1891:
803:
1574: = 50, 82, and 126 are reached, and neutron capture is temporarily paused. These so-called waiting points are characterized by increased binding energy relative to heavier isotopes, leading to low neutron capture cross sections and a buildup of semi-magic nuclei that are more stable toward beta decay. In addition, nuclei beyond the shell closures are susceptible to quicker beta decay owing to their proximity to the drip line; for these nuclei, beta decay occurs before further neutron capture. Waiting point nuclei are then allowed to beta decay toward stability before further neutron capture can occur, resulting in a slowdown or
3831:
1435:
4430:
816:
1114:
31:
4440:
1877:
1780:). When released from the huge internal pressure of the neutron star, these ejecta expand and form seed heavy nuclei that rapidly capture free neutrons, and radiate detected optical light for about a week. Such duration of luminosity would not be possible without heating by internal radioactive decay, which is provided by
1202:, who hypothesized that conditions in the core of collapsing stars would enable nucleosynthesis of the remainder of the elements via rapid capture of densely packed free neutrons. However, there remained unanswered questions about equilibrium in stars that was required to balance beta-decays and precisely account for
1229:
containing magic numbers of neutrons which were also in abundance, suggesting that radioactive neutron-rich nuclei having the magic neutron numbers but roughly ten fewer protons were formed. These observations also implied that rapid neutron capture occurred faster than
987:. Early studies theorized that 10 free neutrons per cm would be required, for temperatures of about 1 GK, in order to match the waiting points, at which no more neutrons can be captured, with the mass numbers of the abundance peaks for
1362:
building on preexisting iron. Primary stellar nucleosynthesis begins earlier in the galaxy than does secondary nucleosynthesis. Alternatively the high density of neutrons within neutron stars would be available for rapid assembly into
991:-process nuclei. This amounts to almost a gram of free neutrons in every cubic centimeter, an astonishing number requiring extreme locations. Traditionally this suggested the material ejected from the reexpanded core of a
1715:-process material. The ejected material must be relatively neutron-rich, a condition which has been difficult to achieve in models, so that astrophysicists remain uneasy about their adequacy for successful
2038:
1806:-process. Because of these spectroscopic features it has been argued that such nucleosynthesis in the Milky Way has been primarily ejecta from neutron-star mergers rather than from supernovae.
1427:-process thereby derives from observed abundance spectra in old stars that had been born early, when the galactic metallicity was still small, but that nonetheless contain their complement of
1367:-process nuclei if a collision were to eject portions of a neutron star, which then rapidly expands freed from confinement. That sequence could also begin earlier in galactic time than would
1423:-process emerges from quickly evolving massive stars that become supernovae and leave neutron-star remnants that can merge with another neutron star. The primary nature of the early
1350:
The creation of free neutrons by electron capture during the rapid collapse to high density of a supernova core along with quick assembly of some neutron-rich seed nuclei makes the
1589:
may be low enough before 270 such that neutron capture might induce fission instead of continuing up the neutron drip line. After the neutron flux decreases, these highly unstable
1480:-process is responsible for our natural cohort of radioactive elements, such as uranium and thorium, as well as the most neutron-rich isotopes of each heavy element.
1383:
in 1981. He and subsequent astronomers showed that the pattern of heavy-element abundances in the earliest metal-poor stars matched that of the shape of the solar
1084:, meaning that it requires pre-existing heavy isotopes as seed nuclei to be converted into other heavy nuclei by a slow sequence of captures of free neutrons. The
1379:-process enrichment of interstellar gas and of subsequent newly formed stars, as applied to the abundance evolution of the galaxy of stars, was first laid out by
4165:
2391:
1343:-process abundance curve (vs. atomic weight) has provided for many decades the target for theoretical computations of abundances synthesized by the physical
1738:-process material thrown off by the merging neutron stars. The bulk of this material seems to consist of two types: hot blue masses of highly radioactive
2876:
shows this path of captures reaching magic neutron numbers 82 and 126 at smaller values of nuclear charge Z than it does along the stability path.
1060:-process have half-lives long enough to enable their study in laboratory experiments, but this is not typically true for isotopes involved in the
1453:-process abundances because the overall problem is numerically formidable. However, existing results are supportive; in 2017, new data about the
1213:, which was known to almost certainly have a role in element formation, was also seen in a table of abundances of isotopes of heavy elements by
1088:-process scenarios create their own seed nuclei, so they might proceed in massive stars that contain no heavy seed nuclei. Taken together, the
1375:-process abundances in the galaxy. Each of these scenarios is the subject of active theoretical research. Observational evidence of the early
1441:
showing the cosmogenic origin of each element. The elements heavier than iron with origins in supernovae are typically those produced by the
4380:
1655:
nuclides at the line of beta stability before absorbing more neutrons in the next explosion, thus providing a chance to reach neutron-rich
3482:
1734:
to identify the location of the merger, several teams observed and studied optical data of the merger, finding spectroscopic evidence of
1631:-process also occurs in thermonuclear weapons, and was responsible for the initial discovery of neutron-rich almost stable isotopes of
1523:
of matter. This results in an extremely high density of free neutrons which cannot decay, on the order of 10 neutrons per cm, and high
1647:(atomic numbers 99 and 100) in the 1950s. It has been suggested that multiple nuclear explosions would make it possible to reach the
847:
761:
1825:-process fragments. Otherwise they would dim quickly. Such alternative sites were first seriously proposed in 1974 as decompressing
1703:
in the interstellar gas limits the amount each can have ejected. It requires either that only a small fraction of supernovae eject
1651:, as the affected nuclides (starting with uranium-238 as seed nuclei) would not have time to beta decay all the way to the quickly
1246:-process was named for its characteristic slow neutron capture. A table apportioning the heavy isotopes phenomenologically between
3159:
Watson, Darach; Hansen, Camilla J.; Selsing, Jonatan; Koch, Andreas; Malesani, Daniele B.; Andersen, Anja C.; Fynbo, Johan P. U.;
4360:
1449:
Either interpretation, though generally supported by supernova experts, has yet to achieve a totally satisfactory calculation of
1585:-process when its heaviest nuclei become unstable to spontaneous fission, when the total number of nucleons approaches 270. The
3968:
3438:
3163:; Bauswein, Andreas; Covino, Stefano; Grado, Aniello (2019). "Identification of strontium in the merger of two neutron stars".
1315:-process reinforced those temporal features. Seeger et al. were also able to construct more quantitative apportionment between
2933:
975:
arrives to be captured. This sequence can continue up to the limit of stability of the increasingly neutron-rich nuclei (the
3757:
4390:
909:-process can typically synthesize the heaviest four isotopes of every heavy element; of these, the heavier two are called
4375:
1358:, a process that can occur even in a star initially of pure H and He. This in contrast to the BFH designation which is a
110:
2601:
2853:
1203:
4464:
1153:
1072:, where the neutron flux is sufficient to cause neutron captures to recur every 10–100 years, much too slow for the
4160:
2735:
Wang, R.; Chen, L.W. (2015). "Positioning the neutron drip line and the r-process paths in the nuclear landscape".
2439:
1849:. Current astrophysical models suggest that a single neutron star merger event may have generated between 3 and 13
1845:
of two neutron stars that collide). After preliminary identification of these sites, the scenario was confirmed in
1100:
heavier than iron. The historical challenge has been to locate physical settings appropriate to their time scales.
414:
1890:
802:
4196:
3475:
1546:
Three processes which affect the climbing of the neutron drip line are a notable decrease in the neutron-capture
1399:-process abundances were born from that gas, for it requires about 100 million years of galactic history for the
606:
1323:-process of the abundance table of heavy isotopes, thereby establishing a more reliable abundance curve for the
4405:
4137:
3820:
1135:
1097:
311:
1593:
nuclei undergo a rapid succession of beta decays until they reach more stable, neutron-rich nuclei. While the
3330:
3238:
1297:-process abundance distribution. Shorter-time distributions emphasize abundances at atomic weights less than
1052:, the other predominant mechanism for the production of heavy elements, which is nucleosynthesis by means of
840:
4395:
4370:
4181:
3880:
1809:
These results offer a new possibility for clarifying six decades of uncertainty over the site of origin of
2859:, provides a clear technical introduction to these features. A more technical description can be found in
4443:
4400:
3908:
2200:-process heavy-element production solely or at least significantly takes place in the merger environment.
