781:
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675:
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In practice, it is challenging to ascertain whether the arms of a given galaxy are leading or trailing. To observe the spiral structure, the galaxy should not be tilted excessively towards the picture plane. However, a slight tilt is necessary to determine the direction of rotation. Additionally, the side of the galaxy closer to the observer needs to be identified. A review of the observational data indicates that the majority of galaxies exhibit trailing spiral arms, with leading arms being relatively uncommon. For instance, among the two hundred galaxies studied in this manner, only two may have leading arms. In some instances, galaxies exhibit both leading and trailing spiral arms, as exemplified by
989:
124:
393:
432:
1063:, which describe disparate variants of the spiral structure. The first explanation posits that spiral arms are perpetually forming and dissipating without sufficient time to undergo significant twisting – such spiral arms are designated as material arms. The density wave theory posits that the spiral pattern is a density wave, thereby rotating independently of the disc as a solid body. Consequently, spiral arms are designated as wave arms. It is possible for these types of spiral arms to occur simultaneously within the same galaxy.
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regions where the concentration of stars is higher. Concurrently, at various points in time, different stars emerge within the spiral arm, resulting in the density wave moving at a different speed than the stellar disc. Consequently, the density wave is not subject to twisting. The influence of this mechanism results in the formation of a large-scale, ordered spiral structure, which is also observed in the infrared. The concentration of stars in the spiral arm increases by a mere 10-20%, yet this relatively modest change in
368:
ordered two-arm structure in the interior, which becomes irregular at the periphery. Nevertheless, in almost all cases, both types of structure are present in the spiral structure. Even grand design galaxies have details that do not fit into the spiral pattern. Additionally, there are galaxies that exhibit different types of spiral structure when observed across different spectral ranges. The distinction between the two main types of spiral arms appears to be related to fundamental physical differences between them.
1128:
222:
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940:. In galaxies with a pronounced spiral pattern, the magnetic fields are orientated along the arms. However, in some cases, the magnetic field may form a separate spiral structure that runs in the space between the visible spiral arms. Conversely, magnetic fields can influence the movement of gas within the galaxy and contribute to the formation of spiral arms. However, they are insufficiently strong to play a dominant role in the formation of spiral arms.
527:. In the case of the logarithmic spiral, the pitch angle is constant. It decreases with increasing distance from the centre in the Archimedean spiral and increases in the hyperbolic spiral. The measurements of twist angles in galaxies indicate that only a minority of spiral galaxies have pitch angles of the arms that are close to constant. More than two-thirds of galaxies have pitch angles that vary by more than 20%. The average twist angle is found to
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308:
323:
1233:. In contrast to the density wave theory, the manifold theory does not posit the emergence of colour gradients in spiral arms, which are in fact observed in numerous galaxies. The fact that in galaxies with a bar, spiral arms originate from a region proximate to the bar may suggest a correlation between these structures and the manifold theory. However, this is not the sole theory that explains the genesis of arms due to bars.
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region allows it to stretch into a short arc. Given that starburst is a continuous process occurring in different regions of the disc, there are numerous such arcs at different times throughout the disc, which can be observed as a flocculent spiral pattern. Given that such spiral arms are only visible due to young stars, they have a minimal impact on the mass distribution within the galaxy and are rarely observed in the
17:
408:
1155:, which is a region where the spiral arm moves at the same speed as the stars. It can be identified by observing colour gradients within the arms. Since the stellar population forms within an arm and subsequently reddens over time, a colour gradient should be observed across the arm if its velocity differs from that of the arm. It is hypothesised that density waves are created and maintained by the
1085:
1242:
512:. The pitch angle is the angle between the tangent to spiral arm at a given point and the perpendicular to the radius drawn to that point. In the majority of spiral galaxies, the average pitch angle lies within the range of 5° to 30°. Spiral arms with a small pitch angle are called tightly wound, while those with a larger pitch angle are called open.
295:, spiral galaxies are divided into types Sa, Sb, Sc. Barred spiral galaxies are divided into types SBa, SBb and SBc. The spiral arms of early type Sa and SBa galaxies are tightly wound and smooth, while those of late type Sc and SBc galaxies are knotty and loosely wound. Types Sb and SBb exhibit intermediate characteristics.
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occur within a disc, giving rise to a density wave - the stars move within the disc in such a way that they converge in specific regions and become more concentrated. The density wave exerts a governing influence not only on the stars but also on the gas, thereby promoting a more active starburst in
847:
Spiral arms may additionally be categorized as either trailing or leading. In the case of trailing spiral arms, their outer tips point in the direction opposite to the direction of galaxy rotation. In the case of leading arms, their outer tips point in the same direction in which the galaxy rotates.
157:
they originate at the ends of the bar. The spiral arms do not extend over the entire radius of the disc and cease at the distance at which the disc can still be discerned. A galaxy typically comprises two or more spiral arms. The collective configuration of these arms within a galaxy is referred to
1220:
Some theories propose alternative mechanisms for the appearance of spiral arms that differ from the density wave theory and the SSPSF model. These theories are not intended to replace the aforementioned theories entirely, but rather to explain the appearance of spiral arms in specific cases. For
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The remainder of the galaxies are of an intermediate type, referred to as "multi-armed", which exhibit the proberties of both the flocculent and grand design galaxies. For example, they may appear to be grand design galaxies, yet possess more than two arms. Alternatively, they may exhibit a more
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in the gas, thereby facilitating the spread of star formation across the galactic disk. In a period of less than 100 million years, the brightest stars in this region have time to extinguish. This is less than the time required for one revolution of the galaxy. The differential rotation of this
1260:
In 1896, the problem of twisting was formulated. If spiral arms were material entities, due to differential rotation, they would twist very rapidly to the point where they would be impossible to observe. Consequently, the question of the nature of the spiral structure remained unresolved for a
972:
as one of the classification criteria, subsequent analysis has revealed that this value correlates with the morphological type to a lesser extent than, for example, the indicator of the colour of the spiral arms. The correlation between the pitch angle and the aforementioned parameters can be
885:
The ratio of the luminosity of the spiral structure to the luminosity of the entire galaxy is greatest for grand design spiral galaxies. For these galaxies, this ratio is 21% on average, with some reaching as high as 40-50%. For flocculent and multi-arm galaxies, the ratio is 13% and 14%,
421:
Additionally, spiral arms are subdivided into two categories: massive and filamentary. In the first instance, the spiral arms are wide, diffuse, and do not contrast significantly with the space between them. In contrast, in the second instance, the spiral arms are narrow and clearly
1225:. According to this theory, the gravitational influence of the bar causes the orbits of the stars to be arranged in a certain way, creating spiral arms and moving along them. The name of the theory is related to the fact that in this model the stars moving in spiral arms form a
1170:
The density wave theory postulates that only trailing spiral arms are stable, and that any leading structure must at some point transition into a trailing one. Concurrently, the structure itself is amplified for a period following the transformation, which is called swing
1204:
1202:
1186:
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The classification of galaxies into flocculent, multi-armed, and grand design categories is derived from a more complex morphological classification scheme involving 10 classes that describe the type of spiral pattern. The classification scheme was developed by
1203:
1185:
265:, older stars contribute more, which makes the spiral arms appear smoother, but less contrasted. Radiation from interstellar dust makes the spiral arms bright in the far infrared, while radiation from neutral hydrogen and molecules makes them bright at
1201:
1183:
104:. These theories describe different variants of the spiral structure and do not exclude each other. In addition to these theories, there are other theories that can explain the appearance of spiral structure in some cases.
886:
respectively. Additionally, the proportion of spiral arms in the total luminosity increases in later morphological types. For Sa-type galaxies, this proportion averages 13%, while for Sc-type galaxies it averages 30%.
84:
can reach 40–50% for some galaxies. The characteristics of spiral arms are correlated with other properties of galaxies, for example, the twist angle of spiral arms is related to parameters such as the mass of the
218:, and bright stars than in the remainder of the disk. While spiral arms are primarily identifiable due to their young stellar population, there also exists an increased concentration of old stars within them.
2943:"The start of the Sagittarius spiral arm (Sagittarius origin) and the start ot the Norma spiral arm (Norma origin): Model-computed and observed arm tangents at galactic longitudes −20° < l < +23°"
1069:
observed in interacting galaxies are also considered material spiral arms. Due to the low velocity of matter at a distance from the galaxy, tidal tails appear to persist for an extended period of time.
360:
exhibit a symmetrical and clear pattern comprising two spiral arms that extend throughout the galaxy. They account for 10% of the total number of spiral galaxies. In contrast, the spiral structure of
1055:
rather than as solid bodies, any structure in the disc should curve significantly and disappear in approximately one to two revolutions. The two most prevalent solutions to this issue are the
973:
theoretically explained. The described quantities are related to the mass distribution within the galaxy, which affects the manner in which the density wave propagates within the galaxy disc.
