiellini, G.; Bastieri, D.; Bechtol, K.; Bellazzini, R.; Berenji, B.; Blandford, R.D.; Bonamente, E.; Borgland, A.W.; Bouvier, A.; Brandt, T.J.; Bregeon, J.; Brez, A.; Brigida, M.; Bruel, P.; Buehler, R.; Burnett, T.H.;
4289:
Catalogus stellarum australium; sive, Supplementum catalogi
Tychenici, exhibens longitudines et latitudines stellarum fixarum, quae, prope polum Antarcticum sitae, in horizonte Uraniburgico Tychoni inconspicuae fuere, accurato calculo ex distantiis supputatas, & ad annum 1677 completum correctas
3122:
Richardson, Noel D.; Pablo, Herbert; Sterken, Christiaan; Pigulski, Andrzej; Koenigsberger, Gloria; Moffat, Anthony F. J.; Madura, Thomas I.; Hamaguchi, Kenji; Corcoran, Michael F.; Damineli, Augusto; Gull, Theodore R.; Hillier, D. John; Weigelt, Gerd; Handler, Gerald; Popowicz, Adam (1 April 2018).
2904:
supernova, which would result in a significant increase in UV radiation reaching Earth's surface from the Sun, but this would require a typical supernova to be closer than 50 light-years from Earth, and even a potential hypernova would need to be closer than Eta
Carinae. Another analysis of the
2820:
The existence of a massive companion brings many other possibilities. If Eta Carinae A was rapidly stripped of its outer layers, it might be a less massive WC- or WO-type star when core collapse was reached. This would result in a type Ib or type Ic supernova due to the lack of hydrogen and possibly
2720:
continues with further increases in size and luminosity, although hydrogen shell burning in chemically homogeneous stars may be very brief or absent since the entire star would become depleted of hydrogen. In the late stages of hydrogen burning, mass loss is extremely high due to the high luminosity
2459:
Until late in the 20th century, the temperature of Eta Carinae was assumed to be over 30,000 K because of the presence of high-excitation spectral lines, but other aspects of the spectrum suggested much lower temperatures and complex models were created to account for this. It is now known that
2435:
Following the Great Eruption, Eta Carinae became self-obscured by the ejected material, resulting in dramatic reddening. This has been estimated at four magnitudes at visual wavelengths, meaning the post-eruption luminosity was comparable to the luminosity when first identified. Eta Carinae is still
2002:
The lobes of the Homunculus are considered to be formed almost entirely due to the initial eruption, rather than shaped by or including previously ejected or interstellar material, although the scarcity of material near the equatorial plane allows some later stellar wind and ejected material to mix.
1576:
by one of the stars or due to passage within opaque portions of the complex stellar winds. Despite being ascribed to orbital rotation, these events vary significantly from cycle to cycle. These changes have become stronger since 2003 and it is generally believed that long-term secular changes in the
1055:
of 4 at the time of discovery, which has been calculated as magnitude 3.3 on the modern scale. The handful of possible earlier sightings suggest that Eta Carinae was not significantly brighter than this for much of the 17th century. Further sporadic observations over the next 70 years show
2626:
Rotation rates of massive stars have a critical influence on their evolution and eventual death. The rotation rate of the Eta Carinae stars cannot be measured directly because their surfaces cannot be seen. Single massive stars spin down quickly due to braking from their strong winds, but there are
2138:
that can be studied in great detail. Until recently Eta Carinae was thought to be the most massive single star, but the system's binary nature was proposed by the Brazilian astronomer Augusto Damineli in 1996 and confirmed in 2005. Both component stars are largely obscured by circumstellar material
1225:
Between 1900 and at least 1940, Eta Carinae appeared to have settled at a constant brightness of around magnitude 7.6, but in 1953 it was noted to have brightened again to magnitude 6.5. The brightening continued steadily, but with fairly regular variations of a few tenths of a magnitude.
2916:
Eta Carinae is not expected to produce a gamma-ray burst, and its axis is not currently aimed near Earth. The Earth's atmosphere protects its inhabitants from all the radiation apart from UV light (it is opaque to gamma rays, which have to be observed using space telescopes). The main effect would
2733:
helium fusion has started at the core of Eta Carinae A. The elemental abundances at the surface cannot be accurately measured, but ejecta within the Homunculus are around 60% hydrogen and 40% helium, with nitrogen enhanced to ten times solar levels. This is indicative of ongoing CNO cycle hydrogen
2526:
150 would be 35,200 K. The effective temperature of the visible outer edge of the opaque primary wind is generally treated as being 15,000â25,000 K on the basis of visual and ultraviolet spectral features assumed to be directly from the wind or reflected via the Weigelt Blobs. During the
2478:
In all other directions on the other side of the wind-wind collision zone, there is the wind from Eta Carinae A, cooler and around 100 times denser than Eta Carinae B's wind. It is also optically dense, completely obscuring anything resembling a true photosphere and rendering any definition of its
2408:
The most notable feature of Eta Carinae is its giant eruption or supernova impostor event, which originated in the primary star and was observed around 1843. In a few years, it produced almost as much visible light as a faint supernova explosion, but the star survived. It is estimated that at peak
6252:
Tavani, M.; Sabatini, S.; Pian, E.; Bulgarelli, A.; Caraveo, P.; Viotti, R. F.; Corcoran, M. F.; Giuliani, A.; Pittori, C.; Verrecchia, F.; Vercellone, S.; Mereghetti, S.; Argan, A.; Barbiellini, G.; Boffelli, F.; Cattaneo, P. W.; Chen, A. W.; Cocco, V.; d'Ammando, F.; Costa, E.; Deparis, G.; Del
2474:
The wind-wind collision cone separates the winds of the two stars. For 55â75° behind the secondary, there is a thin hot wind typical of O or WolfâRayet stars. This allows some radiation from Eta Carinae B to be detected and its temperature can be estimated with some accuracy due to spectral lines
2163:
Perhaps the most valuable use of an accurate orbit for a binary star system is to directly calculate the masses of the stars. This requires the dimensions and inclination of the orbit to be accurately known. The dimensions of Eta Carinae's orbit are only known approximately as the stars cannot be
4712:
Ishibashi, Kazunori; Gull, Theodore R.; Davidson, Kris; Smith, Nathan; Lanz, Thierry; Lindler, Don; Feggans, Keith; Verner, Ekaterina; Woodgate, Bruce E.; Kimble, Randy A.; Bowers, Charles W.; Kraemer, Steven; Heap, Sarah R.; Danks, Anthony C.; Maran, Stephen P.; Joseph, Charles L.; Kaiser, Mary
2665:
or more without destroying the star; the highly unusual shape and expansion rates of the ejected material; and the light curve during the eruptions involving a brightness increases of several magnitudes over a period of decades. The best-studied event is the Great Eruption. As well as photometry
2564:
The size of Eta Carinae A is not even well defined. It has an optically dense stellar wind, so the typical definition of a star's surface being approximately where it becomes opaque gives a very different result to where a more traditional definition of a surface might be. One study calculated a
2159:
The period of the orbit is accurately known at 5.539 years, although this has changed over time due to mass loss and accretion. Between the Great Eruption and the smaller 1890 eruption, the orbital period was apparently 5.52 years, while before the Great Eruption it may have been lower
2155:
The binary nature of Eta Carinae is clearly established, although the components have not been directly observed and cannot even be clearly resolved spectroscopically due to scattering and re-excitation in the surrounding nebulosity. Periodic photometric and spectroscopic variations prompted the
913:
Eta Carinae was first recorded as a fourth-magnitude star in the 16th or 17th century. It became the second-brightest star in the sky in the mid-19th century, before fading below naked-eye visibility. During the second half of the 20th century, it slowly brightened to again become visible to the
6818:
Wolk, Scott J.; Broos, Patrick S.; Getman, Konstantin V.; Feigelson, Eric D.; Preibisch, Thomas; Townsley, Leisa K.; Wang, Junfeng; Stassun, Keivan G.; King, Robert R.; McCaughrean, Mark J.; Moffat, Anthony F. J.; Zinnecker, Hans (2011). "The Chandra Carina Complex Project View of Trumpler 16".
2745:
Eta Carinae is a close binary and this complicates the evolution of both stars. Compact massive companions can strip mass from larger primary stars much more quickly than would occur in a single star, so the properties at core collapse can be very different. In some scenarios, the secondary can
1253:
A sudden doubling of brightness was observed in 1998â99 bringing it back to naked-eye visibility. During the 2014 spectroscopic event, the apparent visual magnitude became brighter than magnitude 4.5. The brightness does not always vary consistently at different wavelengths, and does not always
7960:
Pastorello, A.; Smartt, S.J.; Mattila, S.; Eldridge, J.J.; Young, D.; Itagaki, K.; Yamaoka, H.; Navasardyan, H.; Valenti, S.; Patat, F.; Agnoletto, I.; Augusteijn, T.; Benetti, S.; Cappellaro, E.; Boles, T.; Bonnet-Bidaud, J.-M.; Botticella, M.T.; Bufano, F.; Cao, C.; Deng, J.; Dennefeld, M.;
5068:
Hamaguchi, Kenji; Corcoran, Michael F; Pittard, Julian M; Sharma, Neetika; Takahashi, Hiromitsu; Russell, Christopher M. P; Grefenstette, Brian W; Wik, Daniel R; Gull, Theodore R; Richardson, Noel D; Madura, Thomas I; Moffat, Anthony F. J (2018). "Non-thermal X-rays from colliding wind shock
2436:
much brighter at infrared wavelengths, despite the presumed hot stars behind the nebulosity. The recent visual brightening is considered to be largely caused by a decrease in the extinction, due to thinning dust or a reduction in mass loss, rather than an underlying change in the luminosity.
1103:
indicated it peaked in brightness, surpassing Canopus, from 11 to 14 March 1843, then began to fade, then brightened to between the brightness of Alpha Centauri and Canopus between 24 and 28 March before fading once again. For much of 1844 the brightness was midway between Alpha Centauri and
1216:
A new brightening started in 1887, peaked at about magnitude 6.2 in 1892, then at the end of March 1895 faded rapidly to about magnitude 7.5. Although there are only visual records of the 1890 eruption, it has been calculated that Eta Carinae was suffering 4.3 magnitudes of visual
2470:
at the apex between the two stars. This zone is the source of the hard X-rays and gamma rays close to the stars. Near periastron, as the secondary ploughs through ever denser regions of the primary wind, the colliding wind zone becomes distorted into a spiral trailing behind Eta Carinae B.
9655:
2376:
The stars of the Eta Carinae system are completely obscured by dust and opaque stellar winds, with much of the ultraviolet and visual radiation shifted to infrared. The total electromagnetic radiation across all wavelengths for both stars combined is several million solar luminosities
1431:
lines are much weaker than the hydrogen lines, and the absence of He lines provides an upper limit to the possible temperature of the primary star. N lines can be identified but are not strong, while carbon lines cannot be detected and oxygen lines are at best very weak, indicating
2090:, and hence their distance from Earth. It is also necessary to know the amount of interstellar extinction to the cluster and this can be difficult in regions such as the Carina Nebula. A distance of 7,330 light-years (2,250 parsecs) has been determined from the calibration of
980:
a single set of Greek letter Bayer designations within his constellation Argo, and designated three areas within Argo for the purposes of using Latin letter designations three times over. Eta fell within the keel portion of the ship which was later to become the constellation
2546:
The size of the two main stars in the Eta Carinae system is difficult to determine precisely, for neither star can be seen directly. Eta Carinae B is likely to have a well-defined photosphere, and its radius can be estimated from the assumed type of star. An O supergiant of
1817:
All the high-energy emission associated with Eta Carinae varies during the orbital cycle. A spectroscopic minimum, or X-ray eclipse, occurred in July and August 2003, and similar events in 2009 and 2014 have been intensively observed. The highest-energy gamma rays above 100
2042:
The distance to Eta Carinae has been determined by several different methods, resulting in a widely accepted value of 2,330 parsecs (7,600 light-years), with a margin of error around 100 parsecs (330 light-years). The distance to Eta Carinae itself cannot be measured using
2305:
Mass loss is one of the most intensively studied aspects of massive star research. Put simply, calculated mass loss rates in the best models of stellar evolution do not reproduce the observed properties of evolved massive stars such as WolfâRayets, the number and types of
1056:
that Eta Carinae was probably around 3rd magnitude or fainter, until Lacaille reliably recorded it at 2nd magnitude in 1751. It is unclear whether Eta Carinae varied significantly in brightness over the next 50 years; there are occasional observations such as
2746:
accrue significant mass, accelerating its evolution, and in turn be stripped by the now compact WolfâRayet primary. In the case of Eta Carinae, the secondary is clearly causing additional instability in the primary, making it difficult to predict future developments.
2113:
The known expansion rate of the Homunculus Nebula provides an unusual geometric method for measuring its distance. Assuming that the two lobes of the nebula are symmetrical, the projection of the nebula onto the sky depends on its distance. Values of 2,300, 2,250 and
2139:
ejected from Eta Carinae A, and basic properties such as their temperatures and luminosities can only be inferred. Rapid changes to the stellar wind in the 21st century suggest that the star itself may be revealed when dust from the great eruption finally clears.
1447:
The earliest analyses of the star's spectrum are descriptions of visual observations from 1869, of prominent emission lines "C, D, b, F and the principal green nitrogen line". Absorption lines are explicitly described as not being visible. The letters refer to
8181:
van Boekel, R.; Kervella, P.; SchöLler, M.; Herbst, T.; Brandner, W.; de Koter, A.; Waters, L. B. F. M.; Hillier, D. J.; Paresce, F.; Lenzen, R.; Lagrange, A.-M. (2003). "Direct measurement of the size and shape of the present-day stellar wind of η Carinae".
2715:
As core hydrogen burning progresses, a very massive star would slowly expand and become more luminous, becoming a blue hypergiant and eventually an LBV while still fusing hydrogen in the core. When hydrogen at the core is depleted after 2â2.5 million years,
1565:
from dense localised objects in the circumstellar material, but with obvious high-ionisation features indicative of very high temperatures. The line profiles are complex and variable, indicating a number of absorption and emission features at various
2239:
The masses of stars are difficult to measure except by determination of a binary orbit. Eta Carinae is a binary system, but certain key information about the orbit is not known accurately. The mass can be strongly constrained to be greater than
3630:
Damineli, A.; Hillier, D.J.; Corcoran, M.F.; Stahl, O.; Levenhagen, R.S.; Leister, N.V.; Groh, J.H.; Teodoro, M.; Albacete Colombo, J.F.; Gonzalez, F.; Arias, J.; Levato, H.; Grosso, M.; Morrell, N.; Gamen, R.; Wallerstein, G.; Niemela, V. (2008).
9652:
2067:. This implies that Eta Carinae may be more distant than previously thought, and also more luminous, although it is still possible that it is not at the same distance as the cluster or that the parallax measurements have large systematic errors.
8879:
Ekström, S.; Georgy, C.; Eggenberger, P.; Meynet, G.; Mowlavi, N.; Wyttenbach, A.; Granada, A.; Decressin, T.; Hirschi, R.; Frischknecht, U.; Charbonnel, C.; Maeder, A. (2012). "Grids of stellar models with rotation. I. Models from 0.8 to
2345:
Eta Carinae B is presumably also losing mass via a thin, fast stellar wind, but this cannot be detected directly. Models of the radiation observed from interactions between the winds of the two stars show a mass loss rate of the order of
2342:. The bulk of the mass loss occurs in a wind with a terminal velocity of about 420 km/s, but some material is seen at higher velocities, up to 3,200 km/s, possibly material blown from the accretion disk by the secondary star.
1108:, around magnitude +0.2, before brightening again at the end of the year. At its brightest in 1843 it likely reached an apparent magnitude of â0.8, then â1.0 in 1845. The peaks in 1827, 1838 and 1843 are likely to have occurred at the
5524:
Prieto, J.L.; Rest, A.; Bianco, F.B.; Matheson, T.; Smith, N.; Walborn, N.R.; et al. (2014). "Light echoes from η Carinae's Great Eruption: Spectrophotometric evolution and the rapid formation of nitrogen-rich molecules".
1237:
In 1996, the variations were first identified as having a 5.52-year period, later measured more accurately at 5.54 years, leading to the idea of a binary system. The binary theory was confirmed by observations of radio, optical and
2321:
mass loss, the density gradient of lofted material may become continuous enough that a meaningfully discrete physical surface may not exist.) During the Great Eruption the mass loss rate was a thousand times higher, around 1
2832:
event in 2009 with similarities to Eta Carinae's Great Eruption, then an even brighter outburst in 2012 which is likely to have been a true supernova. SN 2006jc, some 77 million light-years away in UGC 4904, in the constellation
2222:
Eta Carinae B is a massive luminous hot star, about which little else is known. From certain high excitation spectral lines that ought not to be produced by the primary, Eta Carinae B is thought to be a young
8841:
Meynet, Georges; Georgy, Cyril; Hirschi, Raphael; Maeder, AndrĂ©; Massey, Phil; Przybilla, Norbert; Nieva, M.-Fernanda (2011). "Red Supergiants, Luminous Blue Variables and WolfâRayet stars: The single massive star perspective".
1998:
within the main nebula, probably formed by the 1890 eruption; a jet; fine streams and knots of material, especially noticeable in the skirt region; and three Weigelt Blobsâdense gas condensations very close to the star itself.
1746:
observations can penetrate the dust at high resolution to observe features that are completely obscured at visual wavelengths, although not the central stars themselves. The central region of the Homunculus contains a smaller
1349:
very close to Eta Carinae. Occurring from 14 to 28 January, the shower peaks around 21 January. Meteor showers are not associated with bodies outside the Solar System, making the proximity to Eta Carinae merely a coincidence.
5613:
Davidson, Kris; Ebbets, Dennis; Weigelt, Gerd; Humphreys, Roberta M.; Hajian, Arsen R.; Walborn, Nolan R.; Rosa, Michael (1995). "HST/FOS spectroscopy of eta Carinae: The star itself, and ejecta within 0.3 arcsec".
2627:
hints that both Eta Carinae A and B are fast rotators, up to 90% of critical velocity. One or both could have been spun up by binary interaction, for example accretion onto the secondary and orbital dragging on the primary.
2475:
that are unlikely to be produced by any other source. Although the secondary star has never been directly observed, there is widespread agreement on models where it has a temperature between 37,000 K and 41,000 K.
6468:
Hamaguchi, K.; Corcoran, M.F.; Gull, T.; Ishibashi, K.; Pittard, J.M.; Hillier, D.J.; Damineli, A.; Davidson, K.; Nielsen, K.E.; Kober, G.V. (2007). "X-Ray Spectral Variation of η Carinae through the 2003 X-Ray Minimum".
2186:
instability strip, with more luminous stars being hotter. In outburst all LBVs have about the same temperature, which is near 8,000 K. LBVs in a normal outburst are visually brighter than when quiescent although the
2725:
begins, massive stars transition very rapidly to the WolfâRayet stage with little or no hydrogen, increased temperatures and decreased luminosity. They are likely to have lost over half their initial mass at this point.
2686:
Eta Carinae is a unique object, with no very close analogues currently known in any galaxy. Therefore, its future evolution is highly uncertain, but almost certainly involves further mass loss and an eventual supernova.
2837:, also underwent a supernova impostor brightening in 2004, followed by a magnitude 13.8 type Ib supernova, first seen on 9 October 2006. Eta Carinae has also been compared to other possible supernova impostors such as
2029:
towards the poles. In contrast the spectrum shows a higher excitation temperature closer to the equatorial plane. By implication the outer envelope of Eta Carinae A is not strongly convective as that would prevent the
6576:
Abraham, Z.; Falceta-Gonçalves, D.; Dominici, T. P.; Nyman, L.-Ă
.; Durouchoux, P.; McAuliffe, F.; Caproni, A.; Jatenco-Pereira, V. (2005). "Millimeter-wave emission during the 2003 low excitation phase of η Carinae".
6523:
Caliandro, G.A.; Cameron, R.A.; Caraveo, P.A.; Carrigan, S.; Casandjian, J.M.; Cecchi, C.; Ăelik, Ă.; et al. (2010). "Fermi Large Area Telescope Observation of a Gamma-ray Source at the Position of Eta Carinae".
2583:, indicating an extended optically thick stellar wind. At the peak of the Great Eruption the radius, so far as such a thing is meaningful during such a violent expulsion of material, would have been around 1,400
5847:
Mehner, Andrea; Ishibashi, Kazunori; Whitelock, Patricia; Nagayama, Takahiro; Feast, Michael; van Wyk, Francois; de Wit, Willem-Jan (2014). "Near-infrared evidence for a sudden temperature increase in Eta Carinae".
4924:
Mehner, Andrea; Ishibashi, Kazunori; Whitelock, Patricia; Nagayama, Takahiro; Feast, Michael; Van Wyk, Francois; De Wit, Willem-Jan (2014). "Near-infrared evidence for a sudden temperature increase in Eta Carinae".
8288:
Corcoran, Michael F.; Ishibashi, Kazunori; Davidson, Kris; Swank, Jean H.; Petre, Robert; Schmitt, Jurgen H. M. M. (1997). "Increasing X-ray emissions and periodic outbursts from the massive star Eta Carinae".
2737:
Models of the evolution and death of single very massive stars predict an increase in temperature during helium core burning, with the outer layers of the star being lost. It becomes a WolfâRayet star on the
2034:. The current axis of rotation of the star does not appear to exactly match the alignment of the Homunculus. This may be due to interaction with Eta Carinae B which also modifies the observed stellar winds.
2530:
The Homunculus contains dust at temperatures varying from 150 K to 400 K. This is the source of almost all the infrared radiation that makes Eta Carinae such a bright object at those wavelengths.
4453:
Results of astronomical observations made during the years 1834, 5, 6, 7, 8, at the Cape of Good Hope: being the completion of a telescopic survey of the whole surface of the visible heavens, commenced in
1681:
emission from dense pockets surrounding many cool supergiant stars, but the latter effect is much weaker at optical and UV wavelengths and Eta Carinae is the only clear instance detected of an ultraviolet
2020:
A unique feature of the Homunculus is the ability to measure the spectrum of the central object at different latitudes by the reflected spectrum from different portions of the lobes. These clearly show a
1983:, a small emission and reflection nebula composed mainly of gas ejected during the Great Eruption event in the mid-19th century, as well as dust that condensed from the debris. The nebula consists of two
7565:
Mehner, A.; Davidson, K.; Humphreys, R.M.; Walter, F.M.; Baade, D.; de Wit, W.J.; et al. (2015). "Eta Carinae's 2014.6 spectroscopic event: Clues to the long-term recovery from its Great Eruption".