624:
594:
95:
4201:
4191:
3810:
3468:
2663:
2510:
2508:
Truran, J. W. (1981). "A new interpretation of the heavy-element abundances in metal-deficient stars".
2196:-process, and astrophysicists need to estimate the frequency of neutron-star mergers to assess whether
1511:
is blocked. This is because the high electron density fills all available free electron states up to a
1179:
1131:
671:
221:
1221:
in 1956. Their abundance table revealed larger than average abundances of natural isotopes containing
1182:
and Louis R. Henrich who postulated that elements were produced at temperatures between 6×10 and 8×10
3865:
3790:
2929:"Future of superheavy element research: Which nuclei could be synthesized within the next few years?"
2300:
2213:
2029:
1989:
996:
557:
1238:
at magic numbers. This process, rapid neutron capture by neutron-rich isotopes, became known as the
4479:
4474:
4385:
3750:
833:
820:
552:
256:
1604:-process, in neutron-rich predecessor nuclei, creates an abundance of radioactive nuclei about 10
4410:
3815:
3805:
3634:
3599:
3579:
3534:
2545:
2339:
1335:-process isotopic abundances from the total isotopic abundances and attributing the remainder to
1293:-process abundances, but, that when superposed, did achieve a successful characterization of the
1277:-process as described by the BFH paper was first demonstrated in a time-dependent calculation at
1124:
1069:
992:
547:
444:
409:
105:
4415:
4319:
4155:
4028:
4008:
3629:
3619:
1621:
1563:
1263:
1222:
1035:
601:
251:
216:
4365:
2982:"Optical emission from a kilonova following a gravitational-wave-detected neutron-star merger"
2845:
2485:-process abundances whereas Figure 18 shows the calculated abundances for long neutron fluxes.
1520:
905:-process usually synthesizes the most neutron-rich stable isotopes of each heavy element. The
4259:
4206:
3860:
2086:"Origin of the heavy elements in binary neutron-star mergers from a gravitational-wave event"
1547:
726:
611:
503:
2886:
Surman, R.; Mumpower, M.; Sinclair, R.; Jones, K. L.; Hix, W. R.; McLaughlin, G. C. (2014).
2718:
Nucleosynthesis in explosive environments: neutron star mergers and core-collapse supernovae
2524:
1174:
in stars, an unknown process responsible for producing heavier elements found on Earth from
666:
4018:
3855:
3624:
3614:
3402:
3339:
3292:
3247:
3182:
3123:
3062:
3005:
2952:
2899:
2807:
2754:
2678:
2622:
2564:
2539:
Abbott, B. P.; et al. (LIGO Scientific
Collaboration and Virgo Collaboration) (2017).
2519:
2448:
2400:
2351:
2309:
2270:
2228:
2173:
2109:
2047:
1998:
1462:
1023:
861:
736:
711:
528:
3830:
1331:-process abundances are determined using their technique of subtracting the more reliable
8:
4484:
4433:
4050:
4040:
4023:
3958:
3887:
3743:
3678:
3569:
3549:
3544:
2965:
2928:
2335:
1912:
1708:
1652:
1648:
1555:
1551:
1501:
1395:-process had not yet begun to enrich interstellar gas when these young stars missing the
1004:
631:
510:
404:
347:
340:
330:
271:
266:
100:
3406:
3344:
3296:
3252:
3186:
3127:
3066:
3009:
2956:
2903:
2811:
2758:
2716:
2682:
2626:
2568:
2453:
2405:
2355:
2313:
2274:
2232:
2177:
2113:
2051:
2002:
967:. The captures must be rapid in the sense that the nuclei must not have time to undergo
4186:
4095:
4071:
3963:
3923:
3785:
3392:
3214:
3172:
3113:
3052:
2995:
2942:
2770:
2744:
2694:
2554:
2367:
2163:
2099:
2063:
1656:
1558:, and the degree of nuclear stability in the heavy-isotope region. Neutron captures in
1011:. The relative contribution of each of these sources to the astrophysical abundance of
574:
569:
384:
1492:-process nucleosynthesis where the required conditions are thought to exist: low-mass
4222:
4066:
3996:
3933:
3845:
3795:
3780:
3559:
3529:
3499:
3420:
3359:
3218:
3206:
3198:
3141:
3080:
2849:
2838:
2833:
2819:
2798:
2698:
2690:
2613:
2582:
2371:
2127:
2067:
1590:
1567:
1540:
1497:
1286:
1282:
976:
968:
746:
741:
701:
579:
318:
306:
289:
261:
231:
72:
2774:
1304:, whereas longer-time distributions emphasized those at atomic weights greater than
4469:
4105:
3913:
3903:
3589:
3554:
3539:
3491:
3410:
3383:
3349:
3300:
3283:
3257:
3190:
3160:
3131:
3104:
3070:
3043:
3013:
2986:
2960:
2907:
2815:
2762:
2686:
2630:
2577:
2572:
2540:
2458:
2410:
2359:
2317:
2278:
2236:
2211:
2181:
2117:
2090:
2055:
2006:
1882:
1802:-process yields have been known since the first time dependent calculations of the
1613:
1605:
1516:
1465:
gravitational-wave observatories discovered a merger of two neutron stars ejecting
1195:
876:
766:
756:
686:
439:
357:
325:
145:
77:
2541:"GW170817: Observation of Gravitational Waves from a Binary Neutron Star Inspiral"
1391:-process component were missing. This was consistent with the hypothesis that the
979:) to physically retain neutrons as governed by the short range nuclear force. The
4013:
3918:
3699:
3594:
3564:
1586:
1528:
1434:
1380:
1210:
956:
880:
751:
731:
706:
636:
523:
451:
397:
362:
22:
983:-process therefore must occur in locations where there exists a high density of
4045:
4001:
3975:
3720:
3704:
3279:"Nucleosynthesis, neutrino bursts and gamma-rays from coalescing neutron stars"
2766:
2634:
2059:
1923:
1896:
1700:
1438:
884:
807:
661:
656:
535:
468:
276:
211:
188:
175:
162:
62:
40:
3194:
3100:"A kilonova as the electromagnetic counterpart to a gravitational-wave source"
2283:
2258:
2011:
1984:
1507:
Immediately after the severe compression of electrons in a Type II supernova,
1178:
and helium was suspected to exist. One early attempt at explanation came from
4458:
4249:
3609:
3524:
3379:"A 'kilonova' associated with the short-duration gamma-ray burst GRB 130603B"
3202:
2638:
2481:. Figure 16 shows the short-flux calculation and its comparison with natural
2321:
2154:
1837:
in compact binaries. In 1989 (and 1999) this scenario was extended to binary
1830:
1636:
1226:
1191:
786:
781:
776:
771:
721:
379:
352:
196:
135:
88:
67:
4227:
4127:
4100:
4078:
3683:
3424:
3363:
3210:
3145:
3084:
2586:
2131:
2084:
Kasen, D.; Metzger, B.; Barnes, J.; Quataert, E.; Ramirez-Ruiz, E. (2017).
1838:
1826:
1727:
1512:
1000:
984:
960:
887:
716:
691:
676:
421:
369:
226:
2600:
Bartlett, A.; Görres, J.; Mathews, G.J.; Otsuki, K.; Wiescher, W. (2006).
4329:
4237:
4132:
4122:
4110:
4035:
3948:
3509:
1842:
1834:
1777:
1660:
1640:
1620: = 50, 82, and 126—which are about 10 protons removed from the
1524:
1515:
which is greater than the energy of nuclear beta decay. However, nuclear
1218:
1027:
922:
681:
374:
296:
149:
3415:
3378:
3136:
3099:
3075:
3034:
3018:
2981:
2122:
2085:
1600:
creates an abundance of stable nuclei having closed neutron shells, the
1415:-process–rich stellar compositions must have been born earlier than any
4344:
4339:
4334:
4314:
4115:
3991:
3953:
3850:
3660:
3514:
1850:
1532:
1508:
1255:
1231:
1214:
1199:
1198:
at non-negligible abundances. This became the foundation of a study by
1138: in this section. Unsourced material may be challenged and removed.