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In more massive galaxies with a more ordered structure, spiral arms are observed to be more pronounced and contrasting. Additionally, the contrast between spiral arms is more pronounced in
825:
772:
719:
666:
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The precise location, length, and number of spiral arms remain uncertain. However, the prevailing view is that the Milky Way contains four major spiral arms: two main ones - the
613:
46:. Typically, spiral galaxies exhibit two or more spiral arms. The collective configuration of these arms is referred to as the spiral pattern or spiral structure of the galaxy.
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1182:
968:
appear to be more increasing. However, these dependencies are not particularly pronounced. Although the pitch angle of the spiral arms was originally introduced into the
863:
The width of spiral arms in the majority of galaxies increases with increasing distance from the centre. Grand design galaxies exhibit the greatest width of spiral arms.
189:
561:
510:
487:
1311:
Despite the considerable successes of the density wave theory, the physical nature of spiral arms remains a topic of debate, with no clear consensus yet reached.
1746:
Bittner, A.; Gadotti, D.A.; Elmegreen, B.G.; Athanassoula, E.; Elmegreen, D.M.; Bosma, A.; Muñoz-Mateos, J. (2020-01-01). Valluri, M.; Sellwood, J.A. (eds.).
980:, although this correlation is relatively weak. In general, flocculent galaxies have a lower mass and a later morphological type than grand design galaxies.
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364:
consists of numerous small fragments of arms that are not connected to each other. Among spiral galaxies, the fraction of such galaxies is equal to 30%.
2779:
2714:
2505:
2258:
2123:
1992:
1265:, who in 1961 correctly concluded that the spiral arms arise due to gravitational interaction between the stars in the disc. Subsequently, in 1964,
3257:
Peterken, T.G.; Merrifield, M.R.; Aragón-Salamanca, A.; Drory, N.; Krawczyk, C.M.; Masters, K.L.; Weijmans, A.-M.; Westfall, K.B. (February 2019).
1151:
It is challenging to confirm the presence of a density wave in practice. However, it is possible to do so, for instance, by detecting a specific
2051:
Shields, D.; Boe, B.; Pfountz, C.; Davis, B.L.; Hartley, M.; Miller, R.; Slade, Z.; Abdeen, M.S.; Kennefick D., D.; Kennefick, J. (2022-10-01).
780:
727:
674:
621:
568:
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becomes active within a region of the galaxy. The presence of young, bright stars in this region has the effect of influencing the surrounding
53:
exhibit a symmetrical and distinct pattern, comprising two spiral arms that extend throughout the galaxy. In contrast, the spiral structure of
4682:
3740:
Shields, D.; Boe, B.; Pfountz, C.; Davis, B.L.; Hartley, M.; Miller, R.; Slade, Z.; Abdeen, M.S.; Kennefick, D.; Kennefick, J. (2022-10-01).
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with other galaxy properties. For instance, it is established that galaxies with a greater pitch angle typically exhibit a lower mass of the
4332:
3215:
2342:
1816:
3152:
198:
The spiral arms exhibit considerable variation in their appearance. In general, they are characterized by an increased concentration of
1004:
through optical observation, given that the Sun is situated within the plane of the Milky Way disc, and the light is being absorbed by
3479:
3203:
2423:
1948:
1804:
1492:
2501:"Updating the (supermassive black hole mass)-(spiral arm pitch angle) relation: a strong correlation for galaxies with pseudobulges"
900:(anemic spirals). These galaxies are distinguished by a diffuse, faint spiral pattern, which is attributed to a reduced quantity of
3672:
3603:
3546:
3388:
2999:
2877:
2565:
1747:
1692:
932:
are observed in the spiral arms than in the remainder of the galaxy. The average value of magnetic fields in spiral galaxies is 10
1621:
1051:
The prevalence of spiral galaxies indicates that spiral structure is a long-lived phenomenon. However, since galaxies themselves
57:
comprises numerous small fragments of arms that are not connected to each other. The appearance of spiral arms varies across the
3258:
2842:
1420:
1296:
in our galaxy were measured with a high degree of accuracy. This enabled the discovery of a spiral structure in the Milky Way.
1277:
that spiral arms can be conceptualised as density waves. The SSPSF model was first proposed in 1978, although the concept of a
4017:
3957:
3930:
3899:
3860:
3835:
2708:
Bittner, A.; Gadotti, D.A.; Elmegreen B.G.; Athanassoula, E.; Elmegreen, D.M.; Bosma, A.; Muñoz-Mateos, J.-C. (2017-10-01).
1748:"The sequence of spiral arm classes: Observational signatures of persistent spiral density waves in grand-design galaxies"
4065:
969:
392:
285:
3000:"The Spiral Arms of the Milky Way: The Relative Location of Each Different Arm Tracer within a Typical Spiral Arm Width"
4748:
4667:
1428:
1331:
4048:
3891:
3157:
2566:"Constraining Dark Matter Halo Profiles and Galaxy Formation Models Using Spiral Arm Morphology. I. Method Outline"
2435:
2195:
1953:
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1144:
has a profound impact on the gas dynamics. The gas accelerates, and shock waves can occur in it, appearing as dark
916:, which results in the rapid loss of gas. It is hypothesized that this type of galaxy may be in-between spiral and
908:
rate in comparison to normal spiral galaxies of the same morphological type. Anemic galaxies are more prevalent in
3324:"Precision Determination of Corotation Radii in Galaxy Disks: Tremaine–Weinberg versus Font–Beckman for NGC 3433"
431:
4753:
856:
have demonstrated that leading spiral arms can emerge in specific circumstances. One such instance is when the
145:
and exhibit heightened brightness relative to their surrounding environment. Such structures take the form of
4480:
992:
A model of the Milky Way. The yellow dot indicates the position of the Sun, the red dots the position of the
161:
Around two thirds of all massive galaxies are spiral galaxies. Spiral arms have been observed in galaxies at
377:
195:
was less than half of the present one. This suggests that the spiral structure is a long-lived phenomenon.
789:
736:
683:
630:
4650:
2775:"Identification of Grand-design and Flocculent spirals from SDSS using deep convolutional neural network"
577:
4768:
4723:
4590:
4531:
4427:
4120:
4115:
4088:
3922:
3484:
3112:
1759:
1497:
988:
446:
407:
357:
269:. The greatest contrast and amount of fine detail in spiral arms can be seen when observed in emission
50:
4369:
889:
The colour of the spiral arms becomes increasingly blue for galaxies of late morphological types. The
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4147:
3677:
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3393:
3328:
2637:
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1308:
in 1987. Subsequently, they proposed a simplified scheme, which is the one that is currently in use.
531:
with a number of different galaxy parameters. For example, the spiral arms of galaxies with brighter
4672:
2254:"A multiwavelength study of spiral structure in galaxies. I. General characteristics in the optical"
115:. The nature of spiral structure in galaxies remained unresolved for a considerable period of time.
64:
In addition to increased brightness, spiral arms are characterised by an increased concentration of
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3004:
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540:
300:
278:
250:
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The appearance and expression of spiral branches in a galaxy may vary depending on the part of the
226:
58:
2710:"How do spiral arm contrasts relate to bars, disc breaks and other fundamental galaxy properties?"
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4713:
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4319:
4307:
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1141:
953:
86:
168:
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150:
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1052:
893:
g-r for Sc-type galaxies is approximately 0.3-0.4, while for Sa-type galaxies it is 0.5-0.6.
337:
123:
3511:
3223:
3129:
3107:
2453:
2213:
2183:
1824:
1524:
1008:. Nevertheless, spiral arms can be observed, for instance, when mapping the distribution of
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3621:
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2015:
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154:
131:
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in different directions, indicating the presence of both leading and trailing spiral arms.
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8:
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4157:
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101:
65:
54:
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2150:
2082:
2019:
1894:
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1832:
1789:
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1732:
1712:
943:
28:
Spiral-shaped regions of enhanced brightness within the galactic disc in spiral galaxies
4856:
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4778:
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4558:
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4337:
3995:
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2727:
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2439:
2271:
2199:
2136:
2068:
2005:
1763:
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520:
516:
307:
230:
3428:
3108:"Stochastic self-propagating star formation with anisotropic probability distribution"
2915:
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4798:
4773:
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4622:
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4454:
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2299:
2225:
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1906:
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1152:
1131:
Schematic representation of colour gradients in spiral arms if they are density waves
1005:
917:
524:
3308:
3029:
2852:
1493:"The shapes of spiral arms in the S4G survey and their connection with stellar bars"
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4828:
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4605:
4585:
4580:
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4422:
4243:
4176:
4005:
3775:
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3515:
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3292:
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3227:
3025:
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2911:
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2601:
2536:
2457:
2394:
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2217:
2154:
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2023:
1898:
1828:
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1528:
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1250:
1164:
1093:
993:
905:
901:
857:
238:
207:
199:
73:
21:
3519:
1622:"Звёздная астрономия в лекциях. 17.1 Наблюдательные данные о спиральной структуре"
1532:
1035:
arms. Their pitch angle is approximately 12°, and their width is estimated at 800
322:
191:, and on occasion even at greater distances, which corresponds to a time when the
4677:
4600:
4292:
4265:
4236:
4188:
4034:
3912:
3873:
2788:
2723:
2514:
2267:
2132:
2001:
1305:
1301:
1262:
1135:
In the context of density wave theory, spiral arms are understood to emerge when
1032:
1013:
965:
437:
398:
292:
274:
258:
138:
35:
356:
The spiral structure of galaxies exhibits considerable diversity in appearance.