7961:
Elias-Rosa, N.; Harutyunyan, A.; Keenan, F.P.; Iijima, T.; Lorenzi, V.; Mazzali, P.A.; Meng, X.; Nakano, S.; et al. (2007). "A giant outburst two years before the core-collapse of a massive star".
5462:
Rest, A.; Prieto, J.L.; Walborn, N.R.; Smith, N.; Bianco, F.B.; Chornock, R.; et al. (2012). "Light echoes reveal an unexpectedly cool η Carinae during its nineteenth-century Great Eruption".
8611:
Khan, Rubab; Kochanek, C. S.; Stanek, K. Z.; Gerke, Jill (2015). "Finding η Car Analogs in Nearby Galaxies Using Spitzer. II. Identification of an Emerging Class of Extragalactic Self-Obscured Stars".
7370:
The, P. S.; Bakker, R.; Antalova, A. (1980). "Studies of the Carina Nebula. IV â A new determination of the distances of the open clusters TR 14, TR 15, TR 16 and CR 228 based on Walraven photometry".
1323:
Located between Canopus and the Southern Cross, Eta Carinae is easily pinpointed as the brightest star within the large naked-eye Carina Nebula. In a telescope the "star" is framed within the dark "V"
5657:
Davidson, Kris; Mehner, Andrea; Humphreys, Roberta; Martin, John C.; Ishibashi, Kazunori (2014). "Eta Carinae's 2014.6 spectroscopic event: The extraordinary He II and N II features".
1316:. Its brightness has varied over a wide range, from the second-brightest star in the sky for a few days in the 19th century, to well below naked-eye visibility. Its location at around 60°S in the far
807:
visibility after 1856. In a smaller eruption, it reached 6th magnitude in 1892 before fading again. It has brightened consistently since about 1940, becoming brighter than magnitude 4.5 by 2014.
5901:
Artigau, Ătienne; Martin, John C.; Humphreys, Roberta M.; Davidson, Kris; Chesneau, Olivier; Smith, Nathan (2011). "Penetrating the HomunculusâNear-Infrared Adaptive Optics Images of Eta Carinae".
1710:
Infrared observations of Eta Carinae have become increasingly important. The vast majority of the electromagnetic radiation from the central stars is absorbed by surrounding dust, then emitted as
8788:
Groh, Jose H.; Meynet, Georges; Georgy, Cyril; Ekström, Sylvia (2013). "Fundamental properties of core-collapse supernova and GRB progenitors: Predicting the look of massive stars before death".
6253:
Monte, E.; Di Cocco, G.; Donnarumma, I.; Evangelista, Y.; Ferrari, A.; Feroci, M.; Fiorini, M.; Froysland, T.; et al. (2009). "Detection of Gamma-Ray Emission from the Eta-Carinae Region".
4256:
Gould, Benjamin Apthorp (1879). "Uranometria Argentina: Brillantez Y posicion de las estrellas fijas, hasta la septima magnitud, comprendidas dentro de cien grados del polo austral: Con atlas".
2770:, very likely not even visible to the naked eye. Nevertheless, the prospect of a supernova originating from an object as extreme, nearby, and well studied as Eta Carinae arouses great interest.
7512:
Mehner, Andrea; Davidson, Kris; Humphreys, Roberta M.; Ishibashi, Kazunori; Martin, John C.; Ruiz, MarĂa Teresa; Walter, Frederick M. (2012). "Secular Changes in Eta Carinae's Wind 1998â2011".
2261:
for the primary and secondary, respectively. Higher masses have been suggested, to model the energy output and mass transfer of the Great Eruption, with a combined system mass of over 250
9000:; de Koter, A.; Langer, N.; Evans, C. J.; Gieles, M.; Gosset, E.; Izzard, R. G.; Le Bouquin, J.- B.; Schneider, F. R. N. (2012). "Binary Interaction Dominates the Evolution of Massive Stars".
2180:
is characterised by irregular changes from a high temperature quiescent state to a low temperature outburst state at roughly constant luminosity. LBVs in the quiescent state lie on a narrow
2051:
has provided the parallax for many stars considered to be members of Trumpler 16, finding that the four hottest O-class stars in the region have very similar parallaxes with a mean value of
5041:
Martin, John C.; Mehner, A.; Ishibashi, K.; Davidson, K.; Humphreys, R.M. (2014). "Eta Carinae's change of state: First new HST/NUV data since 2010, and the first new FUV since 2004".
7907:
Stockdale, Christopher J.; Rupen, Michael P.; Cowan, John J.; Chu, You-Hua; Jones, Steven S. (2001). "The fading radio emission from SN 1961v: evidence for a Type II peculiar supernova?".
2310:, or their progenitors. To match those observations, the models require much higher mass loss rates. Eta Carinae A has one of the highest known mass loss rates, currently around 10
3033:
HĂžg, E.; Fabricius, C.; Makarov, V.V.; Urban, S.; Corbin, T.; Wycoff, G.; Bastian, U.; Schwekendiek, P.; Wicenec, A. (2000). "The Tycho-2 catalogue of the 2.5 million brightest stars".
2017:. The results show that the material from the Great Eruption is strongly concentrated towards the poles; 75% of the mass and 90% of the kinetic energy were released above latitude 45°.
1572:
The 5.5-year orbital cycle produces strong spectral changes at periastron that are known as spectroscopic events. Certain wavelengths of radiation suffer eclipses, either due to actual
8493:
Smith, Nathan; Rest, Armin; Andrews, Jennifer E.; Matheson, Tom; Bianco, Federica B.; Prieto, Jose L.; James, David J.; Smith, R Chris; Strampelli, Giovanni Maria; Zenteno, A. (2018).
3513:
Mehner, A.; De Wit, W.-J.; Asmus, D.; Morris, P.W.; Agliozzo, C.; Barlow, M.J.; Gull, T.R.; Hillier, D.J.; Weigelt, G. (2019). "Mid-infrared evolution of η Carinae from 1968 to 2018".
2164:
directly and separately observed. The inclination has been modelled at 130â145 degrees, but the orbit is still not known accurately enough to provide the masses of the two components.
2913:
and increased risk of cancer and depression. It concludes that a supernova of this magnitude would have to be much closer than Eta Carinae to have any type of major impact on Earth.
1254:
exactly follow the 5.5 year cycle. Radio, infrared and space-based observations have expanded coverage of Eta Carinae across all wavelengths and revealed ongoing changes in the
7214:
Groh, J. H.; Madura, T. I.; Owocki, S. P.; Hillier, D. J.; Weigelt, G. (2010). "Is Eta Carinae a Fast Rotator, and How Much Does the Companion Influence the Inner Wind Structure?".
2789:. If there is still a large amount of expelled material close to the star, the shock formed by the supernova explosion impacting the circumstellar material can efficiently convert
9114:
McKinnon, Darren; Gull, T. R.; Madura, T. (2014). "Eta Carinae: An Astrophysical Laboratory to Study Conditions During the Transition Between a Pseudo-Supernova and a Supernova".
1474:. By 1895 the spectrum again consisted mostly of strong emission lines, with the absorption lines present but largely obscured by emission. This spectral transition from F
1869:(from the combining of an electron and proton to form a hydrogen atom) have been detected in this range. The emission is concentrated in a small non-point source less than 4
6030:
Becker, R. H.; Boldt, E. A.; Holt, S. S.; Pravdo, S. H.; Rothschild, R. E.; Serlemitsos, P. J.; Swank, J. H. (1976). "X-ray emission from the supernova remnant G287.8â0.5".
1470:
Photographic spectra from 1893 were described as similar to an F5 star, but with a few weak emission lines. Analysis to modern spectral standards suggests an early F
1246:, at the predicted time of periastron passage in late 1997 and early 1998. At the same time there was a complete collapse of the X-ray emission presumed to originate in a
3216:
Verner, E.; Bruhweiler, F.; Gull, T. (2005). "The Binarity of η Carinae Revealed from Photoionization Modeling of the Spectral Variability of the Weigelt Blobs B and D".
2094:
luminosities in Trumpler 16. After determining an abnormal reddening correction to the extinction, the distance to both Trumpler 14 and Trumpler 16 has been measured at
8664:
Yusof, Norhasliza; Hirschi, Raphael; Meynet, Georges; Crowther, Paul A.; Ekström, Sylvia; Frischknecht, Urs; Georgy, Cyril; Abu Kassim, Hasan; Schnurr, Olivier (2013).
2813:. The resulting remnant would be a black hole, for it is highly unlikely such a massive star could ever lose sufficient mass for its core not to exceed the limit for a
2821:
helium. This supernova type is thought to be the originator of certain classes of gamma-ray bursts, but models predict they occur only normally in less massive stars.
1718:
appropriate to the temperature of the dust. This allows almost the entire energy output of the system to be observed at wavelengths that are not strongly affected by
1335:
on either side of a bright central core. Variable star observers can compare its brightness with several 4th- and 5th-magnitude stars closely surrounding the nebula.
7424:
Hur, Hyeonoh; Sung, Hwankyung; Bessell, Michael S. (2012). "Distance and the Initial Mass Function of Young Open Clusters in the η Carina Nebula: Tr 14 and Tr 16".
9558:
Martin, Osmel; Cardenas, Rolando; Guimarais, Mayrene; Peñate, Liuba; Horvath, Jorge; Galante, Douglas (2010). "Effects of gamma ray bursts in Earth's biosphere".
6124:
Seward, F. D.; Forman, W. R.; Giacconi, R.; Griffiths, R. E.; Harnden, F. R.; Jones, C.; Pye, J. P. (1979). "X-rays from Eta Carinae and the surrounding nebula".
2655:
involving very high mass loss induced by an increase in the luminosity of the star. The energy source for the explosions or luminosity increase is also unknown.
1549:
events. Further light echo observations show that following the peak brightness of the Great Eruption the spectrum developed prominent P Cygni profiles and
7158:
Smith, Nathan; Davidson, Kris; Gull, Theodore R.; Ishibashi, Kazunori; Hillier, D. John (2003). "Latitude-dependent Effects in the Stellar Wind of η Carinae".
2268:
before the Great Eruption. Eta Carinae A has clearly lost a great deal of mass since it formed, and it is thought that it was initially 150â250
1250:. The confirmation of a luminous binary companion greatly modified the understanding of the physical properties of the Eta Carinae system and its variability.
1623:) and a continuum from a hot central source. The ionisation levels and continuum require the existence of a source with a temperature at least 37,000 K.
2391:
making it one of the most luminous stars in the Milky Way. The luminosity of Eta Carinae B is particularly uncertain, probably several hundred thousand
948:'s independent star catalogue from 1603 does not include Eta Carinae among the other 4th-magnitude stars in the region. The earliest firm record was made by
5954:
Hill, R. W.; Burginyon, G.; Grader, R. J.; Palmieri, T. M.; Seward, F. D.; Stoering, J. P. (1972). "A Soft X-Ray Survey from the Galactic Center to VELA".
1866:
985:. It was not generally known as Eta Carinae until 1879, when the stars of Argo Navis were finally given the epithets of the daughter constellations in the
8940:
Smith, Nathan; Conti, Peter S. (2008). "On the Role of the WNH Phase in the Evolution of Very Massive Stars: Enabling the LBV Instability with Feedback".
2335:
with much of it now forming the Homunculus Nebula. The smaller 1890 eruption produced the Little Homunculus Nebula, much smaller and only about 0.1
2156:
search for a companion, and modelling of the colliding winds and partial "eclipses" of some spectroscopic features have constrained the possible orbits.
1489:
The emission line spectrum associated with dense stellar winds has persisted ever since the late 19th century. Individual lines show widely varying
1076:
In 1827, Burchell specifically noted Eta Carinae's unusual brightness at 1st magnitude, and was the first to suspect that it varied in brightness.
2047:
due to its surrounding nebulosity, but other stars in the Trumpler 16 cluster are expected to be at a similar distance and are accessible to parallax.
4795:
Damineli, Augusto; Kaufer, Andreas; Wolf, Bernhard; Stahl, Otmar; Lopes, Dalton F.; de AraĂșjo, Francisco X. (2000). "Î Carinae: Binarity Confirmed".
1807:
8723:
Groh, Jose H.; Meynet, Georges; Ekström, Sylvia; Georgy, Cyril (2014). "The evolution of massive stars and their spectra. I. A non-rotating 60
4359:
Lost Stars: Lost, missing and troublesome stars from the catalogues of Johannes Bayer, Nicholas Louis de Lacaille, John Flamsteed, and sundry others
1200:
in Sydney showed that this was Eta Carinae during its Great Eruption in the 1840s. From 1857, the brightness decreased rapidly until it faded below
9692:
2805:, several times more luminous than a typical core collapse supernova and much longer-lasting. Highly massive progenitors may also eject sufficient
4897:
Humphreys, R. M.; Martin, J. C.; Mehner, A.; Ishibashi, K.; Davidson, K. (2014). "Eta Carinae â Caught in Transition to the Photometric Minimum".
9643:
2576:
150, near the sonic point or very approximately what might be called a physical surface. At optical depth 0.67 the radius would be over 800
1881:
region at around 10,000 K. High resolution imaging shows the radio frequencies originating from a disk a few arcseconds in diameter, 10,000
4287:
8122:
Madura, T. I.; Gull, T. R.; Okazaki, A. T.; Russell, C. M. P.; Owocki, S. P.; Groh, J. H.; Corcoran, M. F.; Hamaguchi, K.; Teodoro, M. (2013).
5578:
Davidson, K.; Dufour, R.J.; Walborn, N.R.; Gull, T.R. (1986). "Ultraviolet and visual wavelength spectroscopy of gas around Eta Carinae".
6362:
Pittard, J. M.; Corcoran, M. F. (2002). "In hot pursuit of the hidden companion of η Carinae: An X-ray determination of the wind parameters".
5342:
Walborn, N.R.; Liller, M.H. (1977). "The earliest spectroscopic observations of Eta Carinae and its interaction with the Carina Nebula".
4047:
Morris, Patrick W.; Gull, Theodore R.; Hillier, D. John; Barlow, M.J.; Royer, Pierre; Nielsen, Krister; Black, John; Swinyard, Bruce (2017).
5776:
Johansson, S.; Zethson, T. (1999). "Atomic Physics Aspects on Previously and Newly Identified Iron Lines in the HST Spectrum of η Carinae".
6415:
Weis, K.; Duschl, W. J.; Bomans, D. J. (2001). "High velocity structures in, and the X-ray emission from the LBV nebula around η Carinae".
2824:
Several unusual supernovae and impostors have been compared to Eta Carinae as examples of its possible fate. One of the most compelling is
1116:
orbit. From 1845 to 1856, the brightness decreased by around 0.1 magnitudes per year, but with possible rapid and large fluctuations.
5256:
Hillier, D.J.; Allen, D.A. (1992). "A spectroscopic investigation of Eta Carinae and the Homunculus Nebula. I â Overview of the spectra".
1740:) or more. This is much larger than previous estimates, and is all thought to have been ejected in a few years during the Great Eruption.
4049:"η Carinae's Dusty Homunculus Nebula from Near-infrared to Submillimeter Wavelengths: Mass, Composition, and Evidence for Fading Opacity"
2690:
Eta Carinae A would have begun life as an extremely hot star on the main sequence, already a highly luminous object over a million
1327:
of the nebula and appears distinctly orange and clearly non-stellar. High magnification will show the two orange lobes of a surrounding
926:
described a fourth-magnitude star at approximately the correct position around 1595â1596, which was copied onto the celestial globes of
7480:
Iping, R. C.; Sonneborn, G.; Gull, T. R.; Ivarsson, S.; Nielsen, K. (2005). "Searching for Radial Velocity Variations in eta Carinae".
2003:
Therefore, the mass of the lobes gives an accurate measure of the scale of the Great Eruption, with estimates ranging from 12â15
6191:
2658:
Theories about the various eruptions must account for: repeating events, at least three eruptions of various sizes; ejecting 20
1577:
stellar winds or previously ejected material may be the culmination of a return to the state of the star before its Great Eruption.
9061:
Adams, Scott M.; Kochanek, C. S.; Beacom, John F.; Vagins, Mark R.; Stanek, K. Z. (2013). "Observing the Next Galactic Supernova".
2785:, but at solar metallicity and above, there is expected to be sufficient mass loss before collapse to allow a visible supernova of
10920:
3701:"Constraining the absolute orientation of η Carinae's binary orbit: A 3D dynamical model for the broad [Fe III] emission"
1535:
9478:
Thomas, Brian; Melott, A.L.; Fields, B.D.; Anthony-Twarog, B.J. (2008). "Superluminous supernovae: No threat from Eta Carinae".
10925:
4133:"On the influence of the companion star in Eta Carinae: 2D radiative transfer modelling of the ultraviolet and optical spectra"
2667:
1527:
9255:
Smith, Nathan; Owocki, Stanley P. (2006). "On the Role of Continuum-driven Eruptions in the Evolution of Very Massive Stars".
3400:. Astrophysics and Space Science Library. Vol. 384. New York, NY: Springer Science & Business Media. pp. 26â27.
2881:). At 7,500 light-years from the star it is unlikely to directly affect terrestrial lifeforms, as they will be protected from
2208:, although this grouping may also include other types of non-terminal transients that approach the brightness of a supernova.
1004:
7295:
5760:
5240:
5213:
5188:
5178:
4411:
4394:
4366:
4240:
4207:
3421:
9685:
9424:
Ruderman, M. A. (1974). "Possible Consequences of Nearby Supernova Explosions for Atmospheric Ozone and Terrestrial Life".
2873:
A typical core collapse supernova at the distance of Eta Carinae would peak at an apparent magnitude around â4, similar to
1366:
7621:"3D radiative transfer simulations of Eta Carinae's inner colliding winds â I. Ionization structure of helium at apastron"
922:
There is no reliable evidence of Eta Carinae being observed or recorded before the 17th century, although Dutch navigator
2463:
The powerful stellar winds from the two stars collide in a roughly conical WWC zone and produce temperatures as high as
1888:
The radio emission from Eta Carinae shows continuous variation in strength and distribution over a 5.5-year cycle. The H
7680:"Luminous blue variables are antisocial: Their isolation implies that they are kicked mass gainers in binary evolution"
6954:
Abraham, Zulema; Falceta-Gonçalves, Diego; Beaklini, Pedro P.B. (2014). "ΠCarinae Baby Homunculus Uncovered by ALMA".
9635:
7042:
Gomez, H. L.; Vlahakis, C.; Stretch, C. M.; Dunne, L.; Eales, S. A.; Beelen, A.; Gomez, E. L.; Edmunds, M. G. (2010).
1787:
catalog. The earliest detection of X-rays in the Eta Carinae region was from the Terrier-Sandhawk rocket, followed by
9141:
Heger, A.; Fryer, C.L.; Woosley, S.E.; Langer, N.; Hartmann, D.H. (2003). "How Massive Single Stars End Their Life".
4856:
Ishibashi, K.; Corcoran, M. F.; Davidson, K.; Swank, J. H.; Petre, R.; Drake, S. A.; Damineli, A.; White, S. (1999).
3062:
3182:
Skiff, B.A. (2014). "VizieR Online Data Catalog: Catalogue of Stellar Spectral Classifications (Skiff, 2009â2014)".
2773:
As a single star, a star originally around 150 times as massive as the Sun would typically reach core collapse as a
1060:'s at 4th magnitude in 1815, but it is uncertain whether these are just re-recordings of earlier observations.
10890:
8235:
Martin, John C.; Davidson, Kris; Humphreys, Roberta M.; Mehner, Andrea (2010). "Mid-cycle Changes in Eta Carinae".
4506:
Hamacher, Duane W.; Frew, David J. (2010). "An Aboriginal Australian Record of the Great Eruption of Eta Carinae".
3354:
Ducati, J. R. (2002). "VizieR On-line Data Catalog: Catalogue of Stellar Photometry in Johnson's 11-color system".
2704:
and possibly much higher. A typical spectrum when first formed would be O2If and the star would be mostly or fully
1729:
Far infrared observations show a large mass of dust at 100â150 K, suggesting a total mass for the Homunculus of 20
8372:"Explosions triggered by violent binary-star collisions: Application to Eta Carinae and other eruptive transients"
8124:"Constraints on decreases in η Carinae's mass-loss from 3D hydrodynamic simulations of its binary colliding winds"
7270:
Walborn, Nolan R. (2012). "The Company Eta Carinae Keeps: Stellar and Interstellar Content of the Carina Nebula".
1538:. Analysis of the reflected spectra indicated the light was emitted when Eta Carinae had the appearance of a
10910:
10875:
10786:
9678:
2762:
The overwhelming probability is that the next supernova observed in the Milky Way will originate from an unknown
2534:
Further out, expanding gases from the Great Eruption collide with interstellar material and are heated to around
2071:
1270:
72:
4983:
Landes, H.; Fitzgerald, M. (2010). "Photometric observations of the η Carinae 2009.0 spectroscopic event".
1032:). Eta Carinae has the names Tseen She (from the Chinese ć€©ç€Ÿ "Heaven's altar") and Foramen. It is also known as
10709:
2900:
At least one paper has projected that complete loss of the Earth's ozone layer is a plausible consequence of a
2877:. A SLSN could be five magnitudes brighter, potentially the brightest supernova in recorded history (currently
2678:
1405:
but with the absorption wing much weaker than the emission. The broad P Cygni lines are typical of strong
6785:
Smith, N.; Brooks, K. J. (2008). "The Carina Nebula: A Laboratory for Feedback and Triggered Star Formation".
6083:
Forman, W.; Jones, C.; Cominsky, L.; Julien, P.; Murray, S.; Peters, G.; Tananbaum, H.; Giacconi, R. (1978).
3095:
Frew, David J. (2004). "The Historical Record of η Carinae. I. The Visual Light Curve, 1595â2000".