651:
641:
498:
478:
301:
171:
2912:
2887:
2789:
2363:
2240:
2186:
2149:
1784:-process nuclei near their waiting points. Two distinct mass regions (
1371:-process nucleosynthesis; so each scenario fits the earlier growth of
4324:
4304:
4299:
4294:
4289:
4244:
3938:
3870:
3800:
3766:
3655:
3647:
3604:
3519:
3305:
3278:
1862:
1750:
1676:
1594:
1493:
1046:
1022:-process-like series of neutron captures occurs to a minor extent in
895:
891:
696:
646:
473:
456:
335:
3460:
1978:
1976:
1974:
1972:
1970:
1968:
1616:
produced from successive beta decays of waiting point nuclei having
1113:
963:, typically beginning with nuclei in the abundance peak centered on
4309:
4274:
4269:
4264:
4088:
3928:
3354:
3321:
3262:
3233:
3177:
3118:
3057:
3000:
2888:"Sensitivity studies for the weak r process: neutron capture rates"
2559:
2463:
2434:
2415:
2386:
2342:; Thielemann, Friedrich-Karl (2019). "The origin of the elements".
2168:
2104:
1983:
Burbidge, E. M.; Burbidge, G. R.; Fowler, W. A.; Hoyle, F. (1957).
1846:
1765:
1731:
1663:-291 and -293 which may have half-lives of centuries or millennia.
1632:
1187:
1175:
1167:
1008:
3397:
2947:
2749:
1817:-process is that it is radiogenic power from radioactive decay of
30:
4284:
4254:
4232:
1965:
1773:
1769:
1644:
1562:-process nucleosynthesis leads to the formation of neutron-rich,
1278:
1225:
of neutrons as well as abundance peaks about 10 amu lighter than
1031:
972:
964:
158:
131:
123:
55:
45:
2298:
Suess, H. E.; Urey, H. C. (1956). "Abundances of the
Elements".
2032:; et al. (2011). "What are the astrophysical sites for the
1821:-process nuclei that maintains the visibility of these spun off
4279:
4083:
1691:), which may provide the necessary physical conditions for the
1327:-process isotopes than BFH had been able to define. Today, the
1289:, who found that no single temporal snapshot matched the solar
1183:
1171:
50:
2212:
Cowan, John J.; Thielemann, Friedrich-Karl
Thielemann (2004).
1570:
as low as 2 MeV. At this stage, closed neutron shells at
1068:-process primarily occurs within ordinary stars, particularly
1015:-process elements is a matter of ongoing research as of 2018.
3735:
3439:"Neutron star mergers may create much of the universe's gold"
3319:
1234:, and the resulting abundance peaks were caused by so-called
1711:, or that each supernova ejects only a very small amount of
890:, the "heavy elements", with the other half produced by the
3943:
2885:
2599:
1982:
1911:
neutrons 1,674,927,471,000,000,000,000,000/cc vs 1 atom/cc
1612:-process peaks. These abundance peaks correspond to stable
1458:
1056:
captures of neutrons. In general, isotopes involved in the
3277:
Eichler, D.; Livio, M.; Piran, T.; Schramm, D. N. (1989).
2083:
3039:-process nucleosynthesis in a double neutron-star merger"
3320:
Freiburghaus, C.; Rosswog, S.; Thielemann, F.-K (1999).
3276:
2334:
4166:
Timeline of white dwarfs, neutron stars, and supernovae
3158:
2392:
1726:-process was discovered in data from the merger of two
1531:
by still-existing heavy nuclei occurs much faster than
1026:
explosions. These led to the discovery of the elements
2926:
2435:"Nucleosynthesis of heavy elements by neutron capture"
1445:-process, which is powered by supernova neutron bursts
1076:-process, which requires 100 captures per second. The
2710:
2708:
2433:
Seeger, P. A.; Fowler, W. A.; Clayton, D. D. (1965).
1675:-process has long been suggested to be core-collapse
1543:
and highly-unstable neutron-rich nuclei are created.
1872:
1829:
matter. It was proposed such matter is ejected from
2873:
2860:
2840:
Principles of
Stellar Evolution and Nucleosynthesis
2787:
2495:
2478:
2432:
1742:-process matter of lower-mass-range heavy nuclei (
2837:
2794:-process and the synthesis of superheavy elements"
2788:Boleu, R.; Nilsson, S. G.; Sheline, R. K. (1972).
2705:
2192:Nuclear physicists are still working to model the
1407:-process can begin after two million years. These
1262:-process and outlined the physics that guides it.
1190:, though there was no explanation for elements of
2263:Monthly Notices of the Royal Astronomical Society
2036:-process and the production of heavy elements?".
4456:
1730:. Using the gravitational wave data captured in
1209:The need for a physical setting providing rapid
3231:
2927:Zagrebaev, V.; Karpov, A.; Greiner, W. (2013).
1254:-process isotopes was published in 1957 in the
2879:
2387:"Nuclear reactions in stars and nucleogenesis"
1753:) and cooler red masses of higher mass-number
3751:
3476:
2259:"The Synthesis of the Elements from Hydrogen"
1813:-process nuclei. Confirming relevance to the
1695:-process. However, the very low abundance of
913:because they are created exclusively via the
841:
4381:Monte Agliale Supernovae and Asteroid Survey
2024:
2022:
1581:Decreasing nuclear stability terminates the
1488:There are three natural candidate sites for
1186:. Their theory accounted for elements up to
2661:
2147:
3758:
3744:
3483:
3469:
2664:"Reaching the limits of nuclear stability"
2028:
848:
834:
3414:
3396:
3353:
3343:
3304:
3261:
3251:
3176:
3135:
3117:
3074:
3056:
3017:
2999:
2964:
2946:
2920:
2911:
2748:
2576:
2558:
2523:
2462:
2452:
2428:
2426:
2414:
2404:
2297:
2282:
2214:"R-Process Nucleosynthesis in Supernovae"
2185:
2167:
2121:
2103:
2019:
2010:
1722:In 2017, new astronomical data about the
1671:The most probable candidate site for the
1266:also published a smaller study about the
1206:that would be formed in such conditions.
1154:Learn how and when to remove this message
1096:-processes account for almost the entire
3232:Lattimer, J. M.; Schramm, D. N. (1974).
2734:
2728:
2655:
2593:
2150:"The formation of the heaviest elements"
2143:
2141:
2039:Progress in Particle and Nuclear Physics
1470:
1433:
2832:
2724:(Doctoral thesis). University of Basel.
2714:
2602:"Two-neutron capture reactions and the
2384:
2252:
2250:
2079:
2077:
1166:Following pioneering research into the
971:(typically via β decay) before another
4457:
3376:
3097:
2979:
2538:
2532:
2507:
2423:
1666:
959:(hence the name) by one or more heavy
3796:Type II (IIP, IIL, IIn, and IIb)
3739:
3490:
3464:
2934:Journal of Physics: Conference Series
2256:
2138:
4439:
3234:"Black Hole–Neutron Star Collisions"
3032:
2247:
2074:
1985:"Synthesis of the Elements in Stars"
1519:still occurs, and causes increasing
1403:-process to get started whereas the
1136:adding citations to reliable sources
1107:
4376:Katzman Automatic Imaging Telescope
3098:Smartt, S. J.; et al. (2017).
1951: = 90, 138, 208, respectively.
13:
1483:
917:-process. Abundance peaks for the
14:
4496:
3326:-process in Neutron Star Mergers"
3035:"Spectroscopic identification of
2874:Seeger, Fowler & Clayton 1965
2861:Seeger, Fowler & Clayton 1965
2496:Seeger, Fowler & Clayton 1965
2479:Seeger, Fowler & Clayton 1965
2148:Frebel, A.; Beers, T. C. (2018).