4541:
4374:
4277:
4272:
4226:
4169:
3949:
3686:
3617:
3560:
3402:
3364:
3337:
3323:
3013:
2956:
2889:
2673:
2646:
2632:
2579:
1902:
1720:
1266:
957:
929:
909:
532:
257:
parts of the spectrum, the spiral arms are well defined due to the presence of
96:
Two main theories have been proposed to explain the origin of spiral arms: the
90:
77:
4009:
3296:
2461:
2399:
2372:
2221:
1785:
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as early as 1953. This observation formed the basis of the subsequent theory.
1175:
Influence of differential rotation on the structure of spiral arms (animation)
1127:
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4697:
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4526:
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4095:
3967:
3887:
3789:
3780:
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3584:
3527:
3436:
3387:
Martínez-García, E.E.; González-Lópezlira, R.A.; Bruzual-A, G. (2009-03-01).
3373:
3304:
3239:
3137:
3037:
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2759:
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2100:
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considerable period of time. Since 1927, this question has been addressed by
1009:
897:
879:
270:
262:
221:
142:
43:
3855:] (in Russian) (2, revised and supplemented ed.). Fryazino: Век 2.
3153:"Structure and Evolution of Irregular Galaxies. 4.3 SSPSF: A Possible Model"
2750:
2709:
2541:
2500:
2294:
2253:
2028:
1987:
1286:
4595:
4536:
4521:
4352:
4137:
3493:
3121:
2377:
1506:
1491:
Díaz-García, S.; Salo, H.; Knapen, J.H.; Herrera-Endoqui, M. (2019-11-01).
913:
289:
211:
69:
3943:
3386:
1039:. In addition to the large arms, smaller, similar formations, such as the
1000:
It is challenging to ascertain the presence of spiral arms in the disc of
956:
at their centre and a smaller galaxy mass in general. Additionally, their
153:
usually originate from a region near the centre of the galaxy, whereas in
80:
strength in galaxies. The contribution of spiral arms to the total galaxy
4610:
4500:
4490:
4287:
4253:
4193:
4073:
3389:"Spiral Density Wave Triggering of Star Formation in SA and SAB Galaxies"
2588:
2204:
1230:
1160:
1136:
1079:
1056:
1024:
890:
528:
465:
254:
234:
215:
203:
97:
2707:
2633:"On the Connection between Spiral Arm Pitch Angle and Galaxy Properties"
1658:
1467:
1365:
515:
The shape of spiral arms is often described in a simplified manner as a
4495:
4432:
3883:
3872:
Karttunen, H.; Kroger, P.; Oja, H.; Poutanen, M.; Donner, K.J. (2016).
3322:
Beckman, J.E.; Font, J.; Borlaff, A.; García-Lorenzo, B. (2018-02-26).
3256:
2119:"Bar-driven leading spiral arms in a counter-rotating dark matter halo"
1254:
1105:
1066:
1001:
937:
933:
452:
383:
266:
112:
108:
81:
3259:"A direct test of density wave theory in a grand-design spiral galaxy"
2252:
Savchenko, S.; Marchuk, A.; Mosenkov, A.; Grishunin, K. (2020-03-01).
539:
Several galaxies for which measurements of the pitch angle were made,
4505:
3918:
1270:
1145:
1040:
1028:
949:
944:
Correlation between spiral arm parameters and other galaxy properties
1490:
137:
Spiral arms are a defining feature of the structural composition of
3762:
3702:
3633:
3576:
3502:
3346:
3279:
2965:
2898:
2797:
2773:
Sarkar, S.; Narayanan, G.; Banerjee, A.; Prakash, P. (2023-01-01).
2732:
2655:
2605:
2523:
2444:
2276:
2141:
2073:
1768:
1745:
1515:
1226:
1110:
1084:
875:
849:
837:
413:
343:
313:
242:
162:
127:
4000:
3480:"Manifold spirals in barred galaxies with multiple pattern speeds"
3411:
2010:
871:
832:
3477:
3162:
2564:
Seigar, M.S.; Bullock, J.S.; Barth, A.J.; Ho, L.C. (2006-07-01).
2251:
1958:
492:
The shape of the arm is usually parameterised by the pitch angle
16:
3478:
Efthymiopoulos, C.; Harsoula, M.; Contopoulos, G. (2020-04-01).
3321:
4342:
4327:
4057:
3879:
3827:
1036:
146:
39:
2772:
1192:"Material" spiral arms twist greatly in a short amount of time
4415:
4410:
4405:
4362:
1886:
1704:
3604:"Stochastic star formation and spiral structure of galaxies"
1241:
960:
contributes less to the total luminosity, they have a lower
912:. Apparently, the galaxies in these clusters are subject to
4026:
3753:
2064:
3742:"Spirality: A Novel Way to Measure Spiral Arm Pitch Angle"
2053:"Spirality: A Novel Way to Measure Spiral Arm Pitch Angle"
1046:
328:
284:
The appearance of spiral arms is one of the criteria for
1057:
stochastic self-propagating star formation model (SSPSF)
299:
Spiral galaxies of different morphological types in the
3826:] (in Russian) (2, rev. and supplement ed.).
3739:
2499:
Davis, B.L.; Graham, A.W.; Seigar, M.S. (2017-10-01).
2050:
2116:
792:
739:
686:
633:
580:
549:
498:
475:
171:
107:
The spiral structure was first identified in 1850 by
3982:
Buta, R.J. (2011). Oswalt, T.D.; Keel, W.C. (eds.).
2563:
1221:
instance, the manifold theory is applicable only to
1210:
Density waves create arms that don't twist over time
1092:
The SSPSF model posits that spiral arms emerge when
983:
2181:
2117:Lieb E.; Collier, A.; Madigan, A.-M. (2022-01-01).
996:, which serve as indicators of the spiral structure
519:. However, spiral arms may also be described as an
426:
Galaxies with different spiral structure morphology
372:
Galaxies with different spiral structure morphology
49:The appearance of spiral sleeves is quite diverse.
3670:
819:
766:
713:
660:
607:
555:
504:
481:
183:
42:-shaped regions of enhanced brightness within the
2780:Monthly Notices of the Royal Astronomical Society
2715:Monthly Notices of the Royal Astronomical Society
2506:Monthly Notices of the Royal Astronomical Society
2498:
2259:Monthly Notices of the Royal Astronomical Society
2124:Monthly Notices of the Royal Astronomical Society
1993:Monthly Notices of the Royal Astronomical Society
4843:
3910:
1593:
98:stochastic self-propagating star formation model
3671:Elmegreen, D.M.; Elmegreen, B.G. (1987-03-01).
3105:
1338:. Vol. 6. pp. 298–301. Archived from
1285:in neighbouring regions was first proposed by
4683:List of the most distant astronomical objects
4042:
1752:Galactic Dynamics in the Era of Large Surveys
1249:The spiral arms were first discovered in the
3846:
3601:
3186:
3081:
2182:Capozziello, S.; Lattanzi, A. (2006-01-01).
1860:
1569:
1404:
3208:Annual Review of Astronomy and Astrophysics
3204:"Six Decades of Spiral Density Wave Theory"
3150:
1988:"Pitch angle variations in spiral galaxies"
1809:Annual Review of Astronomy and Astrophysics
1805:"Six Decades of Spiral Density Wave Theory"
1088:Emergence of spiral arms in the SSPSF model
4049:
4035:
3547:"On the Spiral Structure of Disk Galaxies"
1875:"Spiral Arm Morphology of Nearby Galaxies"
1693:"Spiral Arm Morphology of Nearby Galaxies"
860:rotates in opposition to the galaxy disk.
118:
89:at the centre and the contribution of the
3999:
3779:
3761:
3673:"Arm Classifications for Spiral Galaxies"
3501:
3410:
3363:
3345:
3278:
2974:
2964:
2897:
2814:
2796:
2749:
2731:
2672:
2654:
2587:
2540:
2522:
2443:
2398:
2293:
2275:
2203:
2158:
2140:
2090:
2072:
2027:
2009:
1985:
1767:
1514:
1257:identified the spiral structure in 1850.
253:in which it is observed. In the blue and
158:as a spiral pattern or spiral structure.
3106:Jungwiert, B.; Palous, J. (1994-07-01).
1889:: Korean Astronomical Society: 141–149.
1707:: Korean Astronomical Society: 141–149.
1240:
1126:
1083:
987:
870:
866:
831:
464:
460:
220:
122:
15:
3602:Gerola, H.; Seiden, P.E. (1978-07-01).