2930:
2194:
An event similar to Eta Carinae A's Great Eruption has been observed in only one other star in the
1389:
are highly variable, but there are a number of consistent distinctive features. The spectrum is dominated by
1317:
1068:
2025:
where the stellar wind is faster and stronger at high latitudes thought to be due to rapid rotation causing
1553:
molecular bands, although this is likely from the material being ejected which may have been colliding with
1531:
1365:
composite of Eta Carinae showing the unusual emission spectrum (near-IR image spectrum from the Hubble
10753:
8024:"Luminous blue variable eruptions and related transients: Diversity of progenitors and outburst properties"
4294:
3816:
Kashi, A.; Soker, N. (2010). "Periastron Passage Triggering of the 19th Century Eruptions of Eta Carinae".
2966:
2950:
2523:
1393:, usually broad although the higher excitation lines are overlaid by a narrow central component from dense
1255:
5125:
2697:. The exact properties would depend on the initial mass, which is expected to have been at least 150
10895:
9717:
4927:
2591:
2504:
with a temperature of between 20,000 K and 25,000 K at the time of its discovery by Halley. An
1723:
2739:
10797:
10254:
8022:
Smith, Nathan; Li, Weidong; Silverman, Jeffrey M.; Ganeshalingam, Mohan; Filippenko, Alexei V. (2011).
2782:
2712:
stars undergo such strong mixing that they remain chemically homogeneous during core hydrogen burning.
2416:. Other supernova impostors have been seen in other galaxies, for example the possible false supernova
2328:/year sustained for ten years or more. The total mass loss during the eruption was at least 10â20
2135:
1920:
1763:
1490:
1029:
880:, which consists of material ejected from the primary during the Great Eruption. It is a member of the
9640:
6817:
3987:"Eta Carinae: an evolving view of the central binary, its interacting winds and its foreground ejecta"
2497:. This pseudo-photosphere is observed to be elongated and hotter along the presumed axis of rotation.
9794:
3218:
2786:
2126:
2075:
1811:
1585:
1433:
969:
9312:; Pols, O. R.; Eldridge, J. J.; Baes, M. (2011). "Binary progenitor models of type IIb supernovae".
2188:
1308:
As a fourth-magnitude star, Eta Carinae is comfortably visible to the naked eye in all but the most
10244:
2722:
1494:
1440:
with some mixing to the surface. Perhaps the most striking feature is the rich Fe emission in both
1418:
1281:
3699:
Madura, T. I.; Gull, T. R.; Owocki, S. P.; Groh, J. H.; Okazaki, A. T.; Russell, C. M. P. (2012).
2717:
2604:
The stellar sizes should be compared with their orbital separation, which is only around 250
1702:
9712:
2798:
1346:
923:
902:
800:
3876:
Gull, T.R.; Damineli, A. (2010). "JD13 â Eta Carinae in the Context of the Most Massive Stars".
2986:
1208:
in the ejected material surrounding the star, rather than to an intrinsic change in luminosity.
741:
10915:
10905:
10885:
10180:
9701:
7101:
Smith, Nathan (2006). "The Structure of the Homunculus. I. Shape and Latitude Dependence from H
6693:
4451:
3573:"A revised historical light curve of Eta Carinae and the timing of close periastron encounters"
2639:
2448:
2353:/year at speeds of 3,000 km/s, typical of a hot O-class star. For a portion of the highly
2227:. Most authors suggest it is a somewhat evolved star such as a supergiant or giant, although a
2173:
1987:
aligned with the rotation axis of the star, plus an equatorial "skirt", the whole being around
1755:
of separate clumps and filaments from the two eruptions, and an elongated stellar wind region.
1719:
1594:
1526:
from the eruption reflected from other parts of the Carina Nebula were detected using the U.S.
1362:
1290:
990:
982:
842:
788:
716:
708:
704:
258:
148:
141:
85:
57:
50:
9625:. Facultad de Ciencias AstronĂłmicas y GeofĂsicas, Universidad Nacional de La Plata, Argentina.
7854:
Soker, Noam (2004). "Why a Single-Star Model Cannot Explain the Bipolar Nebula of η Carinae".
2905:
possible impact discusses more subtle effects from the unusual illumination, such as possible
1957:
association, an extended grouping of young luminous stars with a common motion through space.
1444:, with the forbidden lines arising from excitation of low density nebulosity around the star.
10900:
10880:
10629:
10445:
10017:
9664:
8554:"Was the nineteenth century giant eruption of Eta Carinae a merger event in a triple system?"
5230:
4232:
4225:
3184:
VizieR On-line Data Catalog: B/Mk. Originally Published in: Lowell Observatory (October 2014)
2709:
2505:
1262:
1247:
997:
700:
658:
565:
9581:
9335:
8910:
8811:
8753:
8332:
Chlebowski, T.; Seward, F. D.; Swank, J.; Szymkowiak, A. (1984). "X-rays from Eta Carinae".
8205:
7589:
7383:
7020:
6600:
6438:
6385:
6329:
5871:
5269:
5163:
4950:
4579:
4325:
3536:
3046:
9577:
9524:
9487:
9433:
9388:
9331:
9274:
9213:
9160:
9123:
9080:
9019:
8959:
8906:
8861:
8807:
8749:
8687:
8630:
8575:
8516:
8452:
8393:
8341:
8298:
8254:
8201:
8145:
8094:
8045:
7980:
7926:
7873:
7820:
7756:
7701:
7642:
7585:
7531:
7489:
7443:
7406:
7379:
7334:
7275:
7233:
7177:
7124:
7065:
7016:
6973:
6926:
6885:
6874:"The young open cluster NGC 3293 and its relation to CAR OB1 and the Carina Nebula complex"
6838:
6800:
6749:
6703:
6656:
6596:
6542:
6488:
6434:
6381:
6325:
6272:
6221:
6175:
6160:
6133:
6096:
6039:
6002:
5963:
5920:
5867:
5819:
5785:
5723:
5676:
5623:
5587:
5544:
5482:
5431:
5390:
5351:
5303:
5265:
5159:
5088:
5050:
5002:
4946:
4906:
4869:
4814:
4767:
4726:
4676:
4625:
4609:
4575:
4563:
4525:
4462:
4458:
4321:
4265:
4154:
4070:
4008:
3951:
3895:
3835:
3771:
3722:
3654:
3594:
3532:
3492:
3459:
3401:
3363:
3305:
3283:
3237:
3191:
3146:
3104:
3042:
2834:
2781:
with no visible explosion or a sub-luminous supernova, and a small fraction will produce a
2777:
within 3 million years. At low metallicity, many massive stars will collapse directly to a
2730:
2452:
2361:. During the Great Eruption of the primary, the secondary could have accreted several
2354:
1858:
1799:
1670:
1197:
1084:. This event marked the beginning of a roughly 18-year period known as the Great Eruption.
1020:
945:
443:
333:
9614:
9367:"SN 2009ip and SN 2010mc: Core-collapse Type IIn supernovae arising from blue supergiants"
3286:(2010). "High-excitation Emission Lines near Eta Carinae, and Its Likely Companion Star".
2479:
temperature moot. The observable radiation originates from a pseudo-photosphere where the
2247:, due to the high luminosity. Standard models of the system assume masses of 100â120
8:
10859:
10659:
2774:
2754:
2228:
2048:
1916:
1683:
1678:
1674:
1604:
spectrum of the Eta Carinae system shows many emission lines of ionised metals such as Fe
1441:
1410:
1378:
823:
815:
9528:
9491:
9437:
9392:
9278:
9217:
9164:
9127:
9084:
9023:
8963:
8865:
8691:
8634:
8579:
8520:
8456:
8397:
8345:
8302:
8258:
8149:
8098:
8049:
7984:
7930:
7877:
7824:
7760:
7705:
7646:
7619:
Clementel, N.; Madura, T. I.; Kruip, C. J. H.; Paardekooper, J.-P.; Gull, T. R. (2015).
7535:
7493:
7447:
7410:
7338:
7279:
7237:
7181:
7128:
7069:
6977:
6930:
6889:
6842:
6804:
6753:
6707:
6660:
6546:
6492:
6276:
6225:
6179:
6137:
6100:
6043:
6006:
5967:
5924:
5823:
5808:"Astrophysical laser operating in the O I 8446-Ă
line in the Weigelt blobs of η Carinae"
5789:
5727:
5680:
5627:
5591:
5548:
5486:
5435:
5394:
5355:
5307:
5092:
5054:
5006:
4910:
4873:
4818:
4771:
4730:
4680:
4629:
4529:
4466:
4269:
4158:
4074:
4012:
3955:
3899:
3839:
3775:
3726:
3658:
3598:
3496:
3463:
3405:
3367:
3309:
3241:
3195:
3150:
3108:
1630:
UV lines are unusually strong. These originate in the Weigelt Blobs and are caused by a
10847:
10835:
9593:
9567:
9540:
9514:
9457:
9406:
9378:
9347:
9321:
9290:
9264:
9237:
9203:
9176:
9150:
9096:
9070:
9043:
9009:
8975:
8949:
8922:
8896:
8851:
8823:
8797:
8765:
8739:
8705:
8677:
8646:
8620:
8593:
8565:
8534:
8506:
8470:
8442:
8411:
8383:
8314:
8270:
8266:
8244:
8217:
8191:
8163:
8135:
8063:
8035:
8004:
7970:
7942:
7916:
7889:
7863:
7836:
7810:
7801:
Kashi, A.; Soker, N. (2009). "Possible implications of mass accretion in Eta Carinae".
7780:
7746:
7719:
7691:
7660:
7632:
7601:
7575:
7547:
7521:
7459:
7433:
7352:
7324:
7249:
7245:
7223:
7193:
7167:
7140:
7114:
7083:
7055:
7007:
Weigelt, G.; Ebersberger, J. (1986). "Eta Carinae resolved by speckle interferometry".
6989:
6963:
6854:
6828:
6790:
6767:
6739:
6674:
6646:
6612:
6586:
6558:
6532:
6504:
6478:
6450:
6424:
6397:
6371:
6341:
6315:
6288:
6284:
6262:
6065:
5936:
5910:
5883:
5857:
5692:
5666:
5560:
5534:
5506:
5472:
5319:
5104:
5078:
5018:
4992:
4962:
4936:
4838:
4804:
4694:
4666:
4591:
4541:
4515:
4361:. Blacksburg, VA: The McDonald & Woodward Publishing Company. pp. 7â8, 82â85.
4172:
4144:
4106:
4093:
4060:
4048:
3998:
3911:
3885:
3851:
3825:
3740:
3712:
3672:
3644:
3612:
3584:
3548:
3522:
3321:
3295:
3253:
3227:
3136:
3125:"BRITE-Constellation reveals evidence for pulsations in the enigmatic binary η Carinae"
2829:
2508:
determined for the surface of a spherical optically thick wind at several hundred
2205:
2118:
have been derived for the Homunculus, and Eta Carinae is clearly at the same distance.
2079:
1554:
1546:
1414:
1072:
The lightcurve of Eta Carinae from some of the earliest observations to the current day
1052:
876:, around 30â80 times as massive as the Sun. The system is heavily obscured by the
792:
354:
220:
209:
198:
187:
176:
165:
117:
10249:
9092:
8642:
6554:
5932:
5688:
4537:
3847:
3783:
3317:
2682:
The recent lightcurve of Eta Carinae, with observations at standard wavelengths marked
10644:
9736:
9544:
9449:
9410:
9241:
9229:
9100:
9035:
8769:
8650:
8538:
8474:
8415:
8406:
8371:
8274:
8167:
8058:
8023:
7996:
7772:
7723:
7664:
7551:
7543:
7463:
7455:
7356:
7291:
7253:
7087:
7078:
7043:
7024:
6985:
6850:
6762:
6727:
6678:
6669:
6634:
6508:
6401:
6069:
5940:
5887:
5832:
5807:
5756:
5696:
5639:
5564:
5556:
5510:
5498:
5323:
5273:
5236:
5209:
5184:
5108:
5022:
4966:
4830:
4689:
4654:
4595:
4545:
4390:
4362:
4339:
4334:
4309:
4236:
4203:
4195:
4176:
4167:
4132:
4098:
4026:
3855:
3744:
3735:
3700:
3667:
3632:
3616:
3607:
3572:
3552:
3417:
3164:
3058:
2810:
2721:
and enhanced surface abundances of helium and nitrogen. As hydrogen burning ends and
2705:
2643:
2087:
2031:
2026:
1980:
1966:
1882:
1827:
1823:
1780:
1590:
1332:
1328:
1100:
1000:
965:
877:
696:
580:
473:
136:
68:
35:
9597:
9461:
9351:
9294:
9180:
9047:
8979:
8926:
8827:
8709:
8597:
8221:
8067:
7946:
7840:
7605:
7197:
7144:
6993:
6858:
6771:
6562:
6454:
6345:
6292:
4698:
4110:
3676:
3257:
2708:
due to CNO cycle fusion at the very high core temperatures. Sufficiently massive or
1726:. Eta Carinae is the brightest source in the night sky at mid-infrared wavelengths.
10811:
9585:
9532:
9441:
9396:
9339:
9282:
9221:
9168:
9088:
9027:
8967:
8914:
8815:
8757:
8695:
8638:
8583:
8524:
8460:
8401:
8349:
8318:
8306:
8262:
8209:
8153:
8102:
8053:
8008:
7988:
7934:
7893:
7881:
7828:
7784:
7764:
7709:
7650:
7593:
7539:
7451:
7397:
Walborn, N. R. (1995). "The Stellar Content of the Carina Nebula (Invited Paper)".
7342:
7283:
7241:
7185:
7132:
7073:
6981:
6934:
6893:
6846:
6757:
6664:
6616:
6604:
6550:
6496:
6442:
6389:
6333:
6280:
6229:
6183:
6141:
6104:
6055:
6047:
6010:
5971:
5928:
5875:
5827:
5731:
5684:
5631:
5595:
5552:
5490:
5439:
5398:
5359:
5311:
5096:
5010:
4954:
4877:
4842:
4822:
4775:
4734:
4684:
4633:
4583:
4533:
4329:
4162:
4088:
4078:
4016:
3959:
3915:
3903:
3843:
3779:
3730:
3662:
3602:
3540:
3467:
3409:
3325:
3313:
3245:
3154:
3050:
2998:
2921:. Eta Carinae is too far away to do that even if it did produce a gamma-ray burst.
2598:
2484:
2307:
2044:
1646:
1449:
1386:
1374:
1133:
1057:
811:
645:
552:
9629:
9445:
9343:
8918:
8819:
8761:
7597:
6306:
Leyder, J.-C.; Walter, R.; Rauw, G. (2008). "Hard X-ray emission from η Carinae".
5879:
5712:"Eta Carinae across the 2003.5 Minimum: Deciphering the Spectrum toward Weigelt D"
4958:
4422:
3544:
1358:
9774:
9754:
9659:
9647:
8213:
7832:
6608:
6446:
6393:
6337:
5291:
4587:
4490:
2866:
2480:
2368:, producing strong jets which formed the bipolar shape of the Homunculus Nebula.
1854:
1838:
1779:
sources have been detected around Eta Carinae, for example 4U 1037â60 in the 4th
1654:
1637:
effect. Ionised hydrogen between a blob and the central star generates intense Ly
1498:
1402:
1309:
977:
957:
931:
927:
834:
673:
429:
281:
156:
93:
8495:"Exceptionally fast ejecta seen in light echoes of Eta Carinae's Great Eruption"
7287:
2289:
for the secondary best-fit one-mass-transfer model of the Great Eruption event.
1421:
are present and strong, showing that Eta Carinae still retains much of its
10735:
10727:
10264:
10259:
7737:
Smith, Nathan (2008). "A blast wave from the 1843 eruption of η Carinae".
7347:
7312:
6728:"A census of the Carina Nebula â I. Cumulative energy input from massive stars"
4083:
4021:
3986:
2985:, where "I" indicates neutral elements, "II" singly ionized elements, etc. See
2790:
2767:
2594:
2358:
2297:
1984:
1874:
1722:, leading to estimates of the luminosity that are more accurate than for other
1566:
1522:
Direct spectral observations did not begin until after the Great Eruption, but
1088:
838:
765:
687:
402:
321:
309:
9589:
9536:
8107:
8082:
6939:
6914:
6015:
5990:
5100:
4780:
4755:
3907:
3487:
Wilson, Ralph Elmer (1953). "General catalogue of stellar radial velocities".
3413:
3054:
2176:(LBV) due to the distinctive spectral and brightness variations. This type of
1204:
visibility by 1886. This has been calculated to be due to the condensation of
10869:
10624:
10509:
9784:
9764:
9309:
8997:
7044:"Submillimetre variability of Eta Carinae: Cool dust within the outer ejecta"
7028:
5643:
5403:
5378:
5277:
4614:"η Carinae's Second Eruption and the Light Curves of the η Carinae Variables"
4447:
4343:
4283:
4191:
4030:
3168:
2886:
2573:
2515:
would be 9,400â15,000 K, while the temperature of a theoretical 60
2177:
2083:
1990:
1902:
1846:
1743:
1666:
1650:
1642:
1550:
1471:
1398:
1390:
1382:
1342:
1286:
1239:
1105:
1077:
949:
898:
888:
785:
769:
298:
253:
80:
9401:
9366:
9225:
9031:
8588:
8553:
8529:
8494:
8465:
8430:
8158:
8123:
7714:
7679:
7655:
7620:
6060:
5294:(1869). "On the nebulae of Argo and Orion, and on the spectrum of Jupiter".
4858:"Recurrent X-Ray Emission Variations of η Carinae and the Binary Hypothesis"
4715:"Discovery of a Little Homunculus within the Homunculus Nebula of η Carinae"
1012:
10823:
10544:
10434:
10395:
10390:
10385:
10380:
10375:
10370:
10007:
9972:
9962:
9957:
9952:
9947:
9942:
9932:
9927:
9922:
9917:
9907:
9902:
9897:
9892:
9882:
9769:
9749:
9453:
9233:
9039:
8700:
8665:
8000:
7776:
6234:
6209:
5502:
5315:
4834:
4102:
3159:
3124:
2982:
2970:
2954:
2814:
2652:
1942:
1715:
1711:
1631:
1613:
1428:
1406:
1339:
1313:
1124:
941:
895:
884:
819:
627:
600:
528:
497:
243:
232:
9670:
4131:
Groh, Jose H.; Hillier, D. John; Madura, Thomas I.; Weigelt, Gerd (2012).
1949:
is another extremely massive luminous star. Trumpler 16 and its neighbour
1320:
means it cannot be seen by observers in Europe and much of North America.
1229:
872:
emission. The secondary star is hot and also highly luminous, probably of
865:
in the astronomically near future. This is the only star known to produce
10766:
10539:
10534:
10529:
10415:
10299:
10294:
10289:
10274:
10002:
9997:
9992:
9987:
9982:
9779:
9269:
9155:
8196:
7975:
7921:
7868:
7274:. Astrophysics and Space Science Library. Vol. 384. pp. 25â27.
7172:
7119:
6744:
6651:
6591:
6483:
6429:
6376:
5235:. New York, New York: Springer Science & Business Media. p. 22.
5113:
4809:
4671:
3232:
2918:
2890:
2763:
2554:
with a temperature of 37,200 K has an effective radius of 23.6
2384:). The best estimate for the luminosity of the primary is 5 million
2224:
2091:
1950:
1936:
1601:
1573:
1510:
1483:
1205:
1127:, north-western Victoria, Australia, told of a reddish star they knew as
1113:
936:
881:
873:
866:
456:
262:
106:
7992:
7768:
5494:
2275:, although it may have formed through binary merger. Masses of 200
1242:
radial velocity and line profile changes, referred to collectively as a
1016:
10761:
10634:
10504:
10499:
10420:
10410:
10405:
10400:
10284:
10279:
9877:
9872:
9867:
9862:
9857:
9852:
9847:
9842:
9837:
9832:
9827:
6208:
Tsuboi, Yohko; Koyama, Katsuji; Sakano, Masaaki; Petre, Robert (1997).
2862:
2778:
2611:
at periastron. The accretion radius of the secondary is around 60
2501:
2466:
2301:
The Carina Nebula. Eta Carinae is the brightest star, on the left side.
1971:
1954:
1730:
1545:
G2-to-G5 supergiant, some 2,000 K cooler than expected from other
1523:
1515:
1503:
1475:
1463:. It is assumed that the final line is from Fe very close to the green
1394:
1301:
1109:
973:
956:(i.e. "following" relative to another star) within a new constellation
846:
777:
773:
607:
541:
504:
470:
340:
269:
9505:
Thomas, B.C. (2009). "Gamma-ray bursts as a threat to life on Earth".
4713:
Elizabeth; Linsky, Jeffrey L.; Roesler, Fred; Weistrop, Donna (2003).
2527:
great eruption, Eta Carinae A was much cooler at around 5,000 K.
2444:
1945:. All the other members are well below naked eye visibility, although
1497:, and assumed to originate mainly with the primary, is similar to the
841:
of 5.54 years. The primary is an extremely unusual star, similar to a
776:
greater than five million times that of the Sun, located around 7,500
10524:
10362:
10025:
9822:
9812:
9802:
6575:
3938:
Hillier, D. John; Davidson, K.; Ishibashi, K.; Gull, T. (June 2001).
3395:
2906:
2894:
2882:
2846:
2842:
2825:
2802:
2794:
2538:, producing less energetic X-rays seen in a horseshoe or ring shape.
2425:
2195:
2182:
1924:
1870:
1842:
1776:
1558:
1437:
1324:
1201:
862:
804:
799:, marking the start of its so-called "Great Eruption". It became the
9622:
6692:
White, S. M.; Duncan, R. A.; Chapman, J. M.; Koribalski, B. (2005).
5989:
Seward, F. D.; Page, C. G.; Turner, M. J. L.; Pounds, K. A. (1976).