1457:-process was discovered when the
952:-process entails a succession of
4438:
4429:
4428:
4161:History of supernova observation
3829:
3377:Tanvir, N.; et al. (2013).
2980:Arcavi, I.; et al. (2017).
2440:Astrophysical Journal Supplement
1889:
1875:
1527:. As this re-expands and cools,
1112:
815:
814:
801:
29:
3431:
3370:
3313:
3270:
3225:
3152:
3091:
3026:
2973:
2866:
2826:
2781:
2501:
2488:
2471:
2378:
2328:
1929:
1517:capture of those free electrons
1356:primary nucleosynthesis process
1339:-process nucleosynthesis. That
1311:. Subsequent treatments of the
1123:needs additional citations for
4406:SuperNova Early Warning System
3821:Common envelope jets supernova
3765:
3033:Pian, E.; et al. (2017).
2966:10.1088/1742-6596/420/1/012001
2671:Reports on Progress in Physics
2578:10.1103/PhysRevLett.119.161101
2291:
2205:
1917:
1905:
1098:abundance of chemical elements
1003:matter thrown off by a binary
1:
3445:. Science AAAS. 20 March 2018
3331:Astrophysical Journal Letters
3239:Astrophysical Journal Letters
1958:
938:(elements Te, I, and Xe) and
883:of approximately half of the
866:rapid neutron-capture process
4396:Supernova/Acceleration Probe
4371:High-Z Supernova Search Team
3969:pulsational pair-instability
2820:10.1016/0370-2693(72)90470-4
1554:, the inhibiting process of
1045:-process contrasts with the
7:
4401:Supernova Cosmology Project
3909:Fast blue optical transient
2790:"On the termination of the
1856:
1568:neutron separation energies
1539:-process runs up along the
1419:-process, showing that the
1270:-process in the same year.
945:(elements Os, Ir, and Pt).
931:(elements Se, Br, and Kr),
595:High-energy nuclear physics
10:
4501:
2767:10.1103/PhysRevC.92.031303
2691:10.1088/0034-4885/67/7/R04
2635:10.1103/PhysRevC.74.015802
2511:Astronomy and Astrophysics
2385:Cameron, A. G. W. (1957).
2060:10.1016/j.ppnp.2011.01.032
1387:-process curve, as if the
1180:Subrahmanyan Chandrasekhar
1103:
4424:
4353:
4215:
4174:
4148:
4059:
3984:
3896:
3838:
3827:
3773:
3713:
3692:
3669:
3578:
3498:
3195:10.1038/s41586-019-1676-3
2844:, Mc-Graw-Hill, pp.
2301:Reviews of Modern Physics
2012:10.1103/RevModPhys.29.547
1990:Reviews of Modern Physics
1947: = 80, 130, 196 and
997:supernova nucleosynthesis
4465:Concepts in astrophysics
4386:Nearby Supernova Factory
2743:(3): 031303–1–031303–5.
2662:Thoennessen, M. (2004).
2322:10.1103/RevModPhys.28.53
1935:Abundance peaks for the
1868:
1653:spontaneously fissioning
1535:. As a consequence, the
879:that is responsible for
4411:Supernova Legacy Survey
3535:Double electron capture
2546:Physical Review Letters
2525:1981A&A....97..391T
2284:10.1093/mnras/106.5.343
1707:-process nuclei to the
1476:Noteworthy is that the
993:core-collapse supernova
106:Interacting boson model
16:Nucleosynthesis pathway
4416:Texas Supernova Search
4391:Sloan Supernova Survey
4009:Luminous blue variable
2715:Eichler, M.A. (2016).
1622:line of beta stability
1550:in nuclei with closed
1446:
1281:by Phillip A. Seeger,
1264:Alastair G. W. Cameron
1242:-process, whereas the
1204:abundances of elements
1036:nuclear weapon fallout
999:, or decompression of
3861:Phillips relationship
1639:and the new elements
1469:-process matter. See
1437:
1170:and the formation of
493:High-energy processes
191:– equal all the above
89:Models of the nucleus
1502:neutron star mergers
1132:improve this article
1024:thermonuclear weapon
921:-process occur near
868:, also known as the
862:nuclear astrophysics
529:nuclear astrophysics
4434:Category:Supernovae
4366:Calán/Tololo Survey
4051:Population III star
3959:Soft gamma repeater
3791:Type Ib and Ic
3679:Photodisintegration
3600:Proton–proton chain
3570:Spontaneous fission
3550:Isomeric transition
3545:Internal conversion
3416:10.1038/nature12505
3407:2013Natur.500..547T
3345:1999ApJ...525L.121F
3297:1989Natur.340..126E
3253:1974ApJ...192L.145L
3187:2019Natur.574..497W
3137:10.1038/nature24303
3128:2017Natur.551...75S
3076:10.1038/nature24298
3067:2017Natur.551...67P
3019:10.1038/nature24291
3010:2017Natur.551...64A
2957:2013JPhCS.420a2001Z
2904:2014AIPA....4d1008S
2812:1972PhLB...40..517B
2759:2015PhRvC..92c1303W
2683:2004RPPh...67.1187T
2627:2006PhRvC..74a5802B
2569:2017PhRvL.119p1101A
2454:1965ApJS...11..121S
2406:1957PASP...69..201C
2356:2019PhT....72b..36W
2314:1956RvMP...28...53S
2275:1946MNRAS.106..343H
2233:2004PhT....57j..47C
2178:2018PhT....71a..30F
2123:10.1038/nature24453
2114:2017Natur.551...80K
2052:2011PrPNP..66..346T
2003:1957RvMP...29..547B
1709:interstellar medium
1667:Astrophysical sites
1649:island of stability
1556:photodisintegration
1471:Astrophysical sites
1258:, which named the
1005:neutron star merger
511:Photodisintegration
434:Capturing processes
348:Spontaneous fission
341:Internal conversion
272:Valley of stability
267:Island of stability
101:Nuclear shell model
4444:Commons:Supernovae
4096:Stellar black hole
4072:Pulsar wind nebula
3924:Gravitational wave
2257:Hoyle, F. (1946).
1943:-processes are at
1913:interstellar space
1843:binary star system
1498:Type II supernovae
1447:
808:Physics portal
602:Quark–gluon plasma
385:Radiogenic nuclide
4452:
4451:
4067:Supernova remnant
3934:Luminous red nova
3846:Carbon detonation
3733:
3732:
3729:
3728:
3560:Positron emission
3530:Double beta decay
3492:Nuclear processes
3291:(6229): 126–128.
3171:(7779): 497–500.
3161:Arcones, Almudena
2913:10.1063/1.4867191
2898:(41008): 041008.
2799:Physics Letters B
2737:Physical Review C
2614:Physical Review C
2364:10.1063/PT.3.4134
2340:Trimble, Virginia
2241:10.1063/1.1825268
2187:10.1063/pt.3.3815
2030:Thielemann, F.-K.
1757:-process nuclei (
1719:-process yields.
1578:of the reaction.
1541:neutron drip line
1431:-process nuclei.
1360:secondary process
1287:Donald D. Clayton
1283:William A. Fowler
1164:
1163:
1156:
1034:(element 100) in
1030:(element 99) and
977:neutron drip line
969:radioactive decay
888:heavier than iron
877:nuclear reactions
858:
857:
544:
290:Radioactive decay
246:Nuclear stability
73:Nuclear structure
4492:
4442:
4441:
4432:
4431:
4295:Remnant G1.9+0.3
3914:Fast radio burst
3833:
3811:Pair-instability
3760:
3753:
3746:
3737:
3736:
3690:
3689:
3590:Deuterium fusion
3555:Neutron emission
3540:Electron capture
3485:
3478:
3471:
3462:
3461:
3455:
3454:
3452:
3450:
3435:
3429:
3428:
3418:
3400:
3374:
3368:
3367:
3357:
3347:
3338:(2): L121–L124.