2878:"The spiral structure of the Milky Way"
2875:
1215:
1047:Theories on the spiral structure origin
24:(M51) has a pronounced spiral structure
4844:
3941:
3817:
3802:
3658:
3544:
3465:
3453:
3197:
3195:
3093:
3077:
3075:
3066:
3054:
2997:
2940:
2882:Research in Astronomy and Astrophysics
2876:Xu, Y.; Hou, L.; Wu, Y. (2018-12-01).
2871:
2869:
2836:
2834:
2695:
2486:
2316:
1879:Journal of Korean Astronomical Society
1872:
1856:
1854:
1697:Journal of Korean Astronomical Society
1690:
1651:"Физика галактик и галактических ядер"
1557:
1292:In 1953, the distances to the various
1116:
936:, while in their spiral arms it is 25
4030:
3871:
2247:
2245:
2243:
2241:
2239:
2112:
2110:
1981:
1979:
1616:
1614:
1581:
1385:
3981:
3727:
2630:
2424:"Magnetic fields in spiral galaxies"
2421:
2370:
2328:
2184:"Spiral Galaxies as Chiral Objects?"
1935:
1923:
1678:
1605:
1486:
1484:
1457:
1453:
1451:
1449:
1415:
1413:
1400:
1398:
1396:
1394:
1351:
1349:
1325:
1323:
820:{\displaystyle \mu =45{,}1^{\circ }}
767:{\displaystyle \mu =29{,}7^{\circ }}
714:{\displaystyle \mu =25{,}7^{\circ }}
661:{\displaystyle \mu =12{,}6^{\circ }}
3988:Planets, Stars, and Stellar Systems
3911:Binney, J.; Merrifield, M. (1998).
3847:Засов, А.В.; Постнов, К.А. (2011).
3545:Lin, C.C.; Shu, F.H. (1964-08-01).
3232:10.1146/annurev-astro-081915-023426
3201:
3192:
3151:Gallagher, J.S. III.; Hunter, D.A.
3072:
2866:
2831:
2340:
1873:Ann, H.B.; Lee, H-R. (2013-06-01).
1851:
1833:10.1146/annurev-astro-081915-023426
1802:
1691:Ann, H.B.; Lee, H-R. (2013-06-01).
1329:
1236:
1027:arms, and two secondary ones - the
970:galaxy morphological classification
608:{\displaystyle \mu =7{,}3^{\circ }}
286:galaxy morphological classification
281:lines produced by cold gas clouds.
13:
2631:Yu, S.-Y.; Ho, L.C. (2019-02-01).
2236:
2107:
1976:
1611:
1429:Swinburne University of Technology
233:: from left to right are bands u (
76:, a bluer colour, and an enhanced
14:
4878:
3975:
2840:
2428:Astronomy and Astrophysics Review
1481:
1446:
1410:
1391:
1355:
1346:
1320:
984:Spiral structure of the Milky Way
923:
4823:
4812:
4811:
3158:NASA/IPAC Extragalactic Database
3057:, p. 172—175, 199, 202—207)
2347:Internet Encyclopedia of Science
1954:NASA/IPAC Extragalactic Database
1197:
1179:
904:and, consequently, a diminished
779:
726:
673:
620:
567:
445:
430:
406:
391:
376:
336:
321:
306:
3811:
3796:
3733:
3721:
3664:
3652:
3595:
3538:
3471:
3459:
3447:
3380:
3315:
3250:
3180:
3144:
3099:
3087:
3060:
3048:
2991:
2934:
2766:
2701:
2689:
2624:
2557:
2492:
2480:
2415:
2364:
2334:
2322:
2310:
2175:
2044:
1941:
1929:
1917:
1866:
1796:
1739:
1684:
1672:
1643:
1599:
1587:
1575:
1460:"Спиральная структура галактик"
1336:Большая российская энциклопедия
1245:Sketch of the M51 by Lord Rosse
543:images (the obtained values of
4754:Galaxy formation and evolution
4749:Galaxy color–magnitude diagram
2188:Astrophysics and Space Science
1986:Savchenko, S.S. (2013-12-01).
1563:
1551:
1379:
1073:
978:galaxies with a pronounced bar
948:The parameters of spiral arms
836:The spiral arms of the galaxy
469:Pitch angle of the spiral arm
386:, a grand design spiral galaxy
210:, and a greater prevalence of
1:
1594:Binney & Merrifield (1998
1314:
401:, a multi-armed spiral galaxy
351:
4056:
3994:. N.Y.: Springer Reference.
3945:Spiral structure in galaxies
416:, a flocculent spiral galaxy
358:Grand design spiral galaxies
141:, which are situated within
51:Grand design spiral galaxies
7:
4636:Galaxies named after people
3520:10.1051/0004-6361/201936871
3429:10.1088/0004-637X/694/1/512
2998:Vallée, J.P. (2014-07-01).
2941:Vallée, J.P. (2016-02-09).
2916:10.1088/1674-4527/18/12/146
1533:10.1051/0004-6361/201936000
1358:"Спиральные ветви галактик"
10:
4883:
4769:Gravitational microlensing
4724:Galactic coordinate system
3923:Princeton University Press
3485:Astronomy and Astrophysics
3113:Astronomy and Astrophysics
2976:10.3847/0004-6256/151/3/55
2373:"Galactic magnetic fields"
1903:10.5303/JKAS.2013.46.3.141
1760:Cambridge University Press
1721:10.5303/JKAS.2013.46.3.141
1498:Astronomy and Astrophysics
1120:
1077:
1043:, are also distinguished.
184:{\displaystyle z\approx 1}
130:is a spiral galaxy with a
34:are a defining feature of
4807:
4706:
4621:
4514:
4473:
4383:
4318:
4209:
4064:
4010:10.1007/978-94-007-5609-0
3948:. San Rafael California:
3678:The Astrophysical Journal
3609:The Astrophysical Journal
3552:The Astrophysical Journal
3394:The Astrophysical Journal
3329:The Astrophysical Journal
3297:10.1038/s41550-018-0627-5
3187:Засов & Постнов (2011
3082:Засов & Постнов (2011
3069:, pp. 40–44, 94–104)
3030:10.1088/0004-6256/148/1/5
2638:The Astrophysical Journal
2571:The Astrophysical Journal
2462:10.1007/s00159-015-0084-4
2400:10.4249/scholarpedia.2411
2222:10.1007/s10509-006-1984-6
1861:Засов & Постнов (2011
1786:10.1017/S1743921319008160
1570:Засов & Постнов (2011
1405:Засов & Постнов (2011
964:in the centre, and their
535:tend to be wound tighter.
93:to the total luminosity.
66:interstellar gas and dust
4734:Galactic magnetic fields
4547:Brightest cluster galaxy
4443:Luminous infrared galaxy
3781:10.3390/galaxies10050100
3661:, pp. 36–40, 94–98)
3365:10.3847/1538-4357/aaa965
3202:Shu, F.H. (2016-09-01).
3005:The Astronomical Journal
2948:The Astronomical Journal
2674:10.3847/1538-4357/aaf895
2092:10.3390/galaxies10050100
1803:Shu, F.H. (2016-09-01).
896:Additionally, there are
279:polyaromatic hydrocarbon
251:electromagnetic spectrum
59:electromagnetic spectrum
4729:Galactic habitable zone
4714:Extragalactic astronomy
4303:Supermassive black hole
4217:Active galactic nucleus
3512:2020A&A...636A..44E
3224:2016ARA&A..54..667S
3130:1994A&A...287...55J
2848:Encyclopedia Britannica
2454:2015A&ARv..24....4B
2422:Beck, R. (2015-12-01).
2371:Beck, R. (2007-08-17).
2214:2006Ap&SS.301..189C
1825:2016ARA&A..54..667S
1525:2019A&A...631A..94D
1142:gravitational potential
1137:mechanical oscillations
954:supermassive black hole
119:General characteristics
87:supermassive black hole
4481:Low surface brightness
4232:Central massive object
2816:10.1093/mnras/stac3096
2160:10.1093/mnras/stab2904
1582:Karttunen et al. (2016
1386:Karttunen et al. (2016
1246:
1223:barred spiral galaxies
1132:
1089:
997:
882:
844:
821:
768:
715:
662:
609:
563:are given in brackets)
557:
506:
489:
483:
246:
225:Images of M 51 in the
185:
134:
25:
4759:Galaxy rotation curve
3942:Seigar, M.S. (2017).
3875:Fundamental Astronomy
3818:Сурдин, В.Г. (2017).