5014:
3759:
2147:
10693:
10639:
10608:
10603:
10598:
10593:
10588:
10583:
10578:
10573:
10483:
10478:
10473:
10468:
10463:
10458:
10453:
10228:
10223:
10218:
10213:
10208:
10203:
10198:
10193:
10188:
10170:
10165:
10160:
10155:
10145:
10140:
10135:
10125:
10115:
10110:
10105:
10100:
10095:
10090:
10085:
10080:
10075:
10065:
10060:
10055:
10050:
10045:
10030:
9977:
9967:
9912:
9887:
9817:
9807:
9286:
9172:
8971:
8570:
8511:
8447:
8353:
7938:
7885:
7580:
7399:
Revista Mexicana de AstronomĂa y AstrofĂsica, Serie de Conferencias
7329:
7189:
7136:
6898:
6873:
6500:
6187:
6145:
6109:
6084:
6051:
5975:
5750:
5736:
5711:
5635:
5599:
5444:
5419:
5363:
5083:
4882:
4857:
4826:
4739:
4714:
4638:
4613:
4389:(in Chinese). ć°çŁæžæżćșçæéć
Źćž (Taiwan Book House Publishing Co., Ltd.).
4065:
4003:
3964:
3939:
3527:
3472:
3447:
3249:
3141:
2910:
2889:. The main damage would be restricted to the upper atmosphere, the
2838:
2483:
of the wind drops to near zero, typically measured at a particular
2429:
2421:
2417:
1826:
show strong variability, while lower-energy gamma rays observed by
1464:
1422:
1096:
1008:
680:
587:
9617:
NASA Missions Take an Unparalleled Look into Superstar Eta Carinae
9572:
9519:
9383:
9326:
9208:
9075:
9014:
8954:
8901:
8856:
8802:
8744:
8730:
star from the zero-age main sequence to the pre-supernova stage".
8682:
8625:
8431:"Ancient eruptions of η Carinae: A tale written in proper motions"
8388:
8310:
8249:
8140:
8040:
7815:
7751:
7696:
7637:
7526:
7438:
7228:
7060:
6968:
6833:
6795:
6537:
6320:
6267:
5915:
5862:
5671:
5539:
5477:
5126:"GIF of a computer simulation of the stellar winds of Eta Carinae"
4997:
4941:
4520:
4149:
3890:
3830:
3717:
3649:
3589:
3300:
2861:
One theory of Eta Carinae's ultimate fate is collapsing to form a
2857:
2130:
X-ray, optical and infrared images of Eta Carinae (26 August 2014)
10654:
10649:
10519:
10514:
10304:
10269:
10150:
10130:
10120:
10070:
10040:
10035:
9937:
9744:
5150:
Bortle, John E. (2001). "Introducing the Bortle Dark-Sky Scale".
2878:
2200:
1788:
1486:
and then the emission spectrum develops as it expands and thins.
1453:
1193:
1120:
1092:
803:
in the sky between 11 and 14 March 1843 before fading well below
9477:
8180:
7618:
7511:
6953:
6872:
Turner, D. G.; Grieve, G. R.; Herbst, W.; Harris, W. E. (1980).
6159:
Corcoran, M. F.; Rawley, G. L.; Swank, J. H.; Petre, R. (1995).
5846:
4923:
1296:
1087:
Eta Carinae was brighter still on 2 January 1838, equivalent to
10678:
10664:
10558:
10344:
10339:
10334:
10314:
10309:
8331:
7959:
2806:
2215:
1941:
Eta Carinae lies within the scattered stars of the Trumpler 16
1784:
1694:
emission has also been confirmed as an astrophysical UV laser.
1541:
1266:
781:
735:
665:
620:
572:
517:
345:
8878:
8287:
6467:
5900:
5612:
5067:
4896:
4855:
3281:
3121:
1413:
in this case because the central star is so heavily obscured.
29:
10329:
10324:
10319:
9557:
8551:
8234:
8021:
7564:
7311:
Davidson, Kris; Helmel, Greta; Humphreys, Roberta M. (2018).
6123:
5656:
5040:
3758:
Damineli, Augusto; Conti, Peter S.; Lopes, Dalton F. (1997).
2874:
2635:
2357:
orbit, it may actually gain material from the primary via an
1946:
1862:
1803:
1792:
1772:
1634:
1261:
In July 2018, Eta Carinae was reported to have the strongest
1081:
1007:
were created at the start of the 17th century. Together with
869:
827:
796:
720:
374:
39:
6691:
6251:
3937:
3629:
1907:
1873:
across and appears to be mainly free-free emission (thermal
1518:
caused by the Eta Carinae eruption in the Carina Nebula
1269:
satellite gave much higher resolution data than the earlier
1180:
1112:
passageâthe point the two stars are closest togetherâof the
9727:
6521:
5953:
5379:"Note on apparent changes in the spectrum of η CarinÊ"
5129:
4618:
The Publications of the Astronomical Society of the Pacific
2070:
The distances to star clusters can be estimated by using a
1479:
1417:
are present but relatively weak, indicating a clumpy wind.
1196:). In 2010, astronomers Duane Hamacher and David Frew from
1160:
1148:
712:
419:
325:
313:
54:
10818:
8663:
7479:
7157:
7048:
Monthly Notices of the Royal Astronomical Society: Letters
4711:
3983:
2865:âenergy released as jets along the axis of rotation forms
2758:
Supernovae types depending on initial mass and metallicity
1767:
X-rays around Eta Carinae (red is low energy, blue higher)
1482:, where ejected material initially radiates like a pseudo-
1142:
914:
naked eye, and by 2014 was again a fourth-magnitude star.
9365:
Smith, Nathan; Mauerhan, Jon C.; Prieto, Jose L. (2014).
9307:
9060:
8995:
8840:
8552:
Portegies Zwart, S. F.; Van Den Heuvel, E. P. J. (2016).
7041:
6082:
5577:
4258:
Resultados del Observatorio Nacional Argentino en Cordoba
2885:
by the atmosphere and from some other cosmic rays by the
2409:
brightness the luminosity was as high as 50 million
1841:
emissions have been observed from Eta Carinae across the
1819:
1662:
1645:
with a small admixture of other elements, including iron
1166:
1154:
1151:
8492:
8429:
Kiminki, Megan M.; Reiter, Megan; Smith, Nathan (2016).
8121:
6871:
6158:
5523:
4130:
3032:
1653:(where emission coincidentally has a suitable energy to
9140:
8787:
8722:
8610:
7310:
7213:
6207:
4794:
4290:... Accedit appendicula de rebus quibusdam astronomicis
4046:
3512:
2500:
Eta Carinae A is likely to have appeared as an early B
1915:
Eta Carinae is found within the Carina Nebula, a giant
1853:
line, but has been particularly closely studied in the
7906:
5988:
5461:
4608:
4412:"Activities of Exhibition and Education in Astronomy"
1641:
emission which penetrates the blob. The blob contains
964:
was published in 1679. The star was also known by the
10795:
6161:"First detection of x-ray variability of Eta Carinae"
6029:
4985:
Publications of the Astronomical Society of Australia
1177:
1169:
1139:
833:
The two main stars of the Eta Carinae system have an
9620:
6915:"The infrared spectrum and structure of Eta Carinae"
3698:
3215:
2134:
The Eta Carinae star system is currently one of the
1163:
1157:
1145:
968:
Eta Roboris Caroli, Eta Argus or Eta Navis. In 1751
894:
Although unrelated to the star and nebula, the weak
795:
star, it brightened in 1837 to become brighter than
9364:
7317:
Research Notes of the American Astronomical Society
5751:Vladilen Letokhov; Sveneric Johansson (June 2008).
5709:
3878:
Proceedings of the International Astronomical Union
3001:"D" usually refers to the sodium doublet; "d" or "D
1649:by radiation from the central stars. An accidental
1174:
1136:
10752:
9113:
8428:
7006:
5710:Nielsen, K. E.; Ivarsson, S.; Gull, T. R. (2007).
4381:
4224:
4189:
3940:"On the Nature of the Central Source in η Carinae"
3757:
3282:Mehner, Andrea; Davidson, Kris; Ferland, Gary J.;
1265:in the solar neighbourhood. Observations with the
1119:In their oral traditions, the Boorong clan of the
9371:Monthly Notices of the Royal Astronomical Society
8670:Monthly Notices of the Royal Astronomical Society
8558:Monthly Notices of the Royal Astronomical Society
8499:Monthly Notices of the Royal Astronomical Society
8435:Monthly Notices of the Royal Astronomical Society
8376:Monthly Notices of the Royal Astronomical Society
8128:Monthly Notices of the Royal Astronomical Society
8087:Monthly Notices of the Royal Astronomical Society
8028:Monthly Notices of the Royal Astronomical Society
7684:Monthly Notices of the Royal Astronomical Society
7625:Monthly Notices of the Royal Astronomical Society
7369:
6919:Monthly Notices of the Royal Astronomical Society
6732:Monthly Notices of the Royal Astronomical Society
6639:Monthly Notices of the Royal Astronomical Society
6628:
6626:
6214:Publications of the Astronomical Society of Japan
5995:Monthly Notices of the Royal Astronomical Society
5812:Monthly Notices of the Royal Astronomical Society
5805:
5383:Monthly Notices of the Royal Astronomical Society
5069:acceleration in the massive binary Eta Carinae".
4760:Monthly Notices of the Royal Astronomical Society
4659:Monthly Notices of the Royal Astronomical Society
4561:
4409:
4375:
4137:Monthly Notices of the Royal Astronomical Society
3705:Monthly Notices of the Royal Astronomical Society
3637:Monthly Notices of the Royal Astronomical Society
3577:Monthly Notices of the Royal Astronomical Society
3393:
3129:Monthly Notices of the Royal Astronomical Society
2398:and almost certainly no more than 1 million
1808:Advanced Satellite for Cosmology and Astrophysics
1233:Light curve for Eta Carinae between 1972 and 2019
10867:
9248:
8545:
6414:
6305:
5775:
4982:
4403:
854:, of which it has already lost at least 30
7900:
6361:
4557:
4555:
1994:long. Closer studies show many fine details: a
1979:Eta Carinae is enclosed by, and lights up, the
1877:) from ionised gas, consistent with a compact H
1706:Stars similar to Eta Carinae in nearby galaxies
1686:. A similar effect from pumping of metastable O
1300:Position of Eta Carinae (top left) compared to
996:Eta Carinae is too far south to be part of the
822:is 26°12âČS), and is not visible north of about
810:At declination â59° 41âČ 04.26âł, Eta Carinae is
10726:
8365:
8363:
7677:
7507:
7505:
7503:
7423:
6635:"Modelling the Radio Light Curve of η Carinae"
6623:
5061:
4293:. London: T. James. p. 13. Archived from
3394:Davidson, Kris; Humphreys, Roberta M. (2012).
2317:/year, and is an obvious candidate for study.
1798:More detailed observations were made with the
9686:
8488:
8486:
8484:
8074:
5341:
5036:
5034:
5032:
4849:
4602:
3811:
3809:
3807:
3805:
3803:
3801:
3799:
3797:
3795:
3793:
3508:
3506:
1677:to take place. This effect is similar to the
1039:
1033:
1023:
9665:ESO: Highest Resolution Image of Eta Carinae
8783:
8781:
8779:
7372:Astronomy and Astrophysics Supplement Series
7304:
6152:
5801:
5799:
5744:
5650:
5606:
5571:
5255:
5170:
4788:
4552:
4508:Journal of Astronomical History and Heritage
4505:
3875:
3751:
3623:
3566:
3564:
3562:
2852:
952:in 1677 when he recorded the star simply as
9700:
9254:
9194:Gal-Yam, A. (2012). "Luminous Supernovae".
8933:
8360:
8325:
8015:
7953:
7558:
7500:
7475:
7473:
7209:
7207:
6912:
6784:
6085:"The fourth Uhuru catalog of X-ray sources"
5769:
5716:The Astrophysical Journal Supplement Series
5420:"Eta Carinae. II. The Spectrum"
5284:
5249:
5203:
5197:
4568:Annual Review of Astronomy and Astrophysics
4566:(1997). "Eta Carinae and Its Environment".
4442:
4440:
4276:
4249:
3979:
3977:
3975:
3389:
3387:
3385:
3383:
3381:
3379:
3377:
3356:CDS/ADC Collection of Electronic Catalogues
2451:image of the Homunculus Nebula; inset is a
2172:Eta Carinae A is classified as a
1312:skies in inner-city areas according to the
111:â59° 41′ 04.26″
9693:
9679:
9473:
9471:
8939:
8666:"Evolution and fate of very massive stars"
8481:
7800:
7671:
7612:
7265:
7263:
6632:
6357:
6355:
6117:
6076:
6023:
5982:
5840:
5337:
5335:
5333:
5296:Proceedings of the Royal Society of London
5029:
4705:
3933:
3931:
3929:
3927:
3925:
3815:
3790:
3503:
3441:
3439:
3437:
3435:
3433:
3028:
3026:
3024:
3022:
2845:, and to superluminous supernovae such as
1953:are the two dominant star clusters of the
1885:(AU) wide at the distance of Eta Carinae.
16:Stellar system in the constellation Carina
10361:
9571:
9518:
9400:
9382:
9325:
9268:
9207:
9154:
9107:
9074:
9013:
8953:
8900:
8855:
8801:
8776:
8743:
8716:
8699:
8681:
8624:
8587:
8569:
8528:
8510:
8464:
8446:
8405:
8387:
8281:
8248:
8195:
8157:
8139:
8106:
8057:
8039:
7974:
7920:
7867:
7814:
7796:
7794:
7750:
7713:
7695:
7654:
7636:
7579:
7525:
7482:American Astronomical Society Meeting 207
7437:
7346:
7328:
7227:
7171:
7118:
7094:
7077:
7059:
6967:
6938:
6897:
6832:
6794:
6761:
6743:
6721:
6719:
6717:
6668:
6650:
6590:
6536:
6482:
6428:
6375:
6319:
6266:
6247:
6245:
6233:
6201:
6108:
6059:
6014:
5991:"X-ray sources in the southern Milky Way"
5914:
5861:
5831:
5796:
5735:
5670:
5538:
5476:
5443:
5402:
5376:
5370:
5222:
5082:
4996:
4978:
4976:
4940:
4881:
4808:
4779:
4753:
4747:
4738:
4688:
4670:
4637:
4519:
4333:
4183:
4166:
4148:
4092:
4082:
4064:
4042:
4040:
4020:
4002:
3963:
3889:
3829:
3734:
3716:
3694:
3692:
3690:
3688:
3686:
3666:
3648:
3633:"The periodicity of the η Carinae events"
3606:
3588:
3570:
3559:
3526:
3471:
3299:
3231:
3158:
3140:
3115:
2059:(mas), which translates to a distance of
71:J2000
9551:
9423:
9187:
8991:
8989:
8872:
8422:
8080:
7470:
7390:
7204:
7151:
6811:
5290:
5176:
5118:
4917:
4890:
4756:"Note on the brightening of Eta Carinae"
4612:; Davidson, Kris; Smith, Nathan (1999).
4492:Wergaia Community Grammar and Dictionary
4446:
4437:
3972:
3445:
3374:
3349:
3347:
3345:
3343:
3341:
3339:
3337:
3335:
3277:
3275:
3273:
3271:
3269:
3267:
3211:
3209:
3207:
3205:
2856:
2753:
2677:
2634:
2443:
2296:
2146:
2125:
1970:
1906:
1762:
1758:
1701:
1584:
1509:
1478:to strong emission is characteristic of
1357:
1295:
1280:
1228:
1067:
908:
9498:
9468:
9358:
9301:
9193:
8834:
8228:
8174:
7730:
7678:Smith, Nathan; Tombleson, Ryan (2015).
7396:
7272:Eta Carinae and the Supernova Impostors
7269:
7260:
7000:
6947:
6778:
6352:
5894:
5806:Johansson, S.; Letokhov, V. S. (2005).
5457:
5455:
5417:
5411:
5330:
4499:
4410:éłèŒæšș (Chen Huihua), ed. (28 July 2006).
4126:
4124:
4122:
4120:
3922:
3871:
3869:
3867:
3865:
3430:
3397:Eta Carinae and the Supernova Impostors
3019:
1536:Cerro Tololo Inter-American Observatory
917:
305:
42:at red and near-ultraviolet wavelengths
10868:
9504:
9417:
9134:
9054:
8657:
7791:
6906:
6865:
6714:
6242:
5517:
5149:
5143:
4973:
4655:"The systemic velocity of Eta Carinae"
4356:
4350:
4307:
4301:
4282:
4037:
3683:
3571:Smith, Nathan; Frew, David J. (2011).
3486:
3480:
3353:
3090:
3088:
3086:
3084:
3082:
3080:
3078:
3076:
3074:
3005:" was used for the nearby helium line.
2828:, a blue supergiant which underwent a
2749:
2082:of the stars, for example fitting the
1528:National Optical Astronomy Observatory
9674:
9507:International Journal of Astrobiology
8986:
8604:
8369:
7853:
7847:
7736:
7100:
7035:
6725:
6685:
6569:
6197:from the original on 10 October 2022.
5228:
4652:
4646:
4473:
4255:
4222:
4216:
3332:
3264:
3202:
3181:
2572:for a hot "core" of 35,000 K at
861:, and it is expected to explode as a
845:(LBV). It was initially 150â250
38:, surrounding Eta Carinae, imaged by
8844:Société Royale des Sciences de LiÚge
7417:
7313:"Gaia, Trumpler 16, and Eta Carinae"
6821:The Astrophysical Journal Supplement
6515:
6461:
6408:
6299:
5947:
5452:
5232:Meteor Showers: An Annotated Catalog
4488:
4117:
3862:
3760:"Eta Carinae: A long period binary?"
3448:"The 5.52 Year Cycle of Eta Carinae"
3175:
3094:
1507:which has a spectral type of B0Ieq.
1367:Space Telescope Imaging Spectrograph
1220:
830:, which is at a latitude of 30°2âČN.
9623:"Optical monitoring of Eta Carinae"
8887:at solar metallicity (Z = 0.014)".
8115:
7363:
5180:A Down to Earth Guide to the Cosmos
3071:
2455:NACO infrared image of Eta Carinae.
1975:A 3D model of the Homunculus Nebula
1491:widths, profiles and Doppler shifts
1095:, and in colour and size very like
1046:the Second Star of Sea and Mountain
317:
13:
7105:and Velocity Maps of η Carinae".
6700:The Fate of the Most Massive Stars
6210:"ASCA Observations of Eta Carinae"
5703:
4227:Star Names: Their Lore and Meaning
2086:or identifying features such as a
1845:band. It has been detected in the
1353:
1211:
14:
10937:
9608:
7216:The Astrophysical Journal Letters
6913:Aitken, D. K.; Jones, B. (1975).
6633:Kashi, Amit; Soker, Noam (2007).
6255:The Astrophysical Journal Letters
5527:The Astrophysical Journal Letters
4538:10.3724/SP.J.1440-2807.2010.03.06
2167:
1833:
1063:
814:from locations on Earth south of
10853:
10841:
10829:
10817:
10805:
10782:
10781:
8407:10.1111/j.1365-2966.2011.18607.x
8059:10.1111/j.1365-2966.2011.18763.x
7079:10.1111/j.1745-3933.2009.00784.x
6787:Handbook of Star Forming Regions
6763:10.1111/j.1365-2966.2006.10007.x
6670:10.1111/j.1365-2966.2007.11908.x
5833:10.1111/j.1365-2966.2005.09605.x
4690:10.1111/j.1365-2966.2004.07943.x
4448:Herschel, John Frederick William
4335:10.1046/j.1468-4004.2002.43225.x
4223:Allen, Richard Hinckley (1963).
4168:10.1111/j.1365-2966.2012.20984.x
3736:10.1111/j.1365-2966.2011.20165.x
3668:10.1111/j.1365-2966.2007.12815.x
3608:10.1111/j.1365-2966.2011.18993.x
3097:The Journal of Astronomical Data
2809:to cause a SLSN simply from the
1911:Annotated image of Carina Nebula
1657:the excited state) allows the Ly
1514:Animation showing the expanding
1132:
818:(for reference, the latitude of
28:
2992:
2975:
2959:
2943:
1896:
1557:in a similar way to a type IIn
1271:Fermi Gamma-ray Space Telescope
10921:Henry Draper Catalogue objects
10710:Carina Dwarf Spheroidal Galaxy
9667:including photos and animation
9560:Astrophysics and Space Science
8083:"On the Nature of Eta Carinae"
6702:. Vol. 332. p. 126.
6695:The Radio Cycle of Eta Carinae
4231:. Dover Publications. p.
2439:
1930:
1580:
1450:Fraunhofer's spectral notation
1188:"Old Woman Crow", the wife of
962:Catalogus Stellarum Australium
1:
10926:Bright Star Catalogue objects
9480:American Astronomical Society
9446:10.1126/science.184.4141.1079
9116:American Astronomical Society
5778:Eta Carinae at the Millennium
5043:American Astronomical Society
3784:10.1016/S1384-1076(97)00008-0
3452:Astrophysical Journal Letters
3012:
2931:Lists of astronomical objects
2897:and any astronauts in space.
2428:'s pre-explosion outburst in
2371:
2121:
1960:
1783:catalogue and 1044â59 in the
1467:line now known to be from O.
1442:permitted and forbidden lines
1338:Discovered in 1961, the weak
1318:southern celestial hemisphere
1276:
1003:, but it was mapped when the
1001:traditional Chinese astronomy
9314:Astronomy & Astrophysics
8889:Astronomy & Astrophysics
8790:Astronomy & Astrophysics
8732:Astronomy & Astrophysics
8267:10.1088/0004-6256/139/5/2056
7833:10.1016/j.newast.2008.04.003
7568:Astronomy & Astrophysics
7246:10.1088/2041-8205/716/2/L223
6285:10.1088/0004-637X/698/2/L142
5850:Astronomy & Astrophysics
4928:Astronomy & Astrophysics
4588:10.1146/annurev.astro.35.1.1
4487:"woman" lost in Stanbridge.
4421:(in Chinese). Archived from
4310:"Lacaille 250 years on"
3515:Astronomy & Astrophysics
2673:
2668:pulsational pair-instability
2630:
2292:
2282:for the primary and 90
1256:spectral energy distribution
549:(2.96 million â 4.1 million)
7:
9718:Carina in Chinese astronomy
9641:The 2003 Observing Campaign
9344:10.1051/0004-6361/201015410
9093:10.1088/0004-637X/778/2/164
8919:10.1051/0004-6361/201117751
8820:10.1051/0004-6361/201321906
8762:10.1051/0004-6361/201322573
8643:10.1088/0004-637X/799/2/187
7598:10.1051/0004-6361/201425522
7288:10.1007/978-1-4614-2275-4_2
6555:10.1088/0004-637X/723/1/649
5933:10.1088/0004-6256/141/6/202
5880:10.1051/0004-6361/201322729
5689:10.1088/2041-8205/801/1/L15
4959:10.1051/0004-6361/201322729
4384:Chinese horoscope mythology
4382:éłäč
é (Chen Jiu Jin) (2005).