3317:
3311:
3310:
3308:
3306:10.1038/340126a0
3274:
3268:
3267:
3265:
3255:
3229:
3223:
3222:
3180:
3156:
3150:
3149:
3139:
3121:
3095:
3089:
3088:
3078:
3060:
3030:
3024:
3023:
3021:
3003:
2977:
2971:
2970:
2968:
2950:
2924:
2918:
2917:
2915:
2883:
2877:
2870:
2864:
2858:
2843:
2830:
2824:
2823:
2785:
2779:
2778:
2752:
2732:
2726:
2725:
2723:
2712:
2703:
2702:
2677:(7): 1187–1232.
2668:
2659:
2653:
2652:
2650:
2649:
2643:
2637:. Archived from
2610:
2597:
2591:
2590:
2580:
2562:
2536:
2530:
2529:
2527:
2505:
2499:
2492:
2486:
2475:
2469:
2468:
2466:
2456:
2430:
2421:
2420:
2418:
2408:
2382:
2376:
2375:
2332:
2326:
2325:
2295:
2289:
2288:
2286:
2254:
2245:
2244:
2218:
2209:
2203:
2202:
2189:
2171:
2145:
2136:
2135:
2125:
2107:
2081:
2072:
2071:
2026:
2017:
2016:
2014:
1980:
1952:
1933:
1927:
1921:
1915:
1909:
1899:
1894:
1893:
1885:
1883:Astronomy portal
1880:
1879:
1878:
1797:
1790:
1763:
1748:
1679:(spectral types
1533:beta-minus decay
1509:beta-minus decay
1310:
1303:
1256:BFH review paper
1194:heavier than 40
1159:
1152:
1148:
1145:
1139:
1116:
1108:
957:neutron captures
944:
937:
930:
850:
843:
836:
823:
818:
817:
810:
806:
805:
682:Skłodowska-Curie
542:
358:Neutron emission
126:' classification
78:Nuclear reaction
33:
19:
18:
4500:
4499:
4495:
4494:
4493:
4491:
4490:
4489:
4480:Nucleosynthesis
4475:Nuclear physics
4455:
4454:
4453:
4448:
4420:
4349:
4335:SN 2016aps
4315:SN Refsdal
4211:
4170:
4144:
4055:
4041:Wolf–Rayet star
3980:
3919:Gamma-ray burst
3892:
3866:Nucleosynthesis
3834:
3825:
3769:
3764:
3734:
3725:
3709:
3700:Neutron capture
3688:
3671:
3665:
3582:nucleosynthesis
3581:
3574:
3565:Proton emission
3520:Gamma radiation
3501:
3494:
3489:
3459:
3458:
3448:
3446:
3437:
3436:
3432:
3391:(7464): 547–9.
3375:
3371:
3318:
3314:
3275:
3271:
3246:(2): L145–147.
3230:
3226:
3157:
3153:
3112:(7678): 75–79.
3096:
3092:
3051:(7678): 67–70.
3031:
3027:
2994:(7678): 64–66.
2978:
2974:
2925:
2921:
2884:
2880:
2871:
2867:
2856:
2831:
2827:
2786:
2782:
2733:
2729:
2721:
2713:
2706:
2666:
2660:
2656:
2647:
2645:
2641:
2608:
2598:
2594:
2537:
2533:
2506:
2502:
2494:See Table 4 in
2493:
2489:
2476:
2472:
2431:
2424:
2383:
2379:
2333:
2329:
2296:
2292:
2255:
2248:
2216:
2210:
2206:
2146:
2139:
2098:(7678): 80–84.
2082:
2075:
2027:
2020:
1981:
1966:
1961:
1956:
1955:
1934:
1930:
1922:
1918:
1910:
1906:
1895:
1888:
1881:
1876:
1874:
1871:
1859:
1792:
1785:
1758:
1743:
1669:
1587:fission barrier
1529:neutron capture
1486:
1484:Nuclear physics
1411:-process–poor,
1381:James W. Truran
1305:
1298:
1273:The stationary
1211:neutron capture
1160:
1149:
1143:
1140:
1129:
1117:
1106:
939:
932:
925:
854:
813:
800:
799:
792:
791:
627:
617:
616:
597:
587:
586:
531:
527:
524:Nucleosynthesis
516:
515:
494:
486:
485:
435:
427:
426:
400:
398:Nuclear fission
390:
389:
363:Proton emission
292:
282:
281:
247:
239:
238:
140:
127:
116:
115:
91:
23:Nuclear physics
17:
12:
11:
5:
4498:
4488:
4487:
4482:
4477:
4472:
4467:
4450:
4449:
4447:
4446:
4436:
4425:
4422:
4421:
4419:
4418:
4413:
4408:
4403:
4398:
4393:
4388:
4383:
4378:
4373:
4368:
4363:
4357:
4355:
4351:
4350:
4348:
4347:
4342:
4337:
4332:
4327:
4325:SN 2006gy
4322:
4317:
4312:
4307:
4305:SN 2011fe
4302:
4300:SN 2007bi
4297:
4292:
4290:SN 2003fg
4287:
4282:
4277:
4272:
4267:
4262:
4257:
4252:
4247:
4242:
4241:
4240:
4230:
4225:
4223:Barnard's Loop
4219:
4217:
4213:
4212:
4210:
4209:
4204:
4199:
4194:
4189:
4184:
4178:
4176:
4172:
4171:
4169:
4168:
4163:
4158:
4152:
4150:
4146:
4145:
4143:
4142:
4141:
4140:
4138:Orion–Eridanus
4130:
4125:
4120:
4119:
4118:
4113:
4108:
4098:
4093:
4092:
4091:
4086:
4076:
4075:
4074:
4063:
4061:
4057:
4056:
4054:
4053:
4048:
4046:Super-AGB star
4043:
4038:
4033:
4032:
4031:
4026:
4021:
4011:
4006:
4005:
4004:
3999:
3988:
3986:
3982:
3981:
3979:
3978:
3976:Symbiotic nova
3973:
3972:
3971:
3961:
3956:
3951:
3946:
3941:
3936:
3931:
3926:
3921:
3916:
3911:
3906:
3900:
3898:
3894:
3893:
3891:
3890:
3885:
3884:
3883:
3878:
3873:
3863:
3858:
3853:
3848:
3842:
3840:
3836:
3835:
3828:
3826:
3824:
3823:
3818:
3813:
3808:
3803:
3798:
3793:
3788:
3783:
3777:
3775:
3771:
3770:
3763:
3762:
3755:
3748:
3740:
3731:
3730:
3727:
3726:
3724:
3723:
3721:(n-p) reaction
3717:
3715:
3711:
3710:
3708:
3707:
3705:Proton capture
3702:
3696:
3694:
3687:
3686:
3681:
3675:
3673:
3667:
3666:
3664:
3663:
3658:
3653:
3645:
3637:
3632:
3627:
3622:
3617:
3612:
3607:
3602:
3597:
3592:
3586:
3584:
3576:
3575:
3573:
3572:
3567:
3562:
3557:
3552:
3547:
3542:
3537:
3532:
3527:
3522:
3517:
3512:
3506:
3504:
3496:
3495:
3488:
3487:
3480:
3473:
3465:
3457:
3456:
3430:
3369:
3355:10.1086/312343
3312:
3269:
3263:10.1086/181612
3224:
3151:
3090:
3025:
2972:
2919:
2878:
2865:
2855:978-0226109534
2854:
2834:Clayton, D. D.
2825:
2806:(5): 517–521.
2780:
2727:
2704:
2654:
2592:
2553:(16): 161101.
2531:
2500:
2487:
2470:
2464:10.1086/190111
2422:
2416:10.1086/127051
2377:
2327:
2290:
2269:(5): 343–383.
2246:
2204:
2137:
2073:
2046:(2): 346–353.
2018:
1997:(4): 547–650.