2751:10.1093/mnras/stx1646
2542:10.1093/mnras/stx1794
2295:10.1093/mnras/staa258
2029:10.1093/mnras/stt1627
1425:astronomy.swin.edu.au
1244:
1130:
1087:
1053:rotate differentially
991:
874:
867:Luminosity and colour
854:Numerical simulations
835:
822:
769:
716:
663:
610:
558:
507:
484:
468:
461:Shape and pitch angle
293:classification scheme
224:
186:
126:
19:
4794:Population III stars
4789:Intergalactic travel
4739:Galactic orientation
4606:Voids and supervoids
3853:General Astrophysics
1608:, pp. 129, 167)
1294:stellar associations
1216:Alternative theories
790:
737:
684:
631:
578:
556:{\displaystyle \mu }
547:
505:{\displaystyle \mu }
496:
482:{\displaystyle \mu }
473:
440:has filamentary arms
169:
4784:Intergalactic stars
4673:Large quasar groups
4668:Groups and clusters
4532:Groups and clusters
4391:Lyman-alpha emitter
4283:Interstellar medium
3984:"Galaxy Morphology"
3805:, pp. 126–129)
3772:2022Galax..10..100S
3695:1987ApJ...314....3E
3626:1978ApJ...223..129G
3569:1964ApJ...140..646L
3421:2009ApJ...694..512M
3356:2018ApJ...854..182B
3289:2019NatAs...3..178P
3189:, pp. 385–387)
3084:, pp. 385–386)
3022:2014AJ....148....5V
2908:2018RAA....18..146X
2807:2023MNRAS.518.1022S
2742:2017MNRAS.471.1070B
2698:, pp. 108–123)
2665:2019ApJ...871..194Y
2598:2006ApJ...645.1012S
2533:2017MNRAS.471.2187D
2391:2007SchpJ...2.2411B
2319:, pp. 224–225)
2286:2020MNRAS.493..390S
2151:2022MNRAS.509..685L
2083:2022Galax..10..100S
2020:2013MNRAS.436.1074S
1895:2013JKAS...46..141A
1863:, pp. 384–386)
1778:2020IAUS..353..140B
1713:2013JKAS...46..141A
1596:, pp. 153–154)
1584:, pp. 388–391)
1572:, pp. 382–384)
1388:, pp. 389–390)
1279:supernova explosion
1123:Density wave theory
1117:Density wave theory
1102:supernova explosion
1098:interstellar medium
1061:density wave theory
962:velocity dispersion
362:flocculent galaxies
193:age of the Universe
102:density wave theory
68:, bright stars and
55:flocculent galaxies
38:. They manifest as
4779:Intergalactic dust
4764:Gravitational lens
4719:Galactic astronomy
4688:Starburst galaxies
4428:blue compact dwarf
4384:Energetic galaxies
4348:BL Lacertae object
3914:Galactic Astronomy
3096:, pp. 94–104)
2843:"Milky Way Galaxy"
1949:"Spiral Structure"
1681:, pp. 11, 34)
1247:
1159:of galaxies or by
1133:
1100:. For instance, a
1090:
998:
883:
845:
817:
764:
711:
658:
605:
553:
517:logarithmic spiral
502:
490:
479:
288:. For example, in
247:
181:
135:
26:
4839:
4838:
4799:Galaxy X (galaxy)
4774:Illustris project
4744:Galactic quadrant
4465:Wolf-Rayet galaxy
4455:Green bean galaxy
4450:Hot dust-obscured
4401:Luminous infrared
4165:Elliptical galaxy
4019:978-94-007-5609-0
3959:978-1-6817-4609-8
3932:978-0-691-23332-1
3901:978-3-662-53045-0
3862:978-5-85099-188-3
3849:Общая астрофизика
3837:978-5-9221-1726-5
3730:, pp. 33–37)
3468:, pp. 78–84)
3456:, pp. 53–54)
1560:, pp. 31–32)
1205:
1187:
1153:corotation radius
1006:interstellar dust
994:embedded clusters
525:hyperbolic spiral
261:. In the red and
231:photometric bands
151:unbarred galaxies
4874:
4827:
4815:
4814:
4460:Hanny's Voorwerp
4370:Relativistic jet
4244:Dark matter halo
4051:
4044:
4037:
4028:
4027:
4023:
4003:
3971:
3936:
3905:
3866:
3841:
3806:
3800:
3794:
3793:
3783:
3765:
3737:
3731:
3725:
3719:
3718:
3713:. Archived from
3668:
3662:
3656:
3650:
3649:
3644:. Archived from
3599:
3593:
3592:
3587:. Archived from
3542:
3536:
3535:
3530:. Archived from
3505:
3475:
3469:
3463:
3457:
3451:
3445:
3444:
3439:. Archived from
3414:
3384:
3378:
3377:
3367:
3349:
3319:
3313:
3312:
3307:. Archived from
3282:
3271:Nature Portfolio
3263:Nature Astronomy
3254:
3248:
3247:
3242:. Archived from
3199:
3190:
3184:
3178:
3177:
3175:
3174:
3165:. Archived from
3148:
3142:
3141:
3103:
3097:
3091:
3085:
3079:
3070:
3064:
3058:
3052:
3046:
3045:
3040:. Archived from
2995:
2989:
2988:
2978:
2968:
2938:
2932:
2931:
2926:. Archived from
2901:
2873:
2864:
2863:
2861:
2860:
2851:. Archived from
2838:
2829:
2828:
2818:
2800:
2770:
2764:
2763:
2753:
2735:
2705:
2699:
2693:
2687:
2686:
2676:
2658:
2628:
2622:
2621:
2616:. Archived from
2591:
2589:astro-ph/0603622
2561:
2555:
2554:
2544:
2526:
2496:
2490:
2484:
2478:
2477:
2472:. Archived from
2447:
2419:
2413:
2412:
2402:
2368:
2362:
2361:
2359:
2358:
2349:. Archived from
2338:
2332:
2326:
2320:
2314:
2308:
2307:
2297:
2279:
2249:
2234:
2233:
2207:
2205:astro-ph/0509487
2179:
2173:
2172:
2162:
2144:
2114:
2105:
2104:
2094:
2076:
2048:
2042:
2041:
2031:
2013:
1983:
1974:
1973:
1971:
1970:
1961:. Archived from
1945:
1939:
1933:
1927:
1921:
1915:
1914:
1870:
1864:
1858:
1849:
1848:
1843:. Archived from
1800:
1794:
1793:
1788:. Archived from
1771:
1743:
1737:
1736:
1731:. Archived from
1688:
1682:
1676:
1670:
1669:
1667:
1666:
1657:. Archived from
1647:
1641:
1640:
1638:
1637:
1628:. Archived from
1618:
1609:
1603:
1597:
1591:
1585:
1579:
1573:
1567:
1561:
1555:
1549:
1548:
1543:. Archived from
1518:
1488:
1479:
1478:
1476:
1475:
1466:. Archived from
1455:
1444:
1443:
1441:
1440:
1431:. Archived from
1417:
1408:
1402:
1389:
1383:
1377:
1376:
1374:
1373:
1364:. Archived from
1353:
1344:
1343:
1327:
1253:(M51), in which
1251:Whirlpool Galaxy
1237:Research history
1207:
1206:
1189:
1188:
1021:Scutum-Centaurus
1014:molecular clouds
1010:neutral hydrogen
858:dark matter halo
826:
824:
823:
818:
816:
815:
806:
783:
773:
771:
770:
765:
763:
762:
753:
730:
720:
718:
717:
712:
710:
709:
700:
677:
667:
665:
664:
659:
657:
656:
647:
624:
614:
612:
611:
606:
604:
603:
594:
571:
562:
560:
559:
554:
511:
509:
508:
503:
488:
486:
485:
480:
455:has massive arms
449:
434:
410:
395:
380:
340:
325:
310:
277:, as well as in
275:emission nebulae
259:blue supergiants
208:active starburst
190:
188:
187:
182:
22:Whirlpool Galaxy
4882:
4881:
4877:
4876:
4875:
4873:
4872:
4871:
4852:Spiral galaxies
4842:
4841:
4840:
4835:
4803:
4702:
4617:
4510:
4469:
4379:
4314:
4293:Galaxy filament
4237:Galactic Center
4205:
4060:
4055:
4020:
3978:
3960:
3933:
3902:
3863:
3838:
3814:
3809:
3801:
3797:
3738:
3734:
3726:
3722:
3669:
3665:
3657:
3653:
3600:
3596:
3543:
3539:
3476:
3472:
3464:
3460:
3452:
3448:
3385:
3381:
3320:
3316:
3255:
3251:
3200:
3193:
3185:
3181:
3172:
3170:
3149:
3145:
3104:
3100:
3092:
3088:
3080:
3073:
3065:
3061:
3053:
3049:
2996:
2992:
2939:
2935:
2888:(12). Bristol:
2874:
2867:
2858:
2856:
2839:
2832:
2789:Wiley-Blackwell
2771:
2767:
2724:Wiley-Blackwell
2706:
2702:
2694:
2690:
2629:
2625:
2562:
2558:
2515:Wiley-Blackwell
2497:
2493:
2485:
2481:
2420:
2416:
2369:
2365:
2356:
2354:
2343:"Spiral galaxy"
2339:
2335:
2327:
2323:
2315:
2311:
2268:Wiley-Blackwell
2250:
2237:
2180:
2176:
2133:Wiley-Blackwell
2115:
2108:
2049:
2045:
2002:Wiley-Blackwell
1984:
1977:
1968:
1966:
1947:
1946:
1942:
1934:
1930:
1922:
1918:
1871:
1867:
1859:
1852:
1801:
1797:
1744:
1740:
1689:
1685:
1677:
1673:
1664:
1662:
1649:
1648:
1644:
1635:
1633:
1620:
1619:
1612:
1604:
1600:
1592:
1588:
1580:
1576:
1568:
1564:
1556:
1552:
1489:
1482:
1473:
1471:
1458:Марочник, Л.С.