3848:10.1088/0004-637X/723/1/602
3545:10.1051/0004-6361/201936277
3318:10.1088/0004-637X/710/1/729
2924:
2909:suppression with resulting
2646:which surrounds Eta Carinae
2621:
2072:HertzsprungâRussell diagram
2037:
1697:
1397:nebulosity, especially the
1051:Halley gave an approximate
1040:
905:very close to Eta Carinae.
10:
10942:
9621:FernĂĄndez-LajĂșs, Eduardo.
8214:10.1051/0004-6361:20031500
8184:Astronomy and Astrophysics
7544:10.1088/0004-637X/751/1/73
7456:10.1088/0004-6256/143/2/41
7009:Astronomy and Astrophysics
6986:10.1088/0004-637X/791/2/95
6851:10.1088/0067-0049/194/1/12
6609:10.1051/0004-6361:20041604
6579:Astronomy and Astrophysics
6447:10.1051/0004-6361:20000460
6417:Astronomy and Astrophysics
6394:10.1051/0004-6361:20020025
6364:Astronomy and Astrophysics
6338:10.1051/0004-6361:20078981
6308:Astronomy and Astrophysics
5755:. OUP Oxford. p. 39.
5557:10.1088/2041-8205/787/1/L8
5258:Astronomy and Astrophysics
5204:Ian Ridpath (1 May 2008).
3035:Astronomy and Astrophysics
2917:result from damage to the
2783:pair-instability supernova
2642:image showing the bipolar
2057:0.017 milliarcseconds
1964:
1934:
1900:
1751:from the 1890 eruption, a
10779:
10748:
10722:
10702:
10686:
10677:
10617:
10566:
10557:
10492:
10444:
10433:
10357:
10237:
10179:
10016:
9793:
9735:
9726:
9708:
9590:10.1007/s10509-009-0211-7
9537:10.1017/S1473550409004509
9257:The Astrophysical Journal
9143:The Astrophysical Journal
9063:The Astrophysical Journal
8942:The Astrophysical Journal
8613:The Astrophysical Journal
8334:The Astrophysical Journal
7856:The Astrophysical Journal
7514:The Astrophysical Journal
7160:The Astrophysical Journal
7107:The Astrophysical Journal
6956:The Astrophysical Journal
6525:The Astrophysical Journal
6471:The Astrophysical Journal
6168:The Astrophysical Journal
6126:The Astrophysical Journal
6089:The Astrophysical Journal
6032:The Astrophysical Journal
5956:The Astrophysical Journal
5659:The Astrophysical Journal
5580:The Astrophysical Journal
5424:The Astrophysical Journal
5344:The Astrophysical Journal
5101:10.1038/s41550-018-0505-1
4899:The Astronomer's Telegram
4862:The Astrophysical Journal
4797:The Astrophysical Journal
4754:Thackeray, A. D. (1953).
4053:The Astrophysical Journal
3991:The Astrophysical Journal
3944:The Astrophysical Journal
3908:10.1017/S1743921310009890
3818:The Astrophysical Journal
3414:10.1007/978-1-4614-2275-4
3288:The Astrophysical Journal
3219:The Astrophysical Journal
2969:2/3, near the top of the
2853:Possible effects on Earth
2191:luminosity is unchanged.
2010:up to as high as 45
1830:show little variability.
1812:Chandra X-ray Observatory
1499:extreme P Cygni-type
1415:Electron scattering wings
1045:
1034:
1024:
970:Nicolas-Louis de Lacaille
728:
695:Foramen, Tseen She,
693:
686:
593:
490:
485:
373:
369:
275:
268:
130:
65:
26:
9658:22 December 2019 at the
9636:X-ray Monitoring by RXTE
8237:The Astronomical Journal
7909:The Astronomical Journal
7426:The Astronomical Journal
7348:10.3847/2515-5172/aad63c
5903:The Astronomical Journal
5377:Baxandall, F.E. (1919).
4719:The Astronomical Journal
4413:
4386:
4314:Astronomy and Geophysics
4200:The practical astronomer
4084:10.3847/1538-4357/aa71b3
4022:10.3847/1538-4357/ac74c2
2936:
2893:, spacecraft, including
2308:core collapse supernovae
2142:
1724:extremely luminous stars
1667:pseudo-metastable states
1661:emission to pump the Fe
1532:Blanco 4-meter telescope
1019:, Eta Carinae forms the
10891:Luminous blue variables
9713:List of stars in Carina
9702:Constellation of Carina
9582:2010Ap&SS.326...61M
9336:2011A&A...528A.131C
9226:10.1126/science.1203601
9032:10.1126/science.1223344
8911:2012A&A...537A.146E
8812:2013A&A...558A.131G
8754:2014A&A...564A..30G
8206:2003A&A...410L..37V
8108:10.1093/mnras/154.4.415
7590:2015A&A...578A.122M
7384:1980A&AS...41...93T
7021:1986A&A...163L...5W
6940:10.1093/mnras/172.1.141
6601:2005A&A...437..977A
6439:2001A&A...367..566W
6386:2002A&A...383..636P
6330:2008A&A...477L..29L
6016:10.1093/mnras/177.1.13p
5872:2014A&A...564A..14M
5270:1992A&A...262..153H
5229:Kronk, Gary R. (2013).
5177:Thompson, Mark (2013).
5164:2001S&T...101b.126B
4951:2014A&A...564A..14M
4781:10.1093/mnras/113.2.237
4580:1997ARA&A..35....1D
4457:. Vol. 1. London:
4357:Wagman, Morton (2003).
4326:2002A&G....43b..25W
3537:2019A&A...630L...6M
3055:10.1888/0333750888/2862
3047:2000A&A...355L..27H
2981:The roman numerals are
2799:superluminous supernova
2710:differentially rotating
2541:
2234:
1795:, and Uhuru sightings.
1720:interstellar extinction
1291:constellation of Carina
1099:." Observations at the
887:within the much larger
355:Absolute magnitude
221:Apparent magnitude
210:Apparent magnitude
199:Apparent magnitude
188:Apparent magnitude
177:Apparent magnitude
137:Evolutionary stage
118:Apparent magnitude
10911:Durchmusterung objects
10876:Carina (constellation)
9653:AAVSO comparison chart
8370:Smith, Nathan (2011).
6726:Smith, Nathan (2006).
5404:10.1093/mnras/79.9.619
5316:10.1098/rspl.1869.0057
5208:. Dorling Kindersley.
4653:Smith, Nathan (2004).
4308:Warner, Brian (2002).
4202:. Dorling Kindersley.
2870:
2759:
2729:It is unclear whether
2718:hydrogen shell burning
2683:
2647:
2640:Hubble Space Telescope
2522:hydrostatic "core" at
2456:
2302:
2174:luminous blue variable
2152:
2131:
2100:1,000 light-years
1976:
1921:CarinaâSagittarius Arm
1912:
1768:
1707:
1597:
1555:circumstellar material
1519:
1370:
1363:Hubble Space Telescope
1305:
1293:
1234:
1073:
843:luminous blue variable
142:Luminous blue variable
58:Hubble Space Telescope
51:University of Colorado
10630:Finger of God Globule
10421:HD 95086 b (Levantes)
9646:19 March 2006 at the
9615:Goddard Media Studios
9402:10.1093/mnras/stt2269
8589:10.1093/mnras/stv2787
8530:10.1093/mnras/sty1479
8466:10.1093/mnras/stw2019
8159:10.1093/mnras/stt1871
8081:Davidson, K. (1971).
7715:10.1093/mnras/stu2430
7656:10.1093/mnras/stu2614
4610:Humphreys, Roberta M.
4564:Humphreys, Roberta M.
3446:Damineli, A. (1996).
3284:Humphreys, Roberta M.
2860:
2757:
2681:
2638:
2506:effective temperature
2447:
2300:
2231:cannot be ruled out.
2150:
2129:
2076:colourâcolour diagram
1974:
1910:
1766:
1759:High energy radiation
1705:
1589:Ultraviolet image of
1588:
1569:to the central star.
1513:
1434:core hydrogen burning
1361:
1299:
1284:
1232:
1071:
987:Uranometria Argentina
909:Observational history
801:second-brightest star
760:), formerly known as
8701:10.1093/mnras/stt794
6878:Astronomical Journal
6235:10.1093/pasj/49.1.85
5753:Astrophysical Lasers
5616:Astronomical Journal
5418:Gaviola, E. (1953).
4489:Reid, Julie (2008).
4483:, with the onset of
4459:Smith, Elder and Co.
3160:10.1093/mnras/sty157
2590:, comparable to the
1800:Einstein Observatory
1671:population inversion
1403:P Cygni profile
1401:. Most lines show a
1263:colliding wind shock
1198:Macquarie University
946:Frederick de Houtman
918:Discovery and naming
768:containing at least
10754:Astronomical events
9630:Eta Carinae profile
9529:2009IJAsB...8..183T
9492:2008AAS...212.0405T
9438:1974Sci...184.1079R
9432:(4141): 1079â1081.
9393:2014MNRAS.438.1191S
9279:2006ApJ...645L..45S
9218:2012Sci...337..927G
9165:2003ApJ...591..288H
9128:2014AAS...22340503M
9085:2013ApJ...778..164A
9024:2012Sci...337..444S
8964:2008ApJ...679.1467S
8866:2011BSRSL..80..266M
8692:2013MNRAS.433.1114Y
8635:2015ApJ...799..187K
8580:2016MNRAS.456.3401P
8521:2018MNRAS.480.1457S
8457:2016MNRAS.463..845K
8398:2011MNRAS.415.2020S
8346:1984ApJ...281..665C
8303:1997Natur.390..587C
8259:2010AJ....139.2056M
8150:2013MNRAS.436.3820M
8099:1971MNRAS.154..415D
8050:2011MNRAS.415..773S
7993:10.1038/nature05825
7985:2007Natur.447..829P
7931:2001AJ....122..283S
7878:2004ApJ...612.1060S
7825:2009NewA...14...11K
7769:10.1038/nature07269
7761:2008Natur.455..201S
7706:2015MNRAS.447..598S
7647:2015MNRAS.447.2445C
7536:2012ApJ...751...73M
7494:2005AAS...20717506I
7448:2012AJ....143...41H
7411:1995RMxAC...2...51W
7339:2018RNAAS...2..133D
7280:2012ASSL..384...25W
7238:2010ApJ...716L.223G
7182:2003ApJ...586..432S
7129:2006ApJ...644.1151S
7070:2010MNRAS.401L..48G
6978:2014ApJ...791...95A
6931:1975MNRAS.172..141A
6890:1980AJ.....85.1193T
6843:2011ApJS..194...12W
6805:2008hsf2.book..138S
6754:2006MNRAS.367..763S
6708:2005ASPC..332..126W
6661:2007MNRAS.378.1609K
6547:2010ApJ...723..649A
6493:2007ApJ...663..522H
6277:2009ApJ...698L.142T
6226:1997PASJ...49...85T
6180:1995ApJ...445L.121C
6138:1979ApJ...234L..55S
6101:1978ApJS...38..357F
6044:1976ApJ...209L..65B
6007:1976MNRAS.177P..13S
5968:1972ApJ...171..519H
5925:2011AJ....141..202A
5824:2005MNRAS.364..731J
5790:1999ASPC..179..171J
5728:2007ApJS..168..289N
5681:2015ApJ...801L..15D
5628:1995AJ....109.1784D
5592:1986ApJ...305..867D
5549:2014ApJ...787L...8P
5495:10.1038/nature10775
5487:2012Natur.482..375R
5436:1953ApJ...118..234G
5395:1919MNRAS..79..619B
5356:1977ApJ...211..181W
5308:1869RSPS...18..245L
5093:2018NatAs...2..731H
5055:2014AAS...22315109M
5007:2010PASA...27..374L
4911:2014ATel.6368....1H
4874:1999ApJ...524..983I
4819:2000ApJ...528L.101D
4772:1953MNRAS.113..237T
4731:2003AJ....125.3222I
4681:2004MNRAS.351L..15S
4630:1999PASP..111.1124H
4530:2010JAHH...13..220H
4481:gala-gala gurrk waa
4479:Or more accurately
4467:1847raom.book.....H
4297:on 6 November 2015.
4270:1879RNAO....1.....G
4159:2012MNRAS.423.1623G
4075:2017ApJ...842...79M
4013:2022ApJ...933..175G
3956:2001ApJ...553..837H
3900:2010HiA....15..373G
3840:2010ApJ...723..602K
3776:1997NewA....2..107D
3727:2012MNRAS.420.2064M
3659:2008MNRAS.384.1649D
3599:2011MNRAS.415.2009S
3497:1953GCRV..C......0W
3464:1996ApJ...460L..49D
3406:2012ASSL..384.....D
3368:2002yCat.2237....0D
3310:2010ApJ...710..729M
3242:2005ApJ...624..973V
3196:2014yCat....1.2023S
3151:2018MNRAS.475.5417R
3109:2004JAD....10....6F
2750:Potential supernova
2723:core helium burning
2206:supernova impostors
2080:absolute magnitudes
2049:Gaia Data Release 2
2027:gravity brightening
1917:star-forming region
1867:recombination lines
1684:astrophysical laser
1675:stimulated emission
1567:velocities relative
1385:in the Eta Carinae
1248:colliding wind zone
1244:spectroscopic event
1129:Collowgullouric War
729:Database references
644:<1 million
23:
10896:B-type hypergiants
10401:HD 63765 b (Yvaga)
9308:Claeys, J. S. W.;
4624:(763): 1124â1131.
4196:Mitton, Jacqueline
2871:
2830:supernova impostor
2760:
2684:
2648:
2565:radius of 60
2457:
2303:
2153:
2136:most massive stars
2132:
2116:2,300 parsecs
1977:
1913:
1883:astronomical units
1769:
1708:
1598:
1547:supernova impostor
1520:
1452:and correspond to
1371:
1306:
1294:
1235:
1074:
1053:apparent magnitude
1005:Southern Asterisms
972:gave the stars of
966:Bayer designations
715: 10431-5925,
688:Other designations
571:9,470â35,200
254:Variable type
166:Apparent magnitude
149:Spectral type
21:
10793:
10792:
10775:
10774:
10744:
10743:
10718:
10717:
10673:
10672:
10645:Homunculus Nebula
10553:
10552:
10429:
10428:
10353:
10352:
9202:(6097): 927â932.
7969:(7146): 829â832.
7745:(7210): 201â203.
7297:978-1-4614-2274-7
5762:978-0-19-156335-5
5471:(7385): 375â378.
5242:978-1-4614-7897-3
5215:978-1-4053-3620-8
5190:978-1-4481-2691-0
5152:Sky and Telescope
4396:978-986-7332-25-7
4368:978-0-939923-78-6
4242:978-0-486-21079-7
4209:978-1-4053-5620-6
3423:978-1-4614-2274-7
2811:radioactive decay
2797:, resulting in a
2740:nitrogen sequence
2644:Homunculus Nebula
2151:Eta Carinae orbit
2088:horizontal branch
2078:to calibrate the
2032:gravity darkening
1996:Little Homunculus
1981:Homunculus Nebula
1967:Homunculus Nebula
1806:X-ray telescope,
1749:Little Homunculus
1591:Homunculus Nebula
1409:, with very weak
1333:Homunculus Nebula
1329:reflection nebula
1221:Twentieth century
1101:Cape of Good Hope
878:Homunculus Nebula
784:) distant in the
756:, abbreviated to
747:
746:
308: â17.6
153:variable (LBV) +
36:Homunculus Nebula
10933:
10858:
10857:
10856:
10846:
10845:
10844:
10834:
10833:
10832:
10822:
10821:
10810:
10809:
10808:
10801:
10785:
10784:
10750:
10749:
10724:
10723:
10684:
10683:
10564:
10563:
10442:
10441:
10359:
10358:
9813:T (not variable)
9733:
9732:
9695:
9688:
9681:
9672:
9671:
9626:
9602:
9601:
9575:
9555:
9549:
9548:
9522:
9502:
9496:
9495:
9475:
9466:
9465:
9421:
9415:
9414:
9404:
9386:
9362:
9356:
9355:
9329:
9305:
9299:
9298:
9272:
9270:astro-ph/0606174
9252:
9246:
9245:
9211:
9191:
9185:
9184:
9158:
9156:astro-ph/0212469
9138:
9132:
9131:
9111:
9105:
9104:
9078:
9058:
9052:
9051:
9017:
8993:
8984:
8983:
8957:
8948:(2): 1467â1477.
8937:
8931:
8930:
8904:
8876:
8870:
8869:
8859:
8838:
8832:
8831:
8805:
8785:
8774:
8773:
8747:
8720:
8714:
8713:
8703:
8685:
8661:
8655:
8654:
8628:
8608:
8602:
8601:
8591:
8573:
8564:(4): 3401â3412.
8549:
8543:
8542:
8532:
8514:
8505:(2): 1457â1465.
8490:
8479:
8478:
8468:
8450:
8426:
8420:
8419:
8409:
8391:
8382:(3): 2020â2024.
8367:
8358:
8357:
8329:
8323:
8322:
8285:
8279:
8278:
8252:
8232:
8226:
8225:
8199:
8197:astro-ph/0310399
8178:
8172:
8171:
8161:
8143:
8119:
8113:
8112:
8110:
8078:
8072:
8071:
8061:
8043:
8019:
8013:
8012:
7978:
7976:astro-ph/0703663
7957:
7951:
7950:
7924:
7922:astro-ph/0104235
7904:
7898:
7897:
7871:
7869:astro-ph/0403674
7862:(2): 1060â1064.
7851:
7845:
7844:
7818:
7798:
7789:
7788:
7754:
7734:
7728:
7727:
7717:
7699:
7675:
7669:
7668:
7658:
7640:
7616:
7610:
7609:
7583:
7562:
7556:
7555:
7529:
7509:
7498:
7497:
7477:
7468:
7467:
7441:
7421:
7415:
7414:
7394:
7388:
7387:
7367:
7361:
7360:
7350:
7332:
7308:
7302:
7301:
7267:
7258:
7257:
7231:
7211:
7202:
7201:
7175:
7173:astro-ph/0301394
7155:
7149:
7148:
7122:
7120:astro-ph/0602464
7113:(2): 1151â1163.
7098:
7092:
7091:
7081:
7063:
7039:
7033:
7032:
7004:
6998:
6997:
6971:
6951:
6945:
6944:
6942:
6910:
6904:
6903:
6901:
6869:
6863:
6862:
6836:
6815:
6809:
6808:
6798:
6782:
6776:
6775:
6765:
6747:
6745:astro-ph/0601060
6723:
6712:
6711:
6689:
6683:
6682:
6672:
6654:
6652:astro-ph/0702389
6630:
6621:
6620:
6594:
6592:astro-ph/0504180
6573:
6567:
6566:
6540:
6519:
6513:
6512:
6486:
6484:astro-ph/0702409
6465:
6459:
6458:
6432:
6430:astro-ph/0012426
6412:
6406:
6405:
6379:
6377:astro-ph/0201105
6359:
6350:
6349:
6323:
6303:
6297:
6296:
6270:
6249:
6240:
6239:
6237:
6205:
6199:
6198:
6196:
6165:
6156:
6150:
6149:
6121:
6115:
6114:
6112:
6080:
6074:
6073:
6063:
6061:2060/19760020047
6027:
6021:
6020:
6018:
5986:
5980:
5979:
5951:
5945:
5944:
5918:
5898:
5892:
5891:
5865:
5844:
5838:
5837:
5835:
5803:
5794:
5793:
5773:
5767:
5766:
5748:
5742:
5741:
5739:
5707:
5701:
5700:
5674:
5654:
5648:
5647:
5610:
5604:
5603:
5575:
5569:
5568:
5542:
5521:
5515:
5514:
5480:
5459:
5450:
5449:
5447:
5415:
5409:
5408:
5406:
5374:
5368:
5367:
5339:
5328:
5327:
5302:(114â122): 245.
5288:
5282:
5281:
5253:
5247:
5246:
5226:
5220:
5219:
5201:
5195:
5194:
5183:. Random House.
5174:
5168:
5167:
5147:
5141:
5140:
5138:
5136:
5122:
5116:
5112:
5086:
5071:Nature Astronomy
5065:
5059:
5058:
5038:
5027:
5026:
5000:
4980:
4971:
4970:
4944:
4921:
4915:
4914:
4894:
4888:
4887:
4885:
4853:
4847:
4846:
4812:
4810:astro-ph/9912387
4803:(2): L101âL104.
4792:
4786:
4785:
4783:
4751:
4745:
4744:
4742:
4709:
4703:
4702:
4692:
4674:
4672:astro-ph/0406523
4650:
4644:
4643:
4641:
4606:
4600:
4599:
4562:Davidson, Kris;
4559:
4550:
4549:
4523:
4503:
4497:
4496:
4477:
4471:
4470:
4461:pp. 33â35.
4444:
4435:
4434:
4432:
4430:
4407:
4401:
4400:
4379:
4373:
4372:
4354:
4348:
4347:
4337:
4320:(2): 2.25â2.26.
4305:
4299:
4298:
4280:
4274:
4273:
4253:
4247:
4246:
4230:
4220:
4214:
4213:
4187:
4181:
4180:
4170:
4152:
4128:
4115:
4114:
4096:
4086:
4068:
4044:
4035:
4034:
4024:
4006:
3981:
3970:
3969:
3967:
3935:
3920:
3919:
3893:
3873:
3860:
3859:
3833:
3813:
3788:
3787:
3755:
3749:
3748:
3738:
3720:
3696:
3681:
3680:
3670:
3652:
3627:
3621:
3620:
3610:
3592:
3583:(3): 2009â2019.
3568:
3557:
3556:
3530:
3510:
3501:
3500:
3484:
3478:
3477:
3475:
3443:
3428:
3427:
3391:
3372:
3371:
3351:
3330:
3329:
3303:
3279:
3262:
3261:
3235:
3233:astro-ph/0502106
3213:
3200:
3199:
3179:
3173:
3172:
3162:
3144:
3135:(4): 5417â5423.