1963:
1962:
1960:
1957:
1954:
1953:
1928:
1926:50, 82 and 126
1924:Neutron number
1916:
1903:
1902:
1901:
1900:
1897:Physics portal
1886:
1870:
1867:
1866:
1865:
1858:
1855:
1668:
1665:
1659:nuclides like
1552:neutron shells
1521:neutronization
1485:
1482:
1439:Periodic table
1236:waiting points
1162:
1161:
1120:
1118:
1111:
1105:
1102:
1064:-process. The
875:, is a set of
856:
855:
853:
852:
845:
838:
830:
827:
826:
825:
824:
811:
794:
793:
790:
789:
784:
779:
774:
769:
764:
759:
754:
749:
744:
739:
734:
729:
724:
719:
714:
709:
704:
699:
694:
689:
684:
679:
674:
669:
664:
659:
654:
649:
644:
639:
634:
628:
623:
622:
619:
618:
615:
614:
609:
604:
598:
593:
592:
589:
588:
585:
584:
583:
582:
577:
572:
563:
562:
561:
560:
555:
550:
539:
538:
536:Nuclear fusion
532:
522:
521:
518:
517:
514:
513:
508:
507:
506:
495:
492:
491:
488:
487:
484:
483:
482:
481:
476:
466:
465:
464:
459:
449:
448:
447:
436:
433:
432:
429:
428:
425:
424:
419:
418:
417:
407:
401:
396:
395:
392:
391:
388:
387:
382:
377:
372:
366:
365:
360:
355:
350:
345:
344:
343:
338:
328:
323:
322:
321:
316:
315:
314:
299:
293:
288:
287:
284:
283:
280:
279:
277:Stable nuclide
274:
269:
264:
259:
254:
252:Binding energy
248:
245:
244:
241:
240:
237:
236:
235:
234:
224:
219:
214:
208:
207:
193:
192:
185:
184:
168:
167:
155:
154:
142:
141:
128:
122:
121:
118:
117:
114:
113:
108:
103:
98:
92:
87:
86:
83:
82:
81:
80:
75:
70:
65:
63:Nuclear matter
60:
59:
58:
53:
43:
35:
34:
26:
25:
15:
9:
6:
4:
3:
2:
4497:
4486:
4483:
4481:
4478:
4476:
4473:
4471:
4468:
4466:
4463:
4462:
4460:
4445:
4437:
4435:
4427:
4426:
4423:
4417:
4414:
4412:
4409:
4407:
4404:
4402:
4399:
4397:
4394:
4392:
4389:
4387:
4384:
4382:
4379:
4377:
4374:
4372:
4369:
4367:
4364:
4362:
4359:
4358:
4356:
4352:
4346:
4343:
4341:
4338:
4336:
4333:
4331:
4328:
4326:
4323:
4321:
4318:
4316:
4313:
4311:
4310:SN 2014J
4308:
4306:
4303:
4301:
4298:
4296:
4293:
4291:
4288:
4286:
4283:
4281:
4278:
4276:
4275:SN 1994D
4273:
4271:
4270:SN 1987A
4268:
4266:
4265:SN 1885A
4263:
4261:
4258:
4256:
4253:
4251:
4248:
4246:
4243:
4239:
4236:
4235:
4234:
4231:
4229:
4226:
4224:
4221:
4220:
4218:
4214:
4208:
4205:
4203:
4200:
4198:
4195:
4193:
4192:Massive stars
4190:
4188:
4185:
4183:
4180:
4179:
4177:
4173:
4167:
4164:
4162:
4159:
4157:
4154:
4153:
4151:
4147:
4139:
4136:
4135:
4134:
4131:
4129:
4126:
4124:
4121:
4117:
4114:
4112:
4109:
4107:
4104:
4103:
4102:
4099:
4097:
4094:
4090:
4087:
4085:
4082:
4081:
4080:
4077:
4073:
4070:
4069:
4068:
4065:
4064:
4062:
4058:
4052:
4049:
4047:
4044:
4042:
4039:
4037:
4034:
4030:
4027:
4025:
4022:
4020:
4017:
4016:
4015:
4012:
4010:
4007:
4003:
4000:
3998:
3995:
3994:
3993:
3990:
3989:
3987:
3983:
3977:
3974:
3970:
3967:
3966:
3965:
3962:
3960:
3957:
3955:
3952:
3950:
3947:
3945:
3942:
3940:
3937:
3935:
3932:
3930:
3927:
3925:
3922:
3920:
3917:
3915:
3912:
3910:
3907:
3905:
3902:
3901:
3899:
3895:
3889:
3886:
3882:
3879:
3877:
3874:
3872:
3869:
3868:
3867:
3864:
3862:
3859:
3857:
3854:
3852:
3849:
3847:
3844:
3843:
3841:
3837:
3832:
3822:
3819:
3817:
3814:
3812:
3809:
3807:
3806:Superluminous
3804:
3802:
3799:
3797:
3794:
3792:
3789:
3787:
3786:Type Iax
3784:
3782:
3779:
3778:
3776:
3772:
3768:
3761:
3756:
3754:
3749:
3747:
3742:
3741:
3738:
3722:
3719:
3718:
3716:
3712:
3706:
3703:
3701:
3698:
3697:
3695:
3691:
3685:
3682:
3680:
3677:
3676:
3674:
3668:
3662:
3659:
3657:
3654:
3652:
3650:
3646:
3644:
3642:
3638:
3636:
3633:
3631:
3628:
3626:
3623:
3621:
3618:
3616:
3613:
3611:
3608:
3606:
3603:
3601:
3598:
3596:
3593:
3591:
3588:
3587:
3585:
3583:
3577:
3571:
3568:
3566:
3563:
3561:
3558:
3556:
3553:
3551:
3548:
3546:
3543:
3541:
3538:
3536:
3533:
3531:
3528:
3526:
3525:Cluster decay
3523:
3521:
3518:
3516:
3513:
3511:
3508:
3507:
3505:
3503:
3497:
3493:
3486:
3481:
3479:
3474:
3472:
3467:
3466:
3463:
3444:
3440:
3434:
3426:
3422:
3417:
3412:
3408:
3404:
3399:
3394:
3390:
3386:
3385:
3380:
3373:
3365:
3361:
3356:
3351:
3346:
3341:
3337:
3333:
3332:
3327:
3325:
3316:
3307:
3302:
3298:
3294:
3290:
3286:
3285:
3280:
3273:
3264:
3259:
3254:
3249:
3245:
3241:
3240:
3235:
3228:
3220:
3216:
3212:
3208:
3204:
3200:
3196:
3192:
3188:
3184:
3179:
3174:
3170:
3166:
3162:
3155:
3147:
3143:
3138:
3133:
3129:
3125:
3120:
3115:
3111:
3107:
3106:
3101:
3094:
3086:
3082:
3077:
3072:
3068:
3064:
3059:
3054:
3050:
3046:
3045:
3040:
3038:
3029:
3020:
3015:
3011:
3007:
3002:
2997:
2993:
2989:
2988:
2983:
2976:
2967:
2962:
2958:
2954:
2949:
2944:
2941:(1): 012001.
2940:
2936:
2935:
2930:
2923:
2914:
2909:
2905:
2901:
2897:
2893:
2889:
2882:
2875:
2872:Figure 10 of
2869:
2862:
2857:
2851:
2847:
2842:
2841:
2835:
2829:
2821:
2817:
2813:
2809:
2805:
2801:
2800:
2795:
2793:
2784:
2776:
2772:
2768:
2764:
2760:
2756:
2751:
2746:
2742:
2738:
2731:
2720:
2719:
2711:
2709:
2700:
2696:
2692:
2688:
2684:
2680:
2676:
2672:
2665:
2658:
2644:on 2020-08-06
2640:
2636:
2632:
2628:
2624:
2621:(1): 015082.
2620:
2616:
2615:
2607:
2605:
2596:
2588:
2584:
2579:
2574:
2570:
2566:
2561:
2556:
2552:
2548:
2547:
2542:
2535:
2526:
2521:
2518:(2): 391–93.
2517:
2513:
2512:
2504:
2497:
2491:
2484:
2480:
2474:
2465:
2460:
2455:
2450:
2446:
2442:
2441:
2436:
2429:
2427:
2417:
2412:
2407:
2402:
2398:
2394:
2393:
2388:
2381:
2373:
2369:
2365:
2361:
2357:
2353:
2349:
2345:
2344:Physics Today
2341:
2337:
2336:Woosley, Stan
2331:
2323:
2319:
2315:
2311:
2307:
2303:
2302:
2294:
2285:
2280:
2276:
2272:
2268:
2264:
2260:
2253:
2251:
2242:
2238:
2234:
2230:
2227:(10): 47–54.