1456:
1447:
1438:
1436:
1419:
1418:
1411:
1403:
1392:
1384:
1380:
1371:
1369:
1354:
1347:
1328:
1321:
1317:
1306:Bruce Elmegreen
1263:Bertil Lindblad
1239:
1218:
1211:
1208:
1198:
1193:
1190:
1180:
1125:
1119:
1082:
1076:
1049:
986:
966:rotation curves
946:
930:magnetic fields
926:
910:galaxy clusters
898:anemic galaxies
869:
828:
811:
807:
802:
791:
788:
787:
784:
775:
758:
754:
749:
738:
735:
734:
731:
722:
705:
701:
696:
685:
682:
681:
678:
669:
652:
648:
643:
632:
629:
628:
625:
616:
599:
595:
590:
579:
576:
575:
572:
548:
545:
544:
497:
494:
493:
474:
471:
470:
463:
456:
450:
441:
435:
417:
411:
402:
396:
387:
381:
354:
347:
341:
332:
326:
317:
311:
170:
167:
166:
155:barred galaxies
139:spiral galaxies
121:
36:spiral galaxies
29:
12:
11:
5:
4880:
4870:
4869:
4864:
4859:
4854:
4837:
4836:
4834:
4833:
4821:
4808:
4805:
4804:
4802:
4801:
4796:
4791:
4786:
4781:
4776:
4771:
4766:
4761:
4756:
4751:
4746:
4741:
4736:
4731:
4726:
4721:
4716:
4710:
4708:
4704:
4703:
4701:
4700:
4695:
4690:
4685:
4680:
4675:
4670:
4665:
4664:
4663:
4658:
4653:
4648:
4643:
4638:
4627:
4625:
4619:
4618:
4616:
4615:
4614:
4613:
4603:
4598:
4593:
4591:Stellar stream
4588:
4583:
4578:
4577:
4576:
4571:
4566:
4556:
4555:
4554:
4549:
4544:
4539:
4529:
4524:
4518:
4516:
4512:
4511:
4509:
4508:
4503:
4498:
4493:
4488:
4483:
4477:
4475:
4471:
4470:
4468:
4467:
4462:
4457:
4452:
4447:
4446:
4445:
4440:
4435:
4430:
4420:
4419:
4418:
4413:
4408:
4398:
4393:
4387:
4385:
4381:
4380:
4378:
4377:
4372:
4367:
4366:
4365:
4360:
4350:
4345:
4340:
4335:
4330:
4324:
4322:
4316:
4315:
4313:
4312:
4311:
4310:
4300:
4295:
4290:
4285:
4280:
4278:Galactic ridge
4275:
4273:Galactic plane
4270:
4269:
4268:
4258:
4257:
4256:
4246:
4241:
4240:
4239:
4229:
4224:
4219:
4213:
4211:
4207:
4206:
4204:
4203:
4202:
4201:
4191:
4186:
4185:
4184:
4174:
4173:
4172:
4162:
4161:
4160:
4155:
4150:
4145:
4135:
4134:
4133:
4128:
4123:
4118:
4113:
4108:
4103:
4093:
4092:
4091:
4086:
4076:
4070:
4068:
4062:
4061:
4054:
4053:
4046:
4039:
4031:
4025:
4024:
4018:
3977:
3976:External links
3974:
3973:
3972:
3958:
3950:IOP Publishing
3938:
3937:
3931:
3907:
3906:
3900:
3878:(6 ed.).
3868:
3867:
3861:
3843:
3842:
3836:
3813:
3810:
3808:
3807:
3795:
3732:
3720:
3717:on 2022-03-03.
3703:10.1086/165034
3687:IOP Publishing
3663:
3651:
3648:on 2023-01-24.
3634:10.1086/156243
3618:IOP Publishing
3594:
3591:on 2023-02-04.
3577:10.1086/147955
3561:IOP Publishing
3537:
3534:on 2023-01-24.
3470:
3458:
3446:
3443:on 2022-06-21.
3403:IOP Publishing
3401:(1). Bristol:
3379:
3338:IOP Publishing
3336:(2). Bristol:
3314:
3311:on 2023-01-17.
3249:
3246:on 2023-06-18.
3216:Annual Reviews
3191:
3179:
3143:
3098:
3086:
3071:
3059:
3047:
3044:on 2023-04-04.
3014:IOP Publishing
3012:(1). Bristol:
2990:
2957:IOP Publishing
2955:(3). Bristol:
2933:
2930:on 2022-01-24.
2890:IOP Publishing
2865:
2830:
2765:
2700:
2688:
2647:IOP Publishing
2645:(2). Bristol:
2623:
2620:on 2022-06-16.
2606:10.1086/504463
2580:IOP Publishing
2578:(2). Bristol:
2556:
2491:
2479:
2476:on 2022-10-13.
2414:
2363:
2333:
2321:
2309:
2235:
2174:
2106:
2043:
1975:
1940:
1928:
1916:
1865:
1850:
1847:on 2023-06-18.
1817:Annual Reviews
1795:
1792:on 2023-01-03.
1738:
1735:on 2023-01-03.
1683:
1671:
1642:
1610:
1598:
1586:
1574:
1562:
1550:
1547:on 2023-02-20.
1480:
1445:
1409:
1407:, p. 382)
1390:
1378:
1345:
1342:on 2023-01-01.
1330:Ефремов, Ю.Н.
1318:
1316:
1313:
1267:Chia-Chiao Lin
1238:
1235:
1217:
1214:
1213:
1212:
1209:
1196:
1194:
1191:
1178:
1176:
1171:amplification.
1121:Main article:
1118:
1115:
1078:Main article:
1075:
1072:
1048:
1045:
985:
982:
945:
942:
925:
924:Magnetic field
922:
906:star formation
868:
865:
830:
829:
814:
810:
805:
801:
798:
795:
785:
778:
776:
761:
757:
752:
748:
745:
742:
732:
725:
723:
708:
704:
699:
695:
692:
689:
679:
672:
670:
655:
651:
646:
642:
639:
636:
626:
619:
617:
602:
598:
593:
589:
586:
583:
573:
566:
564:
552:
501:
478:
462:
459:
458:
457:
451:
444:
442:
436:
429:
427:
419:
418:
412:
405:
403:
397:
390:
388:
382:
375:
373:
353:
350:
349:
348:
342:
335:
333:
327:
320:
318:
312:
305:
303:
271:spectral lines
180:
177:
174:
132:pronounced bar
120:
117:
78:magnetic field
27:
9:
6:
4:
3:
2:
4879:
4868:
4867:Galactic arms
4865:
4863:
4860:
4858:
4855:
4853:
4850:
4849:
4847:
4832:
4831:
4826:
4822:
4820:
4819:
4810:
4809:
4806:
4800:
4797:
4795:
4792:
4790:
4787:
4785:
4782:
4780:
4777:
4775:
4772:
4770:
4767:
4765:
4762:
4760:
4757:
4755:
4752:
4750:
4747:
4745:
4742:
4740:
4737:
4735:
4732:
4730:
4727:
4725:
4722:
4720:
4717:
4715:
4712:
4711:
4709:
4705:
4699:
4696:
4694:
4693:Superclusters
4691:
4689:
4686:
4684:
4681:
4679:
4676:
4674:
4671:
4669:
4666:
4662:
4659:
4657:
4654:
4652:
4649:
4647:
4644:
4642:
4639:
4637:
4634:
4633:
4632:
4629:
4628:
4626:
4624:
4620:
4612:
4609:
4608:
4607:
4604:
4602:
4599:
4597:
4596:Superclusters
4594:
4592:
4589:
4587:
4584:
4582:
4579:
4575:
4572:
4570:
4567:
4565:
4562:
4561:
4560:
4557:
4553:
4550:
4548:
4545:
4543:
4540:
4538:
4535:
4534:
4533:
4530:
4528:
4527:Galactic tide
4525:
4523:
4520:
4519:
4517:
4513:
4507:
4504:
4502:
4499:
4497:
4494:
4492:
4489:
4487:
4486:Ultra diffuse
4484:
4482:
4479:
4478:
4476:
4472:
4466:
4463:
4461:
4458:
4456:
4453:
4451:
4448:
4444:
4441:
4439:
4436:
4434:
4431:
4429:
4426:
4425:
4424:
4421:
4417:
4414:
4412:
4409:
4407:
4404:
4403:
4402:
4399:
4397:
4394:
4392:
4389:
4388:
4386:
4382:
4376:
4373:
4371:
4368:
4364:
4361:
4359:
4356:
4355:
4354:
4351:
4349:
4346:
4344:
4341:
4339:
4336:
4334:
4331:
4329:
4326:
4325:
4323:
4321:
4320:Active nuclei
4317:
4309:
4306:
4305:
4304:
4301:
4299:
4296:
4294:
4291:
4289:
4286:
4284:
4281:
4279:
4276:
4274:
4271:
4267:
4264:
4263:
4262:
4259:
4255:
4252:
4251:
4250:
4247:
4245:
4242:
4238:
4235:
4234:
4233:
4230:
4228:
4225:
4223:
4220:
4218:
4215:
4214:
4212:
4208:
4200:
4197:
4196:
4195:
4192:
4190:
4187:
4183:
4180:
4179:
4178:
4175:
4171:
4168:
4167:
4166:
4163:
4159:
4156:
4154:
4151:
4149:
4146:
4144:
4141:
4140:
4139:
4136:
4132:
4129:
4127:
4124:
4122:
4119:
4117:
4114:
4112:
4109:
4107:
4104:
4102:
4099:
4098:
4097:
4094:
4090:
4087:
4085:
4082:
4081:
4080:
4077:
4075:
4072:
4071:
4069:
4067:
4063:
4059:
4052:
4047:
4045:
4040:
4038:
4033:
4032:
4029:
4021:
4015:
4011:
4007:
4002:
3997:
3993:
3989:
3985:
3980:
3979:
3969:
3965:
3961:
3955:
3951:
3947:
3946:
3940:
3939:
3934:
3928:
3924:
3920:
3916:
3915:
3909:
3908:
3903:
3897:
3893:
3889:
3885:
3881:
3877:
3876:
3870:
3869:
3864:
3858:
3854:
3850:
3845:
3844:
3839:
3833:
3830:: Физматлит.