3119:
3113:
3112:
3092:
3069:
3068:
3030:
3006:
2996:
2990:
2979:
2973:
2963:
2957:
2947:
2867:gamma-ray bursts
2599:VY Canis Majoris
2537:
2496:
2495:
2491:
2485:Rossland opacity
2469:
2218:
2203:
2185:
2117:
2109:
2108:300 parsecs
2107:
2101:
2099:
2066:
2065:100 parsecs
2064:
2058:
2056:
1993:
1859:centimetre bands
1673:that allows the
1544:
1506:
1285:Eta Carinae and
1187:
1186:
1183:
1182:
1179:
1176:
1172:
1171:
1168:
1165:
1162:
1159:
1156:
1153:
1150:
1147:
1144:
1141:
1138:
1058:William Burchell
1047:
1043:
1037:
1036:
1030:Sea and Mountain
1027:
1026:
874:spectral class O
826:, just south of
772:with a combined
550:
526:
478:
434:
415:
413:
319:
307:
292:â125.0 km/s
160:
131:Characteristics
121:
101:
96:
66:Observation data
32:
24:
20:
10941:
10940:
10936:
10935:
10934:
10932:
10931:
10930:
10866:
10865:
10864:
10854:
10852:
10842:
10840:
10830:
10828:
10816:
10806:
10804:
10796:
10794:
10789:
10771:
10740:
10728:Galaxy clusters
10714:
10698:
10669:
10660:IGR J11014â6103
10613:
10549:
10488:
10436:
10425:
10349:
10233:
10194:63765 (Tapecue)
10175:
10012:
9789:
9750:ÎČ (Miaplacidus)
9722:
9704:
9699:
9660:Wayback Machine
9648:Wayback Machine
9611:
9606:
9605:
9556:
9552:
9503:
9499:
9476:
9469:
9422:
9418:
9363:
9359:
9306:
9302:
9253:
9249:
9192:
9188:
9139:
9135:
9112:
9108:
9059:
9055:
9008:(6093): 444â6.
8994:
8987:
8938:
8934:
8886:
8883:
8877:
8873:
8839:
8835:
8786:
8777:
8729:
8726:
8721:
8717:
8662:
8658:
8609:
8605:
8550:
8546:
8491:
8482:
8427:
8423:
8368:
8361:
8330:
8326:
8286:
8282:
8233:
8229:
8179:
8175:
8120:
8116:
8079:
8075:
8020:
8016:
7958:
7954:
7905:
7901:
7852:
7848:
7799:
7792:
7735:
7731:
7676:
7672:
7617:
7613:
7563:
7559:
7510:
7501:
7478:
7471:
7422:
7418:
7395:
7391:
7368:
7364:
7309:
7305:
7298:
7268:
7261:
7212:
7205:
7156:
7152:
7104:
7099:
7095:
7040:
7036:
7005:
7001:
6952:
6948:
6911:
6907:
6870:
6866:
6816:
6812:
6783:
6779:
6724:
6715:
6690:
6686:
6631:
6624:
6574:
6570:
6520:
6516:
6466:
6462:
6413:
6409:
6360:
6353:
6304:
6300:
6250:
6243:
6206:
6202:
6194:
6163:
6157:
6153:
6122:
6118:
6081:
6077:
6028:
6024:
5987:
5983:
5952:
5948:
5899:
5895:
5845:
5841:
5804:
5797:
5774:
5770:
5763:
5749:
5745:
5708:
5704:
5655:
5651:
5611:
5607:
5576:
5572:
5522:
5518:
5460:
5453:
5416:
5412:
5375:
5371:
5340:
5331:
5289:
5285:
5254:
5250:
5243:
5227:
5223:
5216:
5202:
5198:
5191:
5175:
5171:
5148:
5144:
5134:
5132:
5124:
5123:
5119:
5066:
5062:
5039:
5030:
5015:10.1071/AS09036
4981:
4974:
4922:
4918:
4895:
4891:
4854:
4850:
4793:
4789:
4752:
4748:
4710:
4706:
4651:
4647:
4607:
4603:
4560:
4553:
4504:
4500:
4478:
4474:
4445:
4438:
4428:
4426:
4415:
4408:
4404:
4397:
4388:
4380:
4376:
4369:
4355:
4351:
4306:
4302:
4281:
4277:
4254:
4250:
4243:
4221:
4217:
4210:
4188:
4184:
4129:
4118:
4045:
4038:
3982:
3973:
3936:
3923:
3874:
3863:
3814:
3791:
3756:
3752:
3697:
3684:
3628:
3624:
3569:
3560:
3511:
3504:
3485:
3481:
3444:
3431:
3424:
3392:
3375:
3352:
3333:
3280:
3265:
3214:
3203:
3180:
3176:
3120:
3116:
3093:
3072:
3065:
3031:
3020:
3015:
3010:
3009:
3004:
2997:
2993:
2980:
2976:
2964:
2960:
2953:155, below the
2948:
2944:
2939:
2927:
2855:
2775:WolfâRayet star
2752:
2703:
2700:
2696:
2693:
2676:
2664:
2661:
2633:
2624:
2617:
2614:
2610:
2607:
2595:red supergiants
2589:
2586:
2582:
2579:
2571:
2568:
2560:
2557:
2553:
2550:
2544:
2535:
2521:
2518:
2514:
2511:
2493:
2489:
2488:
2481:optical density
2464:
2442:
2415:
2412:
2404:
2401:
2397:
2394:
2390:
2387:
2383:
2380:
2374:
2367:
2364:
2352:
2349:
2341:
2338:
2334:
2331:
2327:
2324:
2316:
2313:
2295:
2288:
2285:
2281:
2278:
2274:
2271:
2267:
2264:
2260:
2257:
2254:and 30â60
2253:
2250:
2246:
2243:
2237:
2229:WolfâRayet star
2213:
2199:
2181:
2170:
2145:
2124:
2115:
2105:
2103:
2097:
2095:
2062:
2060:
2054:
2052:
2040:
2016:
2013:
2009:
2006:
1988:
1969:
1963:
1939:
1933:
1905:
1899:
1891:
1880:
1852:
1836:
1761:
1739:
1736:
1700:
1693:
1689:
1660:
1643:atomic hydrogen
1640:
1629:
1622:
1618:
1611:
1607:
1583:
1539:
1502:
1462:
1459:, He, Fe, and H
1457:
1356:
1354:Visual spectrum
1279:
1223:
1214:
1212:Lesser Eruption
1173:
1135:
1131:
1066:
978:Robur Carolinum
958:Robur Carolinum
932:Jodocus Hondius
928:Petrus Plancius
920:
911:
860:
857:
852:
849:
835:eccentric orbit
791:. Previously a
724:
699: Carinae,
651:
648:
633:
630:
626:14.3â23.6
613:
610:
558:
555:
548:
534:
531:
524:
510:
507:
468:
430:Semi-major axis
427:
417:
411:
409:
360:
343:
320: 1.0
316:
287:
282:Radial velocity
154:
125:
116:
99:
94:Right ascension
92:
67:
61:
43:
33:
17:
12:
11:
5:
10939:
10929:
10928:
10923:
10918:
10913:
10908:
10903:
10898:
10893:
10888:
10883:
10878:
10863:
10862:
10850:
10838:
10826:
10814:
10791:
10790:
10780:
10777:
10776:
10773:
10772:
10770:
10769:
10764:
10758:
10756:
10746:
10745:
10742:
10741:
10739:
10738:
10736:Bullet Cluster
10732:
10730:
10720:
10719:
10716:
10715:
10713:
10712:
10706:
10704:
10700:
10699:
10697:
10696:
10690:
10688:
10681:
10675:
10674:
10671:
10670:
10668:
10667:
10662:
10657:
10652:
10647:
10642:
10637:
10632:
10627:
10621:
10619:
10615:
10614:
10612:
10611:
10606:
10601:
10596:
10591:
10586:
10581:
10576:
10570:
10568:
10561:
10555:
10554:
10551:
10550:
10548:
10547:
10542:
10537:
10532:
10527:
10522:
10517:
10512:
10507:
10502:
10496:
10494:
10490:
10489:
10487:
10486:
10481:
10476:
10471:
10466:
10461:
10456:
10450:
10448:
10439:
10431:
10430:
10427:
10426:
10424:
10423:
10418:
10413:
10408:
10403:
10398:
10393:
10388:
10383:
10378:
10373:
10367:
10365:
10355:
10354:
10351:
10350:
10348:
10347:
10342:
10337:
10332:
10327:
10322:
10317:
10312:
10307:
10302:
10297:
10292:
10287:
10282:
10277:
10272:
10267:
10262:
10257:
10252:
10247:
10241:
10239:
10235:
10234:
10232:
10231:
10226:
10221:
10216:
10211:
10206:
10201:
10196:
10191:
10185:
10183:
10177:
10176:
10174:
10173:
10168:
10163:
10158:
10153:
10148:
10143:
10138:
10133:
10128:
10123:
10118:
10113:
10108:
10103:
10098:
10093:
10088:
10083:
10078:
10073:
10068:
10063:
10058:
10053:
10048:
10043:
10038:
10033:
10028:
10022:
10020:
10014:
10013:
10011:
10010:
10005:
10000:
9995:
9990:
9985:
9980:
9975:
9970:
9965:
9960:
9955:
9950:
9945:
9940:
9935:
9930:
9925:
9920:
9915:
9910:
9905:
9900:
9895:
9890:
9885:
9880:
9875:
9870:
9865:
9860:
9855:
9850:
9845:
9840:
9835:
9830:
9825:
9820:
9815:
9810:
9805:
9799:
9797:
9791:
9790:
9788:
9787:
9782:
9777:
9772:
9767:
9762:
9757:
9752:
9747:
9741:
9739:
9730:
9724:
9723:
9721:
9720:
9715:
9709:
9706:
9705:
9698:
9697:
9690:
9683:
9675:
9669:
9668:
9662:
9650:
9638:
9633:
9627:
9618:
9610:
9609:External links
9607:
9604:
9603:
9550:
9513:(3): 183â186.
9497:
9467:
9416:
9357:
9310:de Mink, S. E.
9300:
9287:10.1086/506523
9247:
9186:
9173:10.1086/375341
9149:(1): 288â300.
9133:
9106:
9053:
8998:de Mink, S. E.
8985:
8972:10.1086/586885
8932:
8884:
8881:
8871:
8833:
8775:
8727:
8724:
8715:
8656:
8603:
8544:
8480:
8441:(1): 845â857.
8421:
8359:
8354:10.1086/162143
8324:
8280:
8227:
8173:
8114:
8093:(4): 415â427.
8073:
8034:(1): 773â810.
8014:
7952:
7939:10.1086/321136
7899:
7886:10.1086/422599
7846:
7790:
7729:
7690:(1): 598â617.
7670:
7611:
7557:
7499:
7469:
7416:
7389:
7362:
7303:
7296:
7259:
7203:
7190:10.1086/367641
7166:(1): 432â450.
7150:
7137:10.1086/503766
7102:
7093:
7054:(1): L48âL52.
7034:
6999:
6946:
6905:
6899:10.1086/112783
6864:
6810:
6777:
6738:(2): 763â772.
6713:
6684:
6645:(4): 1609â18.
6622:
6568:
6531:(1): 649â657.
6514:
6501:10.1086/518101
6477:(1): 522â542.
6460:
6407:
6351:
6298:
6241:
6200:
6188:10.1086/187904
6151:
6146:10.1086/183108
6116:
6110:10.1086/190561
6075:
6052:10.1086/182269
6022:
5981:
5976:10.1086/151305
5946:
5893:
5839:
5795:
5768:
5761:
5743:
5737:10.1086/509785
5702:
5649:
5636:10.1086/117408
5605:
5600:10.1086/164301
5570:
5516:
5451:
5445:10.1086/145746
5410:
5369:
5364:10.1086/154917
5329:
5283:
5248:
5241:
5221:
5214:
5196:
5189:
5169:
5142:
5117:
5077:(9): 731â736.
5060:
5028:
4991:(3): 374â377.
4972:
4916:
4889:
4883:10.1086/307859
4848:
4827:10.1086/312441
4787:
4766:(2): 237â238.
4746:
4740:10.1086/375306
4704:
4665:(1): L15âL18.
4645:
4639:10.1086/316420
4601:
4551:
4514:(3): 220â234.
4498:
4472:
4436:
4425:on 13 May 2013
4402:
4395:
4374:
4367:
4349:
4300:
4284:Halley, Edmund
4275:
4248:
4241:
4215:
4208:
4192:Vamplew, Anton
4182:
4116:
4036:
3971:
3965:10.1086/320948
3921:
3861:
3824:(1): 602â611.
3789:
3750:
3682:
3622:
3558:
3502:
3479:
3473:10.1086/309961
3429:
3422:
3373:
3331:
3294:(1): 729â742.
3263:
3250:10.1086/429400
3226:(2): 973â982.
3201:
3174:
3114:
3070:
3063:
3017:
3016:
3014:
3011:
3008:
3007:
3002:
2991:
2974:
2958:
2941:
2940:
2938:
2935:
2934:
2933:
2926:
2923:
2854:
2851:
2791:kinetic energy
2768:red supergiant
2751:
2748:
2701:
2698:
2694:
2691:
2675:
2672:
2662:
2659:
2632:
2629:
2623:
2620:
2615:
2612:
2608:
2605:
2587:
2584:
2580:
2577:
2569:
2566:
2558:
2555:
2551:
2548:
2543:
2540:
2519:
2516:
2512:
2509:
2487:value such as
2441:
2438:
2413:
2410:
2402:
2399:
2395:
2392:
2388:
2385:
2381:
2378:
2373:
2370:
2365:
2362:
2359:accretion disk
2350:
2347:
2339:
2336:
2332:
2329:
2325:
2322:
2314:
2311:
2294:
2291:
2286:
2283:
2279:
2276:
2272:
2269:
2265:
2262:
2258:
2255:
2251:
2248:
2244:
2241:
2236:
2233:
2169:
2168:Classification
2166:
2144:
2141:
2123:
2120:
2039:
2036:
2014:
2011:
2007:
2004:
1965:Main article:
1962:
1959:
1935:Main article:
1932:
1929:
1901:Main article:
1898:
1895:
1889:
1878:
1875:bremsstrahlung
1850:
1835:
1834:Radio emission
1832:
1760:
1757:
1737:
1734:
1699:
1696:
1691:
1687:
1658:
1638:
1627:
1620:
1616:
1609:
1605:
1582:
1579:
1460:
1455:
1419:Hydrogen lines
1391:emission lines
1355:
1352:
1310:light-polluted
1304:(bottom right)
1278:
1275:
1222:
1219:
1213:
1210:
1089:Alpha Centauri
1065:
1064:Great Eruption
1062:
919:
916:
910:
907:
858:
855:
850:
847:
766:stellar system
745:
744:
739:
731:
730:
726:
725:
723: 1041â59
694:
691:
690:
684:
683:
677:
669:
668:
662:
654:
653:
649:
646:
642:
636:
635:
631:
628:
624:
616:
615:
611:
608:
604:
596:
595:
591:
590:
584:
576:
575:
569:
561:
560:
556:
553:
545:
537:
536:
532:
529:
521:
513:
512:
508:
505:
501:
493:
492:
488:
487:
483:
482:
479:
465:
464:
461:
452:
451:
448:
439:
438:
435:
424:
423:
407:
398:
397:
394:
388:
387:
384:
378:
377:
371:
370:
367:
366:
363:
358:
350:
349:
337:
329:
328:
303:
294:
293:
290:
285:
277:
276:
273:
272:
266:
265:
256:
250:
249:
246:
239:
238:
235:
228:
227:
224:
217:
216:
213:
206:
205:
202:
195:
194:
191:
184:
183:
180:
173:
172:
169:
162:
161:
151:
145:
144:
139:
133:
132:
128:
127:
122:
113:
112:
109:
103:
102:
97:
89:
88:
83:
77:
76:
63:
62:
27:
15:
9:
6:
4:
3:
2:
10938:
10927:
10924:
10922:
10919:
10917:
10916:Gould objects
10914:
10912:
10909:
10907:
10906:Bayer objects
10904:
10902:
10899:
10897:
10894:
10892:
10889:
10887:
10886:Carina Nebula
10884:
10882:
10879:
10877:
10874:
10873:
10871:
10861:
10851:
10849:
10839:
10837:
10827:
10825:
10820:
10815:
10813:
10803:
10802:
10799:
10788:
10778:
10768:
10765:
10763:
10760:
10759:
10757:
10755:
10751:
10747:
10737:
10734:
10733:
10731:
10729:
10725:
10721:
10711:
10708:
10707:
10705:
10701:
10695:
10692:
10691:
10689:
10685:
10682:
10680:
10676:
10666:
10663:
10661:
10658:
10656:
10653:
10651:
10648:
10646:
10643:
10641:
10638:
10636:
10633:
10631:
10628:
10626:
10625:Carina Nebula
10623:
10622:
10620:
10616:
10610:
10607:
10605:
10602:
10600:
10597:
10595:
10592:
10590:
10587:
10585:
10582:
10580:
10577:
10575:
10572:
10571:
10569:
10565:
10562:
10560:
10556:
10546:
10543:
10541:
10538:
10536:
10533:
10531:
10528:
10526:
10523:
10521:
10518:
10516:
10513:
10511:
10510:Collinder 228
10508:
10506:
10503:
10501:
10498:
10497:
10495:
10491:
10485:
10482:
10480:
10477:
10475:
10472:
10470:
10467:
10465:
10462:
10460:
10457:
10455:
10452:
10451:
10449:
10447:
10443:
10440:
10438:
10432:
10422:
10419:
10417:
10414:
10412:
10409:
10407:
10404:
10402:
10399:
10397:
10394:
10392:
10389:
10387:
10384:
10382:
10379:
10377:
10374:
10372:
10369:
10368:
10366:
10364:
10360:
10356:
10346:
10343:
10341:
10338:
10336:
10333:
10331:
10328:
10326:
10323:
10321:
10318:
10316:
10313:
10311:
10308:
10306:
10303:
10301:
10298:
10296:
10293:
10291:
10288:
10286:
10283:
10281:
10278:
10276:
10273:
10271:
10268:
10266:
10263:
10261:
10258:
10256:
10255:DEN 0817â6155
10253:
10251:
10248:
10246:
10243:
10242:
10240:
10236:
10230:
10227:
10225:
10222:
10220:
10217:
10215:
10212:
10210:
10207:
10205:
10202:
10200:
10197:
10195:
10192:
10190:
10187:
10186:
10184:
10182:
10178:
10172:
10169:
10167:
10164:
10162:
10159:
10157:
10154:
10152:
10149:
10147:
10144:
10142:
10139:
10137:
10134:
10132:
10129:
10127:
10124:
10122:
10119:
10117:
10114:
10112:
10109:
10107:
10104:
10102:
10099:
10097:
10094:
10092:
10089:
10087:
10084:
10082:
10079:
10077:
10074:
10072:
10069:
10067:
10064:
10062:
10059:
10057:
10054:
10052:
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10044:
10042:
10039:
10037:
10034:
10032:
10029:
10027:
10024:
10023:
10021:
10019:
10015:
10009:
10006:
10004:
10001:
9999:
9996:
9994:
9991:
9989:
9986:
9984:
9981:
9979:
9976:
9974:
9971:
9969:
9966:
9964:
9961:
9959:
9956:
9954:
9951:
9949:
9946:
9944:
9941:
9939:
9936:
9934:
9931:
9929:
9926:
9924:
9921:
9919:
9916:
9914:
9911:
9909:
9906:
9904:
9901:
9899:
9896:
9894:
9891:
9889:
9886:
9884:
9881:
9879:
9876:
9874:
9871:
9869:
9866:
9864:
9861:
9859:
9856:
9854:
9851:
9849:
9846:
9844:
9841:
9839:
9836:
9834:
9831:
9829:
9826:
9824:
9821:
9819:
9816:
9814:
9811:
9809:
9806:
9804:
9801:
9800:
9798:
9796:
9792:
9786:
9783:
9781:
9778:
9776:
9773:
9771:
9770:Îč (Aspidiske)
9768:
9766:
9763:
9761:
9758:
9756:
9753:
9751:
9748:
9746:
9743:
9742:
9740:
9738:
9734:
9731:
9729:
9725:
9719:
9716:
9714:
9711:
9710:
9707:
9703:
9696:
9691:
9689:
9684:
9682:
9677:
9676:
9673:
9666:
9663:
9661:
9657:
9654:
9651:
9649:
9645:
9642:
9639:
9637:
9634:
9632:at Solstation
9631:
9628:
9624:
9619:
9616:
9613:
9612:
9599:
9595:
9591:
9587:
9583:
9579:
9574:
9569:
9565:
9561:
9554:
9546:
9542:
9538:
9534:
9530:
9526:
9521:
9516:
9512:
9508:
9501:
9493:
9489:
9485:
9481:
9474:
9472:
9463:
9459:
9455:
9451:
9447:
9443:
9439:
9435:
9431:
9427:
9420:
9412:
9408:
9403:
9398:
9394:
9390:
9385:
9380:
9376:
9372:
9368:
9361:
9353:
9349:
9345:
9341:
9337:
9333:
9328:
9323:
9319:
9315:
9311:
9304:
9296:
9292:
9288:
9284:
9280:
9276:
9271:
9266:
9262:
9258:
9251:
9243:
9239:
9235:
9231:
9227:
9223:
9219:
9215:
9210:
9205:
9201:
9197:
9190:
9182:
9178:
9174:
9170:
9166:
9162:
9157:
9152:
9148:
9144:
9137:
9129:
9125:
9121:
9117:
9110:
9102:
9098:
9094:
9090:
9086:
9082:
9077:
9072:
9068:
9064:
9057:
9049:
9045:
9041:
9037:
9033:
9029:
9025:
9021:
9016:
9011:
9007:
9003:
8999:
8992:
8990:
8981:
8977:
8973:
8969:
8965:
8961:
8956:
8951:
8947:
8943:
8936:
8928:
8924:
8920:
8916:
8912:
8908:
8903:
8898:
8894:
8890:
8875:
8867:
8863:
8858:
8853:
8849:
8845:
8837:
8829:
8825:
8821:
8817:
8813:
8809:
8804:
8799:
8795:
8791:
8784:
8782:
8780:
8771:
8767:
8763:
8759:
8755:
8751:
8746:
8741:
8737:
8733:
8719:
8711:
8707:
8702:
8697:
8693:
8689:
8684:
8679:
8675:
8671:
8667:
8660:
8652:
8648:
8644:
8640:
8636:
8632:
8627:
8622:
8618:
8614:
8607:
8599:
8595:
8590:
8585:
8581:
8577:
8572:
8567:
8563:
8559:
8555:
8548:
8540:
8536:
8531:
8526:
8522:
8518:
8513:
8508:
8504:
8500:
8496:
8489:
8487:
8485:
8476:
8472:
8467:
8462:
8458:
8454:
8449:
8444:
8440:
8436:
8432:
8425:
8417:
8413:
8408:
8403:
8399:
8395:
8390:
8385:
8381:
8377:
8373:
8366:
8364:
8355:
8351:
8347:
8343:
8339:
8335:
8328:
8320:
8316:
8312:
8311:10.1038/37558
8308:
8304:
8300:
8297:(6660): 587.