2226:
2222:
2221:Physics Today
2215:
2208:
2201:
2199:
2195:
2188:
2183:
2179:
2175:
2170:
2165:
2161:
2157:
2156:
2155:Physics Today
2151:
2144:
2142:
2133:
2129:
2124:
2119:
2115:
2111:
2106:
2101:
2097:
2093:
2092:
2087:
2080:
2078:
2069:
2065:
2061:
2057:
2053:
2049:
2045:
2041:
2040:
2035:
2031:
2025:
2023:
2013:
2008:
2004:
2000:
1996:
1992:
1991:
1986:
1979:
1977:
1975:
1973:
1971:
1969:
1964:
1950:
1946:
1942:
1938:
1932:
1925:
1920:
1914:
1908:
1904:
1898:
1892:
1887:
1884:
1873:
1864:
1861:
1860:
1854:
1852:
1848:
1844:
1840:
1836:
1833:merging with
1832:
1831:neutron stars
1828:
1824:
1820:
1816:
1812:
1807:
1805:
1801:
1795:
1788:
1783:
1779:
1775:
1771:
1767:
1761:
1756:
1752:
1746:
1741:
1737:
1733:
1729:
1728:neutron stars
1725:
1720:
1718:
1714:
1710:
1706:
1702:
1698:
1694:
1690:
1686:
1682:
1678:
1674:
1664:
1662:
1658:
1654:
1650:
1646:
1642:
1638:
1637:plutonium-244
1634:
1630:
1625:
1623:
1619:
1615:
1611:
1607:
1603:
1599:
1597:
1592:
1588:
1584:
1579:
1577:
1573:
1569:
1565:
1561:
1557:
1553:
1549:
1548:cross section
1544:
1542:
1538:
1534:
1530:
1526:
1522:
1518:
1514:
1510:
1505:
1503:
1499:
1495:
1491:
1481:
1479:
1474:
1472:
1468:
1464:
1460:
1456:
1452:
1444:
1440:
1436:
1432:
1430:
1426:
1422:
1418:
1414:
1410:
1406:
1402:
1398:
1394:
1390:
1386:
1382:
1378:
1374:
1370:
1366:
1361:
1357:
1353:
1348:
1346:
1342:
1338:
1334:
1330:
1326:
1322:
1319:-process and
1318:
1314:
1308:
1301:
1296:
1292:
1288:
1284:
1280:
1276:
1271:
1269:
1265:
1261:
1257:
1253:
1250:-process and
1249:
1245:
1241:
1237:
1233:
1228:
1227:stable nuclei
1224:
1223:magic numbers
1220:
1216:
1212:
1207:
1205:
1201:
1197:
1193:
1192:atomic weight
1189:
1185:
1181:
1177:
1173:
1169:
1158:
1155:
1147:
1137:
1133:
1127:
1126:
1121:This section
1119:
1115:
1110:
1109:
1101:
1099:
1095:
1091:
1087:
1083:
1079:
1075:
1071:
1067:
1063:
1059:
1055:
1051:
1049:
1044:
1039:
1037:
1033:
1029:
1025:
1021:
1016:
1014:
1010:
1006:
1002:
998:
995:, as part of
994:
990:
986:
985:free neutrons
982:
978:
974:
970:
966:
962:
958:
955:
951:
946:
942:
935:
928:
924:
920:
916:
912:
911:r-only nuclei
908:
904:
900:
898:
893:
889:
886:
885:atomic nuclei
882:
878:
874:
872:
867:
863:
851:
846:
844:
839:
837:
832:
831:
829:
828:
822:
812:
809:
804:
798:
797:
796:
795:
788:
785:
783:
780:
778:
775:
773:
770:
768:
765:
763:
760:
758:
755:
753:
750:
748:
745:
743:
740:
738:
735:
733:
730:
728:
725:
723:
720:
718:
715:
713:
710:
708:
705:
703:
700:
698:
695:
693:
690:
688:
685:
683:
680:
678:
675:
673:
670:
668:
665:
663:
660:
658:
655:
653:
650:
648:
645:
643:
640:
638:
635:
633:
630:
629:
626:
621:
620:
613:
610:
608:
605:
603:
600:
599:
596:
591:
590:
581:
578:
576:
573:
571:
568:
567:
565:
564:
559:
556:
554:
551:
549:
546:
545:
541:
540:
537:
534:
533:
530:
525:
520:
519:
512:
509:
505:
504:by cosmic ray
502:
501:
500:
497:
496:
490:
489:
480:
477:
475:
472:
471:
470:
467:
463:
460:
458:
455:
454:
453:
450:
446:
443:
442:
441:
438:
437:
431:
430:
423:
420:
416:
415:pair breaking
413:
412:
411:
408:
406:
403:
402:
399:
394:
393:
386:
383:
381:
380:Decay product
378:
376:
373:
371:
368:
367:
364:
361:
359:
356:
354:
353:Cluster decay
351:
349:
346:
342:
339:
337:
334:
333:
332:
329:
327:
324:
320:
317:
313:
310:
309:
308:
305:
304:
303:
300:
298:
295:
294:
291:
286:
285:
278:
275:
273:
270:
268:
265:
263:
260:
258:
255:
253:
250:
249:
243:
242:
233:
230:
229:
228:
225:
223:
220:
218:
215:
213:
210:
209:
206:
202:
198:
197:Mirror nuclei
195:
194:
190:
187:
186:
183:
182:
179: −
178:
173:
170:
169:
166:
165:
160:
157:
156:
153:
152:
147:
144:
143:
139:
138:
133:
130:
129:
125:
120:
119:
112:
109:
107:
104:
102:
99:
97:
94:
93:
90:
85:
84:
79:
76:
74:
71:
69:
68:Nuclear force
66:
64:
61:
57:
54:
52:
49:
48:
47:
44:
42:
39:
38:
37:
36:
32:
28:
27:
24:
21:
20:
4320:Vela Remnant
4285:SN 1006
4250:SN 1000+0216
4228:Cassiopeia A
4197:Most distant
4128:Local Bubble
4101:Compact star
4079:Neutron star
3875:
3816:Calcium-rich
3781:Type Ia
3684:Photofission
3648:
3640:
3639:
3447:. Retrieved
3442:
3433:
3388:
3382:
3372:
3335:
3329:
3323:
3315:
3288:
3282:
3272:
3243:
3237:
3227:
3168:
3164:
3154:
3109:
3103:
3093:
3048:
3042:
3036:
3028:
2991:
2985:
2975:
2938:
2932:
2922:
2895:
2892:AIP Advances
2891:
2881:
2868:
2839:
2828:
2803:
2797:
2791:
2783:
2740:
2736:
2730:
2717:
2674:
2670:
2657:
2646:. Retrieved
2639:the original
2618:
2612:
2603:
2595:
2550:
2544:
2534:
2515:
2509:
2503:
2490:
2482:
2473:
2444:
2438:
2399:(408): 201.
2396:
2390:
2380:
2350:(2): 36–37.
2347:
2343:
2330:
2308:(1): 53–74.
2305:
2299:
2293:
2266:
2262:
2224:
2220:
2207:
2197:
2193:
2191:
2162:(1): 30–37.