3829:
3825:
3821:
3816:
3815:
3804:
3799:
3791:
3787:
3782:
3777:
3773:
3769:
3764:
3759:
3755:
3751:
3747:
3743:
3736:
3729:
3724:
3716:
3712:
3708:
3704:
3700:
3696:
3692:
3688:
3684:
3680:
3679:
3674:
3667:
3660:
3655:
3647:
3643:
3639:
3635:
3631:
3627:
3623:
3619:
3615:
3611:
3610:
3605:
3598:
3590:
3586:
3582:
3578:
3574:
3570:
3566:
3562:
3558:
3554:
3553:
3548:
3541:
3533:
3529:
3525:
3521:
3517:
3513:
3509:
3504:
3499:
3495:
3491:
3487:
3486:
3481:
3474:
3467:
3462:
3455:
3450:
3442:
3438:
3434:
3430:
3426:
3422:
3418:
3413:
3408:
3404:
3400:
3396:
3395:
3390:
3383:
3375:
3371:
3366:
3361:
3357:
3353:
3348:
3343:
3339:
3335:
3331:
3330:
3325:
3318:
3310:
3306:
3302:
3298:
3294:
3290:
3286:
3281:
3276:
3272:
3268:
3264:
3260:
3253:
3245:
3241:
3237:
3233:
3229:
3225:
3221:
3217:
3214:. Pato Alto:
3213:
3209:
3205:
3198:
3196:
3188:
3183:
3169:on 2023-01-17
3168:
3164:
3160:
3159:
3154:
3147:
3139:
3135:
3131:
3127:
3123:
3119:
3115:
3114:
3109:
3102:
3095:
3090:
3083:
3078:
3076:
3068:
3063:
3056:
3051:
3043:
3039:
3035:
3031:
3027:
3023:
3019:
3015:
3011:
3007:
3006:
3001:
2994:
2986:
2982:
2977:
2972:
2967:
2962:
2958:
2954:
2950:
2949:
2944:
2937:
2929:
2925:
2921:
2917:
2913:
2909:
2905:
2900:
2895:
2891:
2887:
2883:
2879:
2872:
2870:
2855:on 2022-01-19
2854:
2850:
2849:
2844:
2837:
2835:
2826:
2822:
2817:
2812:
2808:
2804:
2799:
2794:
2791:: 1022–1040.
2790:
2786:
2782:
2781:
2776:
2769:
2761:
2757:
2752:
2747:
2743:
2739:
2734:
2729:
2726:: 1070–1087.
2725:
2721:
2717:
2716:
2711:
2704:
2697:
2692:
2684:
2680:
2675:
2670:
2666:
2662:
2657:
2652:
2648:
2644:
2640:
2639:
2634:
2627:
2619:
2615:
2611:
2607:
2603:
2599:
2595:
2590:
2585:
2582:: 1012–1023.
2581:
2577:
2573:
2572:
2567:
2560:
2552:
2548:
2543:
2538:
2534:
2530:
2525:
2520:
2517:: 2187–2203.
2516:
2512:
2508:
2507:
2502:
2495:
2489:, p. 81)
2488:
2483:
2475:
2471:
2467:
2463:
2459:
2455:
2451:
2446:
2441:
2437:
2433:
2429:
2425:
2418:
2410:
2406:
2401:
2396:
2392:
2388:
2384:
2380:
2379:
2374:
2367:
2353:on 2022-06-16
2352:
2348:
2344:
2337:
2331:, p. 36)
2330:
2325:
2318:
2313:
2305:
2301:
2296:
2291:
2287:
2283:
2278:
2273:
2269:
2265:
2261:
2260:
2255:
2248:
2246:
2244:
2242:
2240:
2231:
2227:
2223:
2219:
2215:
2211:
2206:
2201:
2197:
2194:(1–4). N.Y.:
2193:
2189:
2185:
2178:
2170:
2166:
2161:
2156:
2152:
2148:
2143:
2138:
2134:
2130:
2126:
2125:
2120:
2113:
2111:
2102:
2098:
2093:
2088:
2084:
2080:
2075:
2070:
2066:
2062:
2058:
2054:
2047:
2039:
2035:
2030:
2025:
2021:
2017:
2012:
2007:
2004:: 1074–1083.
2003:
1999:
1995:
1994:
1989:
1982:
1980:
1965:on 2022-10-12
1964:
1960:
1956:
1955:
1950:
1944:
1938:, p. 34)
1937:
1932:
1926:, p. 34)
1925:
1920:
1912:
1908:
1904:
1900:
1896:
1892:
1888:
1884:
1880:
1876:
1869:
1862:
1857:
1855:
1846:
1842:
1838:
1834:
1830:
1826:
1822:
1818:
1815:. San Mateo:
1814:
1810:
1806:
1799:
1791:
1787:
1783:
1779:
1775:
1770:
1765:
1761:
1757:
1753:
1749:
1742:
1734:
1730:
1726:
1722:
1718:
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41:
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4552:fossil group
4474:Low activity
4308:Ultramassive
4138:Dwarf galaxy
4121:intermediate
4116:grand design
3991:
3987:
3944:
3913:
3874:
3852:
3848:
3823:
3819:
3812:Bibliography
3803:Seigar (2017
3798:
3752:(5). Basel:
3749:
3745:
3735:
3723:
3715:the original
3682:
3676:
3666:
3659:Seigar (2017
3654:
3646:the original
3613:
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3589:the original
3556:
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3532:the original
3494:EDP Sciences
3492:. Les Ulis:
3489:
3483:
3473:
3466:Seigar (2017
3461:
3454:Seigar (2017
3449:
3441:the original
3398:
3392:
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3333:
3327:
3317:
3309:the original
3266:
3262:
3252:
3244:the original
3211:
3207:
3182:
3171:. Retrieved
3167:the original
3156:
3146:
3122:EDP Sciences
3120:. Les Ulis:
3117:
3111:
3101:
3094:Seigar (2017
3089:
3067:Seigar (2017
3062:
3055:Сурдин (2017
3050:
3042:the original
3009:
3003:
2993:
2952:
2946:
2936:
2928:the original
2885:
2881:
2857:. Retrieved
2853:the original
2846:
2841:Hodge, P.W.
2784:
2778:
2768:
2719:
2713:
2703:
2696:Seigar (2017
2691:
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2487:Seigar (2017
2482:
2474:the original
2431:
2427:
2417:
2382:
2378:Scholarpedia
2376:
2366:
2355:. Retrieved
2351:the original
2346:
2341:Darling, D.
2336:
2324:
2317:Сурдин (2017
2312:
2263:
2257:
2191:
2187:
2177:
2128:
2122:
2063:(5). Basel:
2060:
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1967:. Retrieved
1963:the original
1952:
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1659:the original
1654:
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1634:. Retrieved
1630:the original
1625:
1601:
1589:
1577:
1565:
1558:Seigar (2017
1553:
1545:the original
1507:EDP Sciences
1505:. Les Ulis:
1502:
1496:
1472:. Retrieved
1468:the original
1463:
1437:. Retrieved
1433:the original
1424:
1421:"Spiral Arm"
1381:
1370:. Retrieved
1366:the original
1361:
1356:Засов, А.В.