8296:
8292:
8284:
8276:
8272:
8268:
8264:
8260:
8256:
8251:
8246:
8242:
8238:
8231:
8223:
8219:
8215:
8211:
8207:
8203:
8198:
8193:
8189:
8185:
8177:
8169:
8165:
8160:
8155:
8151:
8147:
8142:
8137:
8133:
8129:
8125:
8118:
8109:
8104:
8100:
8096:
8092:
8088:
8084:
8077:
8069:
8065:
8060:
8055:
8051:
8047:
8042:
8037:
8033:
8029:
8025:
8018:
8010:
8006:
8002:
7998:
7994:
7990:
7986:
7982:
7977:
7972:
7968:
7964:
7956:
7948:
7944:
7940:
7936:
7932:
7928:
7923:
7918:
7914:
7910:
7903:
7895:
7891:
7887:
7883:
7879:
7875:
7870:
7865:
7861:
7857:
7850:
7842:
7838:
7834:
7830:
7826:
7822:
7817:
7812:
7808:
7804:
7803:New Astronomy
7797:
7795:
7786:
7782:
7778:
7774:
7770:
7766:
7762:
7758:
7753:
7748:
7744:
7740:
7733:
7725:
7721:
7716:
7711:
7707:
7703:
7698:
7693:
7689:
7685:
7681:
7674:
7666:
7662:
7657:
7652:
7648:
7644:
7639:
7634:
7630:
7626:
7622:
7615:
7607:
7603:
7599:
7595:
7591:
7587:
7582:
7577:
7573:
7569:
7561:
7553:
7549:
7545:
7541:
7537:
7533:
7528:
7523:
7519:
7515:
7508:
7506:
7504:
7495:
7491:
7487:
7483:
7476:
7474:
7465:
7461:
7457:
7453:
7449:
7445:
7440:
7435:
7431:
7427:
7420:
7412:
7408:
7404:
7400:
7393:
7385:
7381:
7377:
7373:
7366:
7358:
7354:
7349:
7344:
7340:
7336:
7331:
7326:
7322:
7318:
7314:
7307:
7299:
7293:
7289:
7285:
7281:
7277:
7273:
7266:
7264:
7255:
7251:
7247:
7243:
7239:
7235:
7230:
7225:
7221:
7217:
7210:
7208:
7199:
7195:
7191:
7187:
7183:
7179:
7174:
7169:
7165:
7161:
7154:
7146:
7142:
7138:
7134:
7130:
7126:
7121:
7116:
7112:
7108:
7097:
7089:
7085:
7080:
7075:
7071:
7067:
7062:
7057:
7053:
7049:
7045:
7038:
7030:
7026:
7022:
7018:
7014:
7010:
7003:
6995:
6991:
6987:
6983:
6979:
6975:
6970:
6965:
6961:
6957:
6950:
6941:
6936:
6932:
6928:
6924:
6920:
6916:
6909:
6900:
6895:
6891:
6887:
6883:
6879:
6875:
6868:
6860:
6856:
6852:
6848:
6844:
6840:
6835:
6830:
6826:
6822:
6814:
6806:
6802:
6797:
6792:
6788:
6781:
6773:
6769:
6764:
6759:
6755:
6751:
6746:
6741:
6737:
6733:
6729:
6722:
6720:
6718:
6709:
6705:
6701:
6697:
6696:
6688:
6680:
6676:
6671:
6666:
6662:
6658:
6653:
6648:
6644:
6640:
6636:
6629:
6627:
6618:
6614:
6610:
6606:
6602:
6598:
6593:
6588:
6584:
6580:
6572:
6564:
6560:
6556:
6552:
6548:
6544:
6539:
6534:
6530:
6526:
6518:
6510:
6506:
6502:
6498:
6494:
6490:
6485:
6480:
6476:
6472:
6464:
6456:
6452:
6448:
6444:
6440:
6436:
6431:
6426:
6422:
6418:
6411:
6403:
6399:
6395:
6391:
6387:
6383:
6378:
6373:
6369:
6365:
6358:
6356:
6347:
6343:
6339:
6335:
6331:
6327:
6322:
6317:
6313:
6309:
6302:
6294:
6290:
6286:
6282:
6278:
6274:
6269:
6264:
6260:
6256:
6248:
6246:
6236:
6231:
6227:
6223:
6219:
6215:
6211:
6204:
6193:
6189:
6185:
6181:
6177:
6173:
6169:
6162:
6155:
6147:
6143:
6139:
6135:
6131:
6127:
6120:
6111:
6106:
6102:
6098:
6094:
6090:
6086:
6079:
6071:
6067:
6062:
6057:
6053:
6049:
6045:
6041:
6037:
6033:
6026:
6017:
6012:
6008:
6004:
6000:
5996:
5992:
5985:
5977:
5973:
5969:
5965:
5961:
5957:
5950:
5942:
5938:
5934:
5930:
5926:
5922:
5917:
5912:
5908:
5904:
5897:
5889:
5885:
5881:
5877:
5873:
5869:
5864:
5859:
5855:
5851:
5843:
5834:
5829:
5825:
5821:
5817:
5813:
5809:
5802:
5800:
5791:
5787:
5783:
5779:
5772:
5764:
5758:
5754:
5747:
5738:
5733:
5729:
5725:
5721:
5717:
5713:
5706:
5698:
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5690:
5686:
5682:
5678:
5673:
5668:
5664:
5660:
5653:
5645:
5641:
5637:
5633:
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5609:
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5597:
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5504:
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5492:
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5474:
5470:
5466:
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5309:
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5301:
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5279:
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5110:
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5020:
5016:
5012:
5008:
5004:
4999:
4994:
4990:
4986:
4979:
4977:
4968:
4964:
4960:
4956:
4952:
4948:
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4938:
4934:
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4929:
4920:
4912:
4908:
4904:
4900:
4893:
4884:
4879:
4875:
4871:
4867:
4863:
4859:
4852:
4844:
4840:
4836:
4832:
4828:
4824:
4820:
4816:
4811:
4806:
4802:
4798:
4791:
4782:
4777:
4773:
4769:
4765:
4761:
4757:
4750:
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4736:
4732:
4728:
4724:
4720:
4716:
4708:
4700:
4696:
4691:
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4682:
4678:
4673:
4668:
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4660:
4656:
4649:
4640:
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4627:
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4619:
4615:
4611:
4605:
4597:
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4569:
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4509:
4502:
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4468:
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4353:
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4323:
4319:
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4311:
4304:
4296:
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4291:
4285:
4279:
4271:
4267:
4263:
4259:
4252:
4244:
4238:
4234:
4229:
4228:
4219:
4211:
4205:
4201:
4198:(June 2010).
4197:
4193:
4190:Gater, Will;
4186:
4178:
4174:
4169:
4164:
4160:
4156:
4151:
4146:
4142:
4138:
4134:
4127:
4125:
4123:
4121:
4112:
4108:
4104:
4100:
4095:
4090:
4085:
4080:
4076:
4072:
4067:
4062:
4058:
4054:
4050:
4043:
4041:
4032:
4028:
4023:
4018:
4014:
4010:
4005:
4000:
3996:
3992:
3988:
3980:
3978:
3976:
3966:
3961:
3957:
3953:
3949:
3945:
3941:
3934:
3932:
3930:
3928:
3926:
3917:
3913:
3909:
3905:
3901:
3897:
3892:
3887:
3883:
3879:
3872:
3870:
3868:
3866:
3857:
3853:
3849:
3845:
3841:
3837:
3832:
3827:
3823:
3819:
3812:
3810:
3808:
3806:
3804:
3802:
3800:
3798:
3796:
3794:
3785:
3781:
3777:
3773:
3769:
3765:
3764:New Astronomy
3761:
3754:
3746:
3742:
3737:
3732:
3728:
3724:
3719:
3714:
3710:
3706:
3702:
3695:
3693:
3691:
3689:
3687:
3678:
3674:
3669:
3664:
3660:
3656:
3651:
3646:
3642:
3638:
3634:
3626:
3618:
3614:
3609:
3604:
3600:
3596:
3591:
3586:
3582:
3578:
3574:
3567:
3565:
3563:
3554:
3550:
3546:
3542:
3538:
3534:
3529:
3524:
3520:
3516:
3509:
3507:
3498:
3494:
3490:
3483:
3474:
3469:
3465:
3461:
3457:
3453:
3449:
3442:
3440:
3438:
3436:
3434:
3425:
3419:
3415:
3411:
3407:
3403:
3399:
3398:
3390:
3388:
3386:
3384:
3382:
3380:
3378:
3369:
3365:
3361:
3357:
3350:
3348:
3346:
3344:
3342:
3340:
3338:
3336:
3327:
3323:
3319:
3315:
3311:
3307:
3302:
3297:
3293:
3289:
3285:
3278:
3276:
3274:
3272:
3270:
3268:
3259:
3255:
3251:
3247:
3243:
3239:
3234:
3229:
3225:
3221:
3220:
3212:
3210:
3208:
3206:
3197:
3193:
3189:
3185:
3178:
3170:
3166:
3161:
3156:
3152:
3148:
3143:
3138:
3134:
3130:
3126:
3118:
3110:
3106:
3102:
3098:
3091:
3089:
3087:
3085:
3083:
3081:
3079:
3077:
3075:
3066:
3064:0-333-75088-8
3060:
3056:
3052:
3048:
3044:
3040:
3036:
3029:
3027:
3025:
3023:
3018:
3000:
2995:
2988:
2987:Spectral line
2984:
2978:
2972:
2968:
2967:optical depth
2962:
2956:
2952:
2951:optical depth
2946:
2942:
2932:
2929:
2928:
2922:
2920:
2914:
2912:
2908:
2903:
2898:
2896:
2892:
2888:
2887:magnetosphere
2884:
2880:
2876:
2868:
2864:
2859:
2850:
2848:
2844:
2840:
2836:
2831:
2827:
2822:
2818:
2816:
2812:
2808:
2804:
2800:
2796:
2792:
2788:
2787:type Ib or Ic
2784:
2780:
2776:
2771:
2769:
2766:or anonymous
2765:
2756:
2747:
2743:
2741:
2735:
2732:
2727:
2724:
2719:
2713:
2711:
2707:
2688:
2680:
2671:
2669:
2656:
2654:
2645:
2641:
2637:
2628:
2619:
2602:
2600:
2596:
2593:
2592:largest-known
2575:
2574:optical depth
2562:
2547:933,000
2539:
2532:
2528:
2525:
2524:optical depth
2507:
2503:
2498:
2486:
2482:
2476:
2472:
2468:
2461:
2454:
2450:
2446:
2437:
2433:
2431:
2427:
2423:
2419:
2406:
2369:
2360:
2356:
2343:
2318:
2309:
2299:
2290:
2232:
2230:
2226:
2220:
2217:
2209:
2207:
2202:
2197:
2192:
2190:
2184:
2179:
2178:variable star
2175:
2165:
2161:
2157:
2149:
2140:
2137:
2128:
2119:
2111:
2093:
2089:
2085:
2084:main sequence
2081:
2077:
2073:
2068:
2050:
2046:
2035:
2033:
2028:
2024:
2018:
2000:
1997:
1992:
1986:
1982:
1973:
1968:
1958:
1956:
1952:
1948:
1944:
1938:
1928:
1926:
1922:
1918:
1909:
1904:
1903:Carina Nebula
1894:
1893:wavelengths.
1886:
1884:
1876:
1872:
1868:
1864:
1860:
1856:
1848:
1844:
1840:
1831:
1829:
1825:
1821:
1815:
1813:
1809:
1805:
1801:
1796:
1794:
1790:
1786:
1782:
1778:
1774:
1765:
1756:
1754:
1750:
1745:
1744:Near-infrared
1741:
1732:
1727:
1725:
1721:
1717:
1713:
1704:
1695:
1685:
1680:
1676:
1672:
1669:, creating a
1668:
1664:
1656:
1652:
1648:
1647:photo-ionised
1644:
1636:
1633:
1624:
1615:
1612:, as well as
1603:
1596:
1593:taken by ESA/
1592:
1587:
1578:
1575:
1570:
1568:
1562:
1560:
1556:
1552:
1548:
1543:
1537:
1533:
1529:
1525:
1517:
1512:
1508:
1505:
1500:
1496:
1495:Weigelt Blobs
1492:
1487:
1485:
1481:
1477:
1473:
1472:spectral type
1468:
1466:
1458:
1451:
1445:
1443:
1439:
1435:
1430:
1426:
1424:
1420:
1416:
1412:
1408:
1407:stellar winds
1404:
1400:
1399:Weigelt Blobs
1396:
1392:
1388:
1384:
1380:
1376:
1368:
1364:
1360:
1351:
1348:
1344:
1343:meteor shower
1341:
1336:
1334:
1331:known as the
1330:
1326:
1321:
1319:
1315:
1311:
1303:
1298:
1292:
1288:
1287:Carina Nebula
1283:
1274:
1272:
1268:
1264:
1259:
1257:
1251:
1249:
1245:
1241:
1240:near-infrared
1231:
1227:
1218:
1209:
1207:
1203:
1199:
1195:
1191:
1185:
1130:
1126:
1122:
1117:
1115:
1111:
1107:
1106:Beta Centauri
1102:
1098:
1094:
1090:
1085:
1083:
1079:
1078:John Herschel
1070:
1061:
1059:
1054:
1049:
1042:
1031:
1022:
1018:
1014:
1010:
1006:
1002:
999:
998:mansion-based
994:
992:
988:
984:
979:
975:
971:
967:
963:
959:
955:
951:
950:Edmond Halley
947:
943:
939:
938:
934:and the 1603
933:
929:
925:
924:Pieter Keyser
915:
906:
904:
900:
899:meteor shower
897:
892:
890:
889:Carina Nebula
886:
883:
879:
875:
871:
868:
864:
853:
844:
840:
836:
831:
829:
825:
824:latitude 30°N
821:
817:
816:latitude 30°S
813:
808:
806:
802:
798:
794:
793:4th-magnitude
790:
787:
786:constellation
783:
779:
775:
771:
767:
763:
759:
755:
751:
743:
740:
738:
737:
733:
732:
727:
722:
719: 14799,
718:
714:
710:
707: 93308,
706:
702:
698:
692:
689:
685:
682:
678:
676:
675:
671:
670:
667:
663:
661:
660:
656:
655:
652:
643:
641:
638:
637:
634:
625:
623:
622:
618:
617:
614:
605:
603:
602:
598:
597:
592:
589:
585:
583:
582:
578:
577:
574:
570:
568:
567:
563:
562:
559:
546:
544:
543:
539:
538:
535:
522:
520:
519:
515:
514:
511:
502:
500:
499:
495:
494:
489:
484:
480:
477:
475:
472:
467:
466:
463:130â145°
462:
460:
458:
454:
453:
449:
447:
445:
441:
440:
436:
433:
431:
426:
425:
421:
408:
406:
404:
400:
399:
395:
393:
390:
389:
385:
383:
380:
379:
376:
372:
368:
364:
362:
356:
352:
351:
347:
342:
338:
336:
335:
331:
330:
327:
323:
315:
311:
304:
302:
300:
299:Proper motion
296:
295:
291:
289:
283:
279:
278:
274:
271:
267:
264:
260:
257:
255:
252:
251:
247:
245:
241:
240:
236:
234:
230:
229:
225:
222:
219:
218:
214:
211:
208:
207:
203:
200:
197:
196:
192:
189:
186:
185:
181:
178:
175:
174:
170:
167:
164:
163:
158:
152:
150:
147:
146:
143:
140:
138:
135:
134:
129:
123:
119:
115:
114:
110:
108:
105:
104:
98:
95:
91:
90:
87:
84:
82:
81:Constellation
79:
78:
74:
70:
64:
60:
59:
56:
52:
46:
41:
37:
31:
25:
19:
10901:O-type stars
10881:Binary stars
10860:Solar System
10545:Westerlund 2
10396:OGLE2-TR-L9b
10391:OGLE-TR-211b
10386:OGLE-TR-182b
10381:OGLE-TR-113b
10376:OGLE-TR-132b
10371:OGLE-TR-111b
9759:
9566:(1): 61â67.
9563:
9559:
9553:
9510:
9506:
9500:
9483:
9479:
9429:
9425:
9419:
9374:
9370:
9360:
9317:
9313:
9303:
9260:
9256:
9250:
9199:
9195:
9189:
9146:
9142:
9136:
9119:
9115:
9109:
9066:
9062:
9056:
9005:
9001:
8945:
8941:
8935:
8892:
8888:
8874:
8847:
8843:
8836:
8793:
8789:
8735:
8731:
8718:
8673:
8669:
8659:
8616:
8612:
8606:
8561:
8557:
8547:
8502:
8498:
8438:
8434:
8424:
8379:
8375:
8337:
8333:
8327:
8294:
8290:
8283:
8240:
8236:
8230:
8187:
8183:
8176:
8131:
8127:
8117:
8090:
8086:
8076:
8031:
8027:
8017:
7966:
7962:
7955:
7912:
7908:
7902:
7859:
7855:
7849:
7809:(1): 11â24.
7806:
7802:
7742:
7738:
7732:
7687:
7683:
7673:
7628:
7624:
7614:
7571:
7567:
7560:
7517:
7513:
7485:
7481:
7429:
7425:
7419:
7402:
7398:
7392:
7375:
7371:
7365:
7320:
7316:
7306:
7271:
7219:
7215:
7163:
7159:
7153:
7110:
7106:
7096:
7051:
7047:
7037:
7012:
7008:
7002:
6959:
6955:
6949:
6922:
6918:
6908:
6881:
6877:
6867:
6824:
6820:
6813:
6786:
6780:
6735:
6731:
6699:
6694:
6687:
6642:
6638:
6582:
6578:
6571:
6528:
6524:
6517:
6474:
6470:
6463:
6420:
6416:
6410:
6367:
6363:
6311:
6307:
6301:
6258:
6254:
6217:
6213:
6203:
6171:
6167:
6154:
6129:
6125:
6119:
6092:
6088:
6078:
6035:
6031:
6025:
5998:
5994:
5984:
5959:
5955:
5949:
5906:
5902:
5896:
5853:
5849:
5842:
5815:
5811:
5781:
5777:
5771:
5752:
5746:
5719:
5715:
5705:
5662:
5658:
5652:
5619:
5615:
5608:
5583:
5579:
5573:
5530:
5526:
5519:
5468:
5464:
5427:
5423:
5413:
5386:
5382:
5372:
5347:
5343:
5299:
5295:
5292:Le Sueur, A.
5286:
5261:
5257:
5251:
5231:
5224:
5205:
5199:
5179:
5172:
5155:
5151:
5145:
5133:. Retrieved
5120:
5074:
5070:
5063:
5046:
5042:
4988:
4984:
4932:
4926:
4919:
4902:
4898:
4892:
4865:
4861:
4851:
4800:
4796:
4790:
4763:
4759:
4749:
4722:
4718:
4707:
4662:
4658:
4648:
4621:
4617:
4604:
4571:
4567:
4511:
4507:
4501:
4491:
4484:
4480:
4475:
4452:
4427:. Retrieved
4423:the original
4418:
4405:
4383:
4377:
4358:
4352:
4317:
4313:
4303:
4295:the original
4288:
4278:
4261:
4257:
4251:
4226:
4218:
4199:
4185:
4140:
4136:
4056:
4052:
3994:
3990:
3950:(837): 837.
3947:
3943:
3881:
3877:
3821:
3817:
3767:
3763:
3753:
3708:
3704:
3640:
3636:
3625:
3580:
3576:
3518:
3514:
3488:
3482:
3455:
3451:
3396:
3359:
3355:
3291:
3287:
3223:
3217:
3187:
3183:
3177:
3132:
3128:
3117:
3100:
3096:
3038:
3034:
2994:
2983:ion notation
2977:
2961:
2945:
2915:
2901:
2899:
2872:
2823:
2819:
2815:neutron star
2772:
2761:
2744:
2736:
2731:triple-alpha
2728:
2714:
2689:
2685:
2657:
2653:stellar wind
2649:
2625:
2603:
2597:, including
2563:
2545:
2533:
2529:
2499:
2477:
2473:
2462:
2458:
2434:
2407:
2375:
2344:
2319:
2304:
2238:
2221:
2214:10,000
2210:
2193:
2171:
2162:
2158:
2154:
2133:
2112:
2069:
2041:
2022:
2019:
2001:
1995:
1978:
1943:open cluster
1940:
1914:
1897:Surroundings
1887:
1837:
1822:detected by
1816:
1810:(ASCA), and
1797:
1770:
1752:
1748:
1742:
1731:solar masses
1728:
1716:far infrared
1709:
1690:states by Ly
1625:
1599:
1571:
1563:
1524:light echoes
1521:
1488:
1469:
1446:
1427:
1372:
1340:Eta Carinids
1337:
1322:
1314:Bortle scale
1307:
1260:
1252:
1243:
1236:
1224:
1215:
1189:
1128:
1125:Lake Tyrrell
1118:
1086:
1075:
1050:
995:
986:
961:
953:
942:Johann Bayer
935:
921:
912:
896:Eta Carinids
893:
885:open cluster
832:
820:Johannesburg
809:
761:
757:
753:
749:
748:
734:
703: 4210,
672:
664:37,200
657:
639:
619:
599:
579:
564:
540:
516:
496:
469:
455:
444:Eccentricity
442:
437:15.4 AU
428:
401:
391:
381:
353:
344:(2,300
332:
297:
280:
244:colour index
233:colour index
124:â1.0 to ~7.6
100:10 45 03.591
48:
44:
22:Eta Carinae
18:
10848:Outer space
10836:Spaceflight
10767:GRB 080916C
10540:Trumpler 16
10535:Trumpler 15
10530:Trumpler 14
10416:HD 85628 Ab
10300:OGLE2-TR-L9
10295:OGLE-TR-211
10290:OGLE-TR-182
10275:NGC 3603-A1
10265:Innes' star
10250:CPDâ57°2874
9745:α (Canopus)
9377:(2): 1191.