2159:
2153:
2095:
2089:
2043:
2037:
2033:
1994:
1988:
1948:
1944:
1940:
1936:
1931:
1919:
1907:
1851:Earth masses
1839:neutron star
1827:neutron star
1822:
1818:
1814:
1810:
1808:
1803:
1799:
1793:
1786:
1781:
1759:
1754:
1744:
1739:
1735:
1723:
1721:
1716:
1712:
1704:
1696:
1692:
1688:
1684:
1680:
1672:
1670:
1628:
1626:
1617:
1609:
1601:
1595:
1582:
1580:
1575:
1571:
1566:nuclei with
1564:weakly bound
1559:
1545:
1536:
1525:temperatures
1513:Fermi energy
1506:
1489:
1487:
1477:
1475:
1466:
1454:
1450:
1448:
1442:
1428:
1424:
1420:
1416:
1412:
1408:
1404:
1400:
1396:
1392:
1388:
1384:
1376:
1372:
1368:
1364:
1359:
1355:
1351:
1349:
1344:
1340:
1336:
1332:
1328:
1324:
1320:
1316:
1312:
1306:
1299:
1294:
1290:
1274:
1272:
1267:
1259:
1251:
1247:
1243:
1239:
1235:
1208:
1165:
1150:
1144:October 2022
1141:
1130:Please help
1125:verification
1122:
1093:
1089:
1085:
1081:
1080:-process is
1077:
1073:
1065:
1061:
1057:
1053:
1047:
1042:
1040:
1019:
1017:
1012:
1001:neutron star
988:
980:
953:
949:
947:
940:
933:
926:
923:mass numbers
918:
914:
910:
906:
902:
896:
881:the creation
870:
869:
865:
859:
461:
422:Photofission
370:Decay energy
297:Alpha α
204:
200:
180:
176:
163:
150:
136:
4330:ASASSN-15lh
4280:SN 185
4238:Crab Nebula
4133:Superbubble
4123:Zombie star
4106:electroweak
4036:White dwarf
3985:Progenitors
3949:Pulsar kick
3510:Alpha decay
3500:Radioactive
3443:Sid Perkins
1841:mergers (a
1835:black holes
1778:californium
1661:copernicium
1641:einsteinium
1591:radioactive
1354:-process a
1219:Harold Urey
1028:einsteinium
961:seed nuclei
727:Oppenheimer
405:Spontaneous
375:Decay chain
326:K/L capture
302:Beta β
172:Isodiaphers
96:Liquid drop
4485:Supernovae
4459:Categories
4345:SN 2022jli
4340:SN 2018cow
4207:In fiction
4182:Candidates
4156:Guest star
4014:Supergiant
3992:Hypergiant
3954:Quark-nova
3856:Near-Earth
3839:Physics of
3767:Supernovae
3661:rp-process
3635:Si burning
3625:Ne burning
3595:Li burning
3515:Beta decay
3178:1910.10510
3119:1710.05841
3058:1710.05858
3001:1710.05843
2648:2019-06-17
2560:1710.05832
2447:: 121–66.
2169:1801.01190
2105:1710.05463
1959:References
1798:) for the
1764:) rich in
1677:supernovae
1657:superheavy
1608:below the
1576:freeze-out
1494:supernovae
1347:-process.
1232:beta decay
1215:Hans Suess
1200:Fred Hoyle
1018:A limited
757:Strassmann
747:Rutherford
625:Scientists
580:Artificial
575:Cosmogenic
570:Primordial
566:Nuclides:
543:Processes:
499:Spallation
4245:iPTF14hls
4149:Discovery
3939:Micronova
3888:Neutrinos
3881:γ-process
3876:r-process
3871:p-process
3851:Foe/Bethe
3801:Hypernova
3672:processes
3656:p-process
3630:O burning
3620:C burning
3610:α process
3605:CNO cycle
3398:1306.4971
3219:204837882
3203:0028-0836
2948:1207.5700
2750:1410.2498
2699:250790169
2372:186549912
2068:119412716
1863:HD 222925
1853:of gold.
1768:(such as
1766:actinides
1751:strontium
1699:-process
1633:actinides
1082:secondary
1070:AGB stars
892:p-process
762:Świątecki
677:Pi. Curie
672:Fr. Curie
667:Ir. Curie
662:Cockcroft
637:Becquerel
558:Supernova
262:Drip line
257:p–n ratio
232:Borromean
111:Ab initio
4354:Research
4260:Kepler's
4202:Remnants
4089:magnetar
4060:Remnants
3964:Imposter
3929:Kilonova
3714:Exchange
3651:-process
3643:-process
3615:Triple-α
3449:24 March
3425:23912055
3364:10525469
3211:31645733
3146:29094693
3085:29094694
2836:(1968),
2775:59020556
2606:process"
2587:29099225
2132:29094687
1857:See also
1847:GW170817
1796:> 140
1789:< 140
1762:> 140
1749:such as
1747:< 140
1732:GW170817
1598:-process
1188:chlorine
1176:hydrogen
1168:Big Bang
1050:-process
1009:kilonova
899:-process
873:-process
821:Category
722:Oliphant
707:Lawrence
687:Davisson
657:Chadwick
553:Big Bang
440:electron
410:Products
331:Isomeric
222:Even/odd
199: –
174:– equal
161:– equal
159:Isotones
148:– equal
134:– equal
132:Isotopes
124:Nuclides
46:Nucleons
4470:Neutron
4361:ASAS-SN
4255:Tycho's
4233:SN 1054
4216:Notable
4187:Notable
3897:Related
3774:Classes
3693:Capture
3580:Stellar
3403:Bibcode
3340:Bibcode
3293:Bibcode
3248:Bibcode
3183:Bibcode
3124:Bibcode
3063:Bibcode
3006:Bibcode
2953:Bibcode
2900:Bibcode
2808:Bibcode
2755:Bibcode
2679:Bibcode
2623:Bibcode
2565:Bibcode
2520:Bibcode
2449:Bibcode
2401:Bibcode
2352:Bibcode
2310:Bibcode
2271:Bibcode
2229:Bibcode
2174:Bibcode
2110:Bibcode
2048:Bibcode
1999:Bibcode
1774:thorium
1770:uranium
1645:fermium
1614:isobars
1473:below.
1279:Caltech
1104:History
1032:fermium
973:neutron
777:Thomson
767:Szilárd
737:Purcell
717:Meitner
652:N. Bohr
647:A. Bohr
632:Alvarez
548:Stellar
452:neutron
336:Gamma γ
189:Isomers
146:Isobars
41:Nucleus
4111:exotic
4084:pulsar
4029:yellow
3997:yellow
3904:Failed
3423:
3384:Nature
3362:
3284:Nature
3217:
3209:
3201:
3165:Nature
3144:
3105:Nature
3083:
3044:Nature
2987:Nature
2852:
2846:577–91
2773:
2697:
2585:
2370:
2130:
2091:Nature
2066:
1939:- and
1776:, and
1701:nuclei
1500:, and
1172:helium
1092:- and
901:. The
864:, the
819:
787:Wigner
782:Walton
772:Teller
702:Jensen
469:proton
212:Stable
4175:Lists
4116:quark
3670:Other
3502:decay
3393:arXiv
3215:S2CID
3173:arXiv
3114:arXiv
3053:arXiv
2996:arXiv
2943:arXiv
2771:S2CID
2745:arXiv
2722:(PDF)
2695:S2CID
2667:(PDF)
2642:(PDF)
2609:(PDF)
2555:arXiv
2368:S2CID
2217:(PDF)
2164:arXiv
2100:arXiv
2064:S2CID
1869:Notes
1635:like
1463:Virgo
1309:= 140
1302:= 140
1007:in a
954:rapid
943:= 196
936:= 130
752:Soddy
732:Proca
712:Mayer
692:Fermi
642:Bethe
217:Magic
4019:blue
3944:Nova
3451:2018
3421:PMID
3360:PMID
3207:PMID
3199:ISSN
3142:PMID
3081:PMID
2850:ISBN
2583:PMID
2477:See
2128:PMID
1791:and
1687:and
1643:and
1627:The
1461:and
1459:LIGO
1285:and
1217:and
1054:slow
1041:The
948:The
929:= 82
894:and
742:Rabi
697:Hahn
607:RHIC
227:Halo
4024:red
4002:Red
3411:doi
3389:500
3350:doi
3336:525
3301:doi
3289:340
3258:doi
3244:192
3191:doi
3169:574
3132:doi
3110:551
3071:doi
3049:551
3014:doi
2992:551
2961:doi
2939:420
2908:doi
2816:doi
2763:doi
2687:doi
2631:doi
2573:doi
2551:119
2459:doi
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2360:doi
2318:doi
2279:doi
2267:106
2237:doi
2182:doi
2118:doi
2096:551
2056:doi
2007:doi
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1196:amu
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860:In
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