1340:the original
1335:
1332:"ГАЛА́КТИКА"
1310:
1298:
1291:
1281:stimulating
1259:
1248:
1219:
1169:
1150:
1134:
1104:generates a
1091:
1065:
1050:
1018:
999:
975:
947:
927:
914:ram pressure
895:
891:colour index
888:
884:
862:
846:
840:
514:
491:
420:
366:
355:
283:
273:produced by
248:
216:H II regions
197:
160:
136:
106:
95:
63:
48:
31:
30:
4611:void galaxy
4574:cannibalism
4559:Interacting
4515:Interaction
4501:Blue Nugget
4491:Dark galaxy
4396:Lyman-break
4288:Protogalaxy
4254:Disc galaxy
3685:. Bristol:
3620:: 129–139.
3616:. Bristol:
3559:. Bristol:
3405:: 512–545.
3273:: 178–182.
3269:(2). N.Y.:
3218:: 667–724.
2787:(1). Oxf.:
2722:(1). Oxf.:
2513:(2). Oxf.:
2385:(8): 2411.
2270:: 390–409.
2266:(1). Oxf.:
2198:: 189–193.
2135:: 685–692.
2131:(1). Oxf.:
2000:(2). Oxf.:
1819:: 686–687.
1762:: 140–143.
1231:phase space
1161:tidal force
1080:SSPSF model
1074:SSPSF model
1067:Tidal tails
1033:Sagittarius
521:Archimedean
255:ultraviolet
235:ultraviolet
149:, which in
32:Spiral arms
4846:Categories
4651:Polar-ring
4496:Red nugget
4438:faint blue
4298:Spiral arm
4153:spheroidal
4143:elliptical
4126:Magellanic
4111:flocculent
4079:Lenticular
4066:Morphology
3884:Heidelberg
3763:1511.06365
3728:Buta (2011
3503:1910.06653
3347:1801.07476
3280:1809.08048
3173:2023-01-17
2966:1602.02183
2899:1810.08819
2859:2022-01-19
2798:2205.08733
2733:1706.09904
2656:1812.06010
2524:1707.04001
2445:1509.04522
2357:2022-06-07
2329:Buta (2011
2277:2001.09110
2142:2110.02149
2074:1511.06365
1969:2023-01-01
1936:Buta (2011
1924:Buta (2011
1769:1910.01139
1679:Buta (2011
1665:2023-01-03
1636:2023-01-01
1606:Buta (2011
1516:1908.04246
1474:2023-01-24
1439:2022-12-03
1372:2022-12-03
1315:References
1287:Ernst Opik
1255:Lord Rosse
1165:satellites
1146:dust lanes
1002:our galaxy
938:microgauss
934:microgauss
920:galaxies.
918:lenticular
786:NGC 2532 (
733:NGC 2575 (
680:NGC 4195 (
627:NGC 2649 (
574:NGC 4977 (
352:Morphology
267:radio band
113:galaxy M51
109:Lord Rosse
82:luminosity
4857:Astronomy
4586:Satellite
4581:Jellyfish
4569:collision
4506:Dead disk
4423:Starburst
4338:Markarian
4210:Structure
4177:Irregular
4148:irregular
4001:1102.0550
3968:994877317
3919:Princeton
3820:Галактики
3790:2075-4434
3711:0004-637X
3642:0004-637X
3585:0004-637X
3528:0004-6361
3437:0004-637X
3412:0812.3647
3374:1538-4357
3305:2397-3366
3240:0066-4146
3138:0004-6361
3124:: 55–67.
3038:0004-6256
2985:1538-3881
2924:1674-4527
2825:0035-8711
2760:0035-8711
2683:0004-637X
2614:0004-637X
2551:0035-8711
2470:0935-4956
2409:1941-6016
2304:0035-8711
2230:0004-640X
2169:0035-8711
2101:2075-4434
2038:0035-8711
2011:1309.4308
1911:1225-4614
1841:0066-4146
1729:1225-4614
1541:0004-6361
1283:starburst
1271:Frank Shu
1163:of their
1106:shockwave
1094:starburst
1041:Orion arm
950:correlate
928:Stronger
813:∘
794:μ
760:∘
741:μ
707:∘
688:μ
654:∘
635:μ
601:∘
582:μ
551:μ
529:correlate
500:μ
477:μ
241:) and z (
229:in three
176:≈
163:redshifts
74:starburst
72:, active
4818:Category
4707:See also
4631:Galaxies
4358:X-shaped
4189:Peculiar
4131:unbarred
4089:unbarred
4058:Galaxies
3892:Springer
3824:Galaxies
3746:Galaxies
2436:Springer
2434:. N.Y.:
2196:Springer
2057:Galaxies
1758:. N.Y.:
1655:Астронет
1626:Астронет
1464:Астронет
1362:Астронет
1227:manifold
1111:infrared
1059:and the
876:NGC 4921
850:NGC 4622
838:NGC 4622
422:defined.
414:NGC 2841
344:NGC 3367
314:NGC 4314
290:Hubble's
243:infrared
128:NGC 1300
100:and the
4862:Spirals
4678:Quasars
4646:Nearest
4641:Largest
4542:cluster
4375:Seyfert
3768:Bibcode
3756:: 100.
3691:Bibcode
3622:Bibcode
3565:Bibcode
3563:: 646.
3508:Bibcode
3496:: A44.
3417:Bibcode
3352:Bibcode
3340:: 182.
3285:Bibcode
3220:Bibcode
3163:Caltech
3126:Bibcode
3018:Bibcode
2904:Bibcode
2892:: 146.
2803:Bibcode
2738:Bibcode
2661:Bibcode
2649:: 194.
2594:Bibcode
2529:Bibcode
2450:Bibcode
2387:Bibcode
2282:Bibcode
2210:Bibcode
2147:Bibcode
2079:Bibcode
2067:: 100.
2016:Bibcode
1959:Caltech
1891:Bibcode
1821:Bibcode
1774:Bibcode
1709:Bibcode
1521:Bibcode
1509:: A94.
1037:parsecs
1025:Perseus
239:visible
147:spirals
111:in the
4830:Portal
4661:Spiral
4564:merger
4343:Quasar
4328:Blazar
4266:corona
4182:barred
4158:spiral
4106:barred
4101:anemic
4096:Spiral
4084:barred
4016:
3966:
3956:
3929:
3898:
3880:Berlin
3859:
3834:
3828:Moscow
3788:
3709:
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3526:
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2036:
1909:
1839:
1727:
1539:
1275:theory
841:pitch?
533:bulges
237:), r (
165:up to
40:spiral
4698:Voids
4623:Lists
4601:Walls
4537:group
4522:Field
4416:ELIRG
4411:HLIRG
4406:ULIRG
4363:DRAGN
4353:Radio
4333:LINER
4227:Bulge
4199:Polar
3996:arXiv
3851:[
3822:[
3758:arXiv
3689:: 3.
3498:arXiv
3407:arXiv
3342:arXiv
3275:arXiv
3016:: 5.
2961:arXiv
2894:arXiv
2793:arXiv
2728:arXiv
2651:arXiv
2584:arXiv
2519:arXiv
2440:arXiv
2438:: 4.
2272:arXiv
2200:arXiv
2137:arXiv
2069:arXiv
2006:arXiv
1887:Seoul
1885:(3).
1764:arXiv
1705:Seoul
1703:(3).
1511:arXiv
1302:Debra
1029:Norma
958:bulge
878:- an
346:(SBc)
331:(SBb)
316:(SBa)
143:discs
91:bulge
4656:Ring
4261:Halo
4249:Disc
4194:Ring
4074:Disc
4014:ISBN
3964:OCLC
3954:ISBN
3927:ISBN
3896:ISBN
3888:N.Y.
3857:ISBN
3832:ISBN
3786:ISSN
3754:MDPI
3707:ISSN
3638:ISSN
3581:ISSN
3524:ISSN
3433:ISSN
3370:ISSN
3301:ISSN
3236:ISSN
3134:ISSN
3034:ISSN
2981:ISSN
2920:ISSN
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2679:ISSN
2610:ISSN
2547:ISSN
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2405:ISSN
2300:ISSN
2226:ISSN
2165:ISSN
2097:ISSN
2065:MDPI
2034:ISSN
1907:ISSN
1837:ISSN
1725:ISSN
1537:ISSN
1304:and
1269:and
1157:bars
1031:and
1023:and
541:SDSS
438:M101
399:M101
301:SDSS
227:SDSS
204:dust
202:and
20:The
4433:pea
4222:Bar
4006:doi
3776:doi
3699:doi
3683:314
3630:doi
3614:223
3573:doi
3557:140
3516:doi
3490:636
3425:doi
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3334:854
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3228:doi
3118:287
3026:doi
3010:148
2971:doi
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2811:doi
2785:518
2746:doi
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2643:871
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2192:301
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1998:436
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179:1
173:z
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