9122:: #405.03.
8676:(2): 1114.
8243:(5): 2056.
8134:(4): 3820.
7631:(3): 2445.
7222:(2): L223.
6925:: 141â147.
6261:(2): L142.
6001:: 13Pâ20P.
5049:(151): 09.
4725:(6): 3222.
4429:30 December
4419:nmns.edu.tw
4143:(2): 1623.
3884:: 373â398.
3711:(3): 2064.
3643:(4): 1649.
3103:(6): 1â76.
2919:ozone layer
2891:ozone layer
2764:white dwarf
2670:explosion.
2440:Temperature
2225:O-type star
2092:O-type star
1985:polar lobes
1951:Trumpler 14
1937:Trumpler 16
1931:Trumpler 16
1665:to certain
1602:ultraviolet
1581:Ultraviolet
1574:occultation
1540:5,000
1484:photosphere
1044:, English:
1041:HÇi ShÄn Ăšr
937:Uranometria
882:Trumpler 16
867:ultraviolet
812:circumpolar
778:light-years
750:Eta Carinae
679:<3
659:Temperature
606:30â80
586:<3
566:Temperature
457:Inclination
365:â8.6 (2012)
339:7,500
126:4.2 (2018)
107:Declination
49:Jon Morse (
10870:Categories
10762:GRB 000131
10635:G290.1-0.8
10505:Carina OB2
10500:Carina OB1
10411:HD 65216 c
10406:HD 65216 b
10363:Exoplanets
10285:NGC 3603-C
10280:NGC 3603-B
10260:1E 1048-59
10245:AWI0005x3s
9263:(1): L45.
9069:(2): 164.
8996:Sana, H.;
8619:(2): 187.
8571:1511.06889
8512:1808.00991
8448:1609.00362
8190:(3): L37.
7915:(1): 283.
7581:1504.04940
7330:1808.02073
7323:(3): 133.
6585:(3): 977.
6423:(2): 566.
6370:(2): 636.
6314:(3): L29.
5909:(6): 202.
5818:(2): 731.
5722:(2): 289.
5665:(1): 695.
5389:(9): 619.
5158:(2): 126.
5084:1904.09219
4868:(2): 983.
4066:1706.05112
4004:2205.15116
3997:(2): 175.
3770:(2): 107.
3528:1908.09154
3489:Washington
3142:1801.05445
3013:References
2999:Fraunhofer
2895:satellites
2883:gamma rays
2863:black hole
2801:(SLSN) or
2779:black hole
2706:convective
2502:hypergiant
2372:Luminosity
2189:bolometric
2122:Properties
2023:polar wind
1961:Homunculus
1955:Carina OB1
1871:arcseconds
1855:millimetre
1626:Certain Fe
1516:light echo
1504:HDE 316285
1476:supergiant
1425:envelope.
1411:absorption
1302:PP Carinae
1277:Visibility
1123:people of
1110:periastron
1013:λ Centauri
974:Argo Navis
774:luminosity
711:â59°2620,
697:231 G
640:Luminosity
547:4 million
542:Luminosity
503:~100
471:Periastron
416: days
270:Astrometry
223: (K)
212: (H)
201: (J)
190: (R)
179: (B)
168: (U)
10812:Astronomy
10525:Platais 8
9755:Δ (Avior)
9573:0911.2196
9545:118579150
9520:0903.4710
9411:119208317
9384:1308.0112
9327:1102.1732
9242:206533034
9209:1208.3217
9101:119292900
9076:1306.0559
9015:1207.6397
8955:0802.1742
8902:1110.5049
8880:120
8857:1101.5873
8803:1308.4681
8770:118870118
8745:1401.7322
8683:1305.2099
8651:118438526
8626:1407.7530
8539:119343623
8475:119198766
8416:119202050
8389:1010.3770
8275:118880932
8250:0908.1627
8168:118407295
8141:1310.0487
8041:1010.3718
7816:0802.0167
7752:0809.1678
7724:119284620
7697:1406.7431
7665:118405692
7638:1412.7569
7552:119271857
7527:1112.4338
7520:(1): 73.
7464:119269671
7439:1201.0623
7432:(2): 41.
7357:119030757
7254:119188874
7229:1006.4816
7088:119295262
7061:0911.0176
7029:0004-6361
6969:1406.6297
6962:(2): 95.
6834:1103.1126
6827:(1): 15.
6796:0809.5081
6679:119334960
6538:1008.3235
6509:119341465
6402:119342823
6321:0712.1491
6268:0904.2736
6220:: 85â92.
6070:122613896
5941:119242683
5916:1103.4671
5888:119228664
5863:1401.4999
5697:119187363
5672:1411.0695
5644:0004-6256
5565:119208968
5540:1403.7202
5533:(1): L8.
5511:205227548
5478:1112.2210
5324:122853758
5278:0004-6361
5206:Astronomy
5109:126188024
5023:118568091
4998:0912.2557
4967:119228664
4942:1401.4999
4596:122193829
4546:118454721
4521:1010.4610
4344:1366-8781
4177:119205238
4150:1204.1963
4059:(2): 79.
4031:0004-637X
3891:0910.3158
3856:118399302
3831:0912.1439
3745:119279180
3718:1111.2226
3650:0711.4250
3617:118614725
3590:1010.3719
3553:202149820
3301:0912.1067
3169:0035-8711
2907:melatonin
2847:SN 2006gy
2843:iPTF14hls
2826:SN 2009ip
2803:hypernova
2795:radiation
2674:Evolution
2631:Eruptions
2536:5 MK
2465:100
2426:SN 2006jc
2355:eccentric
2293:Mass loss
2196:Milky Way
2183:S Doradus
1925:Milky Way
1865:hydrogen
1843:microwave
1777:gamma ray
1753:butterfly
1651:resonance
1559:supernova
1438:CNO cycle
1325:dust lane
1202:naked-eye
1009:s Carinae
863:supernova
805:naked-eye
770:two stars
762:Eta Argus
754:η Carinae
392:Companion
120: (V)
10787:Category
10679:Galaxies
10640:Hen 2-47
10437:clusters
10171:4325 (z)
10166:4257 (u)
10151:4177 (t)
10146:4164 (t)
10141:4159 (r)
10131:4138 (K)
10126:4114 (s)
10121:4102 (I)
10116:4089 (L)
10111:4025 (M)
10106:3884 (l)
10101:3856 (m)
10096:3825 (h)
10091:3821 (H)
10086:3728 (k)
10081:3696 (g)
10076:3663 (i)
10071:3643 (G)
10066:3598 (b)
10061:3571 (c)
10056:3415 (e)
10051:3414 (e)
10046:3260 (C)
10041:3220 (B)
10036:3159 (D)
10031:2934 (Q)
10026:2435 (N)
9963:V533 (y)
9953:V520 (w)
9943:V448 (O)
9938:V415 (A)
9933:V399 (P)
9928:V382 (x)
9923:V376 (b)
9913:V371 (z)
9908:V357 (a)
9903:V345 (E)
9898:V344 (f)
9893:V343 (d)
9883:V337 (q)
9795:Variable
9656:Archived
9644:Archived
9598:15141366
9462:21850504
9454:17736193
9352:54848289
9320:: A131.
9295:15424181
9234:22923572
9181:59065632
9048:53596517
9040:22837522
8980:15529810
8927:85458919
8895:: A146.
8885:☉
8828:84177572
8796:: A131.
8728:☉
8710:26170005
8598:53380205
8222:18163131
8068:85440811
8001:17568740
7947:16159958
7841:11665477
7777:18784719
7606:53131136
7574:: A122.
7488:: 1445.
7198:15762674
7145:12453761
6994:62893264
6884:: 1193.
6859:13951142
6772:14060690
6563:51412901
6455:16812330
6346:35225132
6293:18241474
6192:Archived
6174:: L121.
5622:: 1784.
5503:22337057
5135:2 August
4835:10600628
4699:17051247
4574:: 1â32.
4450:(1847).
4286:(1679).
4111:27906029
4103:32601504
3677:14624515
3258:18166928
3190:: 2023.
2925:See also
2911:insomnia
2839:SN 1961V
2734:fusion.
2702:☉
2695:☉
2663:☉
2622:Rotation
2616:☉
2609:☉
2588:☉
2581:☉
2570:☉
2559:☉
2552:☉
2520:☉
2513:☉
2430:UGC 4904
2422:NGC 1058
2418:SN 1961V
2414:☉
2403:☉
2396:☉
2389:☉
2382:☉
2366:☉
2351:☉
2346:10
2340:☉
2333:☉
2326:☉
2315:☉
2287:☉
2280:☉
2273:☉
2266:☉
2259:☉
2252:☉
2245:☉
2240:90
2045:parallax
2038:Distance
2015:☉
2008:☉
1771:Several
1738:☉
1698:Infrared
1632:low-gain
1465:nebulium
1436:via the
1423:hydrogen
1387:spectrum
1375:strength
1192:"Crow" (
1097:Arcturus
1021:asterism
1017:λ Muscae
859:☉
851:☉
650:☉
632:☉
612:☉
557:☉
533:☉
525:(60â742)
509:☉
357: (M
334:Distance
53:) &
10798:Portals
10655:IC 2448
10650:IC 2220
10559:Nebulae
10520:IC 2714
10515:IC 2602
10305:Sher 25
10270:LHS 288
9578:Bibcode
9525:Bibcode
9488:Bibcode
9486:: 193.
9434:Bibcode
9426:Science
9389:Bibcode
9332:Bibcode
9275:Bibcode
9214:Bibcode
9196:Science
9161:Bibcode
9124:Bibcode
9081:Bibcode
9020:Bibcode
9002:Science
8960:Bibcode
8907:Bibcode
8862:Bibcode
8850:: 266.
8808:Bibcode
8750:Bibcode
8738:: A30.
8688:Bibcode
8631:Bibcode
8576:Bibcode
8517:Bibcode
8453:Bibcode
8394:Bibcode
8342:Bibcode
8340:: 665.
8319:4431077
8299:Bibcode
8255:Bibcode
8202:Bibcode
8146:Bibcode
8095:Bibcode
8046:Bibcode
8009:4409319
7981:Bibcode
7927:Bibcode
7894:5965082
7874:Bibcode
7821:Bibcode
7785:4312220
7757:Bibcode
7702:Bibcode
7643:Bibcode
7586:Bibcode
7532:Bibcode
7490:Bibcode
7444:Bibcode
7407:Bibcode
7380:Bibcode
7335:Bibcode
7276:Bibcode
7234:Bibcode
7178:Bibcode
7125:Bibcode
7066:Bibcode
7017:Bibcode
6974:Bibcode
6927:Bibcode
6886:Bibcode
6839:Bibcode
6801:Bibcode
6789:: 138.
6750:Bibcode
6704:Bibcode
6657:Bibcode
6617:8057181
6597:Bibcode
6543:Bibcode
6489:Bibcode
6435:Bibcode
6382:Bibcode
6326:Bibcode
6273:Bibcode
6222:Bibcode
6176:Bibcode
6134:Bibcode
6132:: L55.
6097:Bibcode
6095:: 357.
6040:Bibcode
6038:: L65.
6003:Bibcode
5964:Bibcode
5962:: 519.
5921:Bibcode
5868:Bibcode
5856:: A14.
5820:Bibcode
5786:Bibcode
5784:: 171.
5724:Bibcode
5677:Bibcode
5624:Bibcode
5588:Bibcode
5586:: 867.
5545:Bibcode
5483:Bibcode
5432:Bibcode
5391:Bibcode
5352:Bibcode
5350:: 181.
5304:Bibcode
5266:Bibcode
5264:: 153.
5160:Bibcode
5114:Alt URL
5089:Bibcode
5051:Bibcode
5003:Bibcode
4947:Bibcode
4935:: A14.
4907:Bibcode
4870:Bibcode
4843:9385537
4815:Bibcode
4768:Bibcode
4727:Bibcode
4677:Bibcode
4626:Bibcode
4576:Bibcode
4526:Bibcode
4463:Bibcode
4414:怩ææèČèłèšç¶Č
4322:Bibcode
4266:Bibcode
4155:Bibcode
4094:7323744
4071:Bibcode
4009:Bibcode
3985:2022).
3952:Bibcode
3916:1845338
3896:Bibcode
3836:Bibcode
3772:Bibcode
3723:Bibcode
3655:Bibcode
3595:Bibcode
3533:Bibcode
3493:Bibcode
3460:Bibcode
3458:: L49.
3402:Bibcode
3364:Bibcode
3326:5032987
3306:Bibcode
3238:Bibcode
3192:Bibcode
3147:Bibcode
3105:Bibcode
3043:Bibcode
3041:: L27.
2879:SN 1006
2492:⁄
2201:P Cygni
1923:of the
1919:in the
1789:Ariel 5
1534:at the
1395:ionised
1381:of the
1379:profile
1347:radiant
1289:in the
1194:Canopus
1121:Wergaia
1093:Canopus
954:Sequens
903:radiant
837:with a
782:parsecs
780:(2,300
764:, is a
594:η Car B
491:η Car A
486:Details
481:2009.03
410:2,022.7
396:η Car B
386:η Car A
382:Primary
73:Equinox
10665:RCW 49
10345:WR 42e
10340:WR 31a
10335:WR 30a
10315:WR 21a
10310:WR 20a
9873:PP (p)
9596:
9543:
9460:
9452:
9409:
9350:
9293:
9240:
9232:
9179:
9099:
9046:
9038:
8978:
8925:
8826:
8768:
8708:
8649:
8596:
8537:
8473:
8414:
8317:
8291:Nature
8273:
8220:
8166:
8066:
8007:
7999:
7963:Nature
7945:
7892:
7839:
7783:
7775:
7739:Nature
7722:
7663:
7604:
7550:
7462:
7405:: 51.
7378:: 93.
7355:
7294:
7252:
7196:
7143:
7086:
7027:
7015:: L5.
6992:
6857:
6770:
6677:
6615:
6561:
6507:
6453:
6400:
6344:
6291:
6068:
5939:
5886:
5759:
5695:
5642:
5563:
5509:
5501:
5465:Nature
5430:: 23.
5322:
5276:
5239:
5212:
5187:
5107:
5021:
4965:
4841:
4833:
4697:
4594:
4544:
4393:
4365:
4342:
4239:
4206:
4175:
4109:
4101:
4091:
4029:
3914:
3854:
3743:
3675:
3615:
3551:
3521:: L6.
3420:
3324:
3256:
3167:
3061:
2902:nearby
2807:nickel
2449:Hubble
1863:Masing
1785:HEAO-2
1635:lasing
1608:and Cr
1595:Hubble
1345:has a
1267:NuSTAR
1114:binary
983:Carina
960:. His
901:has a
839:period
789:Carina
736:SIMBAD
621:Radius
551:
527:
518:Radius
418:(5.54
403:Period
263:binary
261:&
248:+0.61
237:â0.45
86:Carina
75:J2000
45:Credit
10824:Stars
10703:Other
10618:Other
10493:Other
10330:WR 25
10325:WR 24
10320:WR 22
10238:Other
10229:97950
10224:95086
10219:93403
10214:93250
10209:93129
10204:85628
10199:65216
10189:53143
9737:Bayer
9728:Stars
9594:S2CID
9568:arXiv
9541:S2CID
9515:arXiv
9458:S2CID
9407:S2CID
9379:arXiv
9348:S2CID
9322:arXiv
9291:S2CID
9265:arXiv
9238:S2CID
9204:arXiv
9177:S2CID
9151:arXiv
9097:S2CID
9071:arXiv
9044:S2CID
9010:arXiv
8976:S2CID
8950:arXiv
8923:S2CID
8897:arXiv
8852:arXiv
8824:S2CID
8798:arXiv
8766:S2CID
8740:arXiv
8706:S2CID
8678:arXiv
8647:S2CID
8621:arXiv
8594:S2CID
8566:arXiv
8535:S2CID
8507:arXiv
8471:S2CID
8443:arXiv
8412:S2CID
8384:arXiv
8315:S2CID
8271:S2CID
8245:arXiv
8218:S2CID
8192:arXiv
8164:S2CID
8136:arXiv
8064:S2CID
8036:arXiv
8005:S2CID
7971:arXiv
7943:S2CID
7917:arXiv
7890:S2CID
7864:arXiv
7837:S2CID
7811:arXiv
7781:S2CID
7747:arXiv
7720:S2CID
7692:arXiv
7661:S2CID
7633:arXiv
7602:S2CID
7576:arXiv
7548:S2CID
7522:arXiv
7460:S2CID
7434:arXiv
7353:S2CID
7325:arXiv
7250:S2CID
7224:arXiv
7194:S2CID
7168:arXiv
7141:S2CID
7115:arXiv
7084:S2CID
7056:arXiv
6990:S2CID
6964:arXiv
6861:. 12.
6855:S2CID
6829:arXiv
6791:arXiv
6768:S2CID
6740:arXiv
6675:S2CID
6647:arXiv
6613:S2CID
6587:arXiv
6559:S2CID
6533:arXiv
6505:S2CID
6479:arXiv
6451:S2CID
6425:arXiv
6398:S2CID
6372:arXiv
6342:S2CID
6316:arXiv
6289:S2CID
6263:arXiv
6195:(PDF)
6164:(PDF)
6066:S2CID
5937:S2CID
5911:arXiv
5884:S2CID
5858:arXiv
5693:S2CID
5667:arXiv
5561:S2CID
5535:arXiv
5507:S2CID
5473:arXiv
5320:S2CID
5105:S2CID
5079:arXiv
5019:S2CID
4993:arXiv
4963:S2CID
4937:arXiv
4905:: 1.
4839:S2CID
4805:arXiv
4695:S2CID
4667:arXiv
4592:S2CID
4542:S2CID
4516:arXiv
4485:gurrk
4387:äžćæćș§ç„
4173:S2CID
4145:arXiv
4107:S2CID
4061:arXiv
3999:arXiv
3912:S2CID
3886:arXiv
3852:S2CID
3826:arXiv
3741:S2CID
3713:arXiv
3673:S2CID
3645:arXiv
3613:S2CID
3585:arXiv
3549:S2CID
3523:arXiv
3491:: 0.
3362:: 0.
3322:S2CID
3296:arXiv
3254:S2CID
3228:arXiv
3137:arXiv
2937:Notes
2875:Venus
2143:Orbit
2104:2,900
2096:9,500
2061:2,600
2053:0.383
1947:WR 25
1847:21 cm
1839:Radio
1828:Fermi
1824:AGILE
1804:ROSAT
1793:OSO 8
1781:Uhuru
1773:X-ray
1679:maser
1614:Lyman
1501:star
1480:novae
1383:lines
1082:Rigel
991:Gould
870:laser
828:Cairo
797:Rigel
758:η Car
721:AAVSO
523:~240
474:epoch
375:Orbit
318:Dec.:
226:0.94
215:2.51
204:3.39
193:4.90
182:6.82
171:6.37
69:Epoch
40:WFPC2
10694:3059
10609:3586
10604:3584
10599:3582
10594:3581
10589:3579
10584:3576
10579:3199
10574:2867
10484:3603
10479:3532
10474:3324
10469:3293
10464:3114
10459:2808
10454:2516
10435:Star
10161:4222
10156:4205
10136:4142
10008:V906
10003:V817
9998:V816
9993:V759
9988:V752
9983:V742
9978:V640
9973:V602
9968:V560
9958:V528
9948:V518
9918:V372
9888:V341
9450:PMID
9230:PMID
9036:PMID
7997:PMID
7773:PMID
7292:ISBN
7025:ISSN
5757:ISBN
5663:1411
5640:ISSN
5499:PMID
5274:ISSN
5237:ISBN
5210:ISBN
5185:ISBN
5137:2018
5130:NASA
4903:6368
4831:PMID
4454:1825
4431:2012
4391:ISBN
4363:ISBN
4340:ISSN
4237:ISBN
4204:ISBN
4099:PMID
4027:ISSN
3418:ISBN
3360:2237
3165:ISSN
3059:ISBN
2971:wind
2955:wind
2841:and
2835:Lynx
2542:Size
2424:and
2235:Mass
1857:and
1775:and
1714:and
1712:mid-
1663:ions
1655:pump
1600:The
1377:and
1373:The
1369:CCD)
1206:dust
1015:and
976:and
930:and
742:data
713:IRAS
601:Mass
498:Mass
242:BâV
231:UâB
55:NASA
34:The
10687:NGC
10567:NGC
10446:NGC
9586:doi
9564:326
9533:doi
9484:212
9442:doi
9430:184
9397:doi
9375:438
9340:doi
9318:528
9283:doi
9261:645
9222:doi
9200:337
9169:doi
9147:591
9120:223
9089:doi
9067:778
9028:doi
9006:337
8968:doi
8946:679
8915:doi
8893:537
8816:doi
8794:558
8758:doi
8736:564
8696:doi
8674:433
8639:doi
8617:799
8584:doi
8562:456
8525:doi
8503:480
8461:doi
8439:463
8402:doi
8380:415
8350:doi
8338:281
8307:doi
8295:390
8263:doi
8241:139
8210:doi
8188:410
8154:doi
8132:436
8103:doi
8091:154
8054:doi
8032:415
7989:doi
7967:447
7935:doi
7913:122
7882:doi
7860:612
7829:doi
7765:doi
7743:455
7710:doi
7688:447
7651:doi
7629:447
7594:doi
7572:578
7540:doi
7518:751
7486:207
7452:doi
7430:143
7343:doi
7284:doi
7242:doi
7220:716
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