2673:
558:
487:(those with periods on the order of decades) are rare. Astronomers theorize, however, that most, if not all, novae recur, albeit on time scales ranging from 1,000 to 100,000 years. The recurrence interval for a nova is less dependent on the accretion rate of the white dwarf than on its mass; with their powerful gravity, massive white dwarfs require less accretion to fuel an eruption than lower-mass ones. Consequently, the interval is shorter for high-mass white dwarfs.
256:
3643:
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4243:
4267:
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334:, quite small relative to the mass of the white dwarf. Furthermore, only five percent of the accreted mass is fused during the power outburst. Nonetheless, this is enough energy to accelerate nova ejecta to velocities as high as several thousand kilometers per second—higher for fast novae than slow ones—with a concurrent rise in
1091:
664:
from magnitude 10.5 to about 9.2 starting in
February 2015. A similar event had been reported in 1938, followed by another outburst in 1946. By June 2018, the star had dimmed slightly but still remained at an unusually high level of activity. In March or April 2023, it dimmed to magnitude 12.3. A
2154:
Patterson, Joseph; Kemp, Jonathan; Monard, Berto; Myers, Gordon; de Miguel, Enrique; Hambsch, Franz-Josef; Warhurst, Paul; Rea, Robert; Dvorak, Shawn; Menzies, Kenneth; Vanmunster, Tonny; Roberts, George; Campbell, Tut; Starkey, Donn; Ulowetz, Joseph; Rock, John; Seargeant, Jim; Boardman, James;
236:. In this work he argued that a nearby object should be seen to move relative to the fixed stars, and thus the nova had to be very far away. Although SN 1572 was later found to be a supernova and not a nova, the terms were considered interchangeable until the 1930s. After this, novae were called
316:
The rise to peak brightness may be very rapid, or gradual; after the peak, the brightness declines steadily. The time taken for a nova to decay by 2 or 3 magnitudes from maximum optical brightness is used for grouping novae into speed classes. Fast novae typically will take less than
429:
experiences roughly 25 to 75 novae per year. The number of novae actually observed in the Milky Way each year is much lower, about 10, probably because distant novae are obscured by gas and dust absorption. As of 2019, 407 probable novae had been recorded in the Milky Way. In the
154:
A recurrent nova involves the same processes as a classical nova, except that the nova event repeats in cycles of a few decades or less as the companion star again feeds the dense atmosphere of the white dwarf after each ignition, as in the star
349:
Potentially, a white dwarf can generate multiple novae over time as additional hydrogen continues to accrete onto its surface from its companion star. Where this repeated flaring is observed, the object is called a recurrent nova. An example is
147:. The sudden increase in energy expels the atmosphere into interstellar space, creating the envelope seen as visible light during the nova event. In past centuries such an event was thought to be a new star. A few novae produce short-lived
282:, leaving its remnant white dwarf core in orbit with the remaining star. The second star—which may be either a main-sequence star or an aging giant—begins to shed its envelope onto its white dwarf companion when it overflows its
1845:
Liimets, T.; Corradi, R.L.M.; Santander-García, M.; Villaver, E.; Rodríguez-Gil, P.; Verro, K.; Kolka, I. (2014). "A Dynamical Study of the Nova
Remnant of GK Persei / Stella Novae: Past and Future Decades.".
286:. As a result, the white dwarf steadily captures matter from the companion's outer atmosphere in an accretion disk, and in turn, the accreted matter falls into the atmosphere. As the white dwarf consists of
162:
Under certain conditions, mass accretion can eventually trigger runaway fusion that destroys the white dwarf rather than merely expelling its atmosphere. In this case, the event is usually classified as a
629:) is an object that has been seen to experience repeated nova eruptions. The recurrent nova typically brightens by about 9 magnitudes, whereas a classic nova may brighten by more than 12 magnitudes.
598:, with a main peak at magnitude −8.8, and a lesser one at −7.5. Novae also have roughly the same absolute magnitude 15 days after their peak (−5.5). Nova-based distance estimates to various nearby
109:, but causes of the dramatic appearance of a nova vary, depending on the circumstances of the two progenitor stars. The main sub-classes of novae are classical novae, recurrent novae (RNe), and
413:. The absence of hydrogen lines may be caused by the explosion of a helium shell on a white dwarf. The theory was first proposed in 1989, and the first candidate helium nova to be observed was
1805:
3618:
3007:
290:, the accreted hydrogen is unable to expand even though its temperature increases. Runaway fusion occurs when the temperature of this atmospheric layer reaches ~20 million
101:
that causes the sudden appearance of a bright, apparently "new" star (hence the name "nova", Latin for "new") that slowly fades over weeks or months. All observed novae involve
632:
Although it is estimated that as many as a quarter of nova systems experience multiple eruptions, only ten recurrent novae (listed below) have been observed in the Milky Way.
313:
reaction, liberating an enormous amount of energy. This blows the remaining gases away from the surface of the white dwarf and produces an extremely bright outburst of light.
444:
has shown that they are enriched in elements such as helium, carbon, nitrogen, oxygen, neon, and magnesium. Classical nova explosions are galactic producers of the element
3608:
3679:
493:
is unusual in that the time of its next eruption can be predicted fairly accurately; it is expected to recur in approximately 2083, plus or minus about 11 years.
3222:
305:, but for most binary system parameters, the hydrogen burning is thermally unstable and rapidly converts a large amount of the hydrogen into other, heavier
140:. This atmosphere, mostly consisting of hydrogen, is heated by the hot white dwarf and eventually reaches a critical temperature, causing ignition of rapid
120:
Classical nova eruptions are the most common type. This type is usually created in a close binary star system consisting of a white dwarf and either a
1606:
1585:
1110:
3202:
2810:
3318:
1900:
1735:
1386:
1357:
1253:
179:
354:, which is known to have flared seven times (in 1898, 1933, 1958, 1967, 1985, 2006, and 2021). Eventually, the white dwarf can explode as a
240:
to distinguish them from supernovae, as their causes and energies were thought to be different, based solely on the observational evidence.
2599:
3217:
434:, roughly 25 novae brighter than about 20th magnitude are discovered each year, and smaller numbers are seen in other nearby galaxies.
365:
Occasionally, novae are bright enough and close enough to Earth to be conspicuous to the unaided eye. The brightest recent example was
3672:
665:
similar dimming occurred in the year before the 1945 outburst, indicating that it will likely erupt between March and
September 2024.
301:
If the accretion rate is just right, hydrogen fusion may occur in a stable manner on the surface of the white dwarf, giving rise to a
67:
2206:
Rodríguez-Gil, Pablo; Corral-Santana, Jesús M; Elías-Rosa, N; Gänsicke, Boris T; Hernanz, Margarita; Sala, Gloria (20 October 2023).
4151:
3002:
2554:
3356:
3613:
3038:
1241:
548:: recurrent novae, where two or more eruptions separated by 80 years or less have been observed. These are generally also fast.
339:
2979:
1969:
Pagnotta, Ashley; Schaefer, Bradley E. (2014). "Identifying and
Quantifying Recurrent Novae Masquerading as Classical Novae".
3247:
2662:
186:, averaging about ten per year in the Milky Way. Most are found telescopically, perhaps only one every 12–18 months reaching
132:. If the orbital period of the system is a few days or less, the white dwarf is close enough to its companion star to draw
4114:
3969:
3800:
3665:
4233:
2563:
1828:"GCVS Variability Types and Distribution Statistics of Designated Variable Stars According to their Types of Variability"
1328:
4292:
3790:
3515:
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3237:
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3023:
2722:
1727:
792:
98:
3931:
3757:
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3242:
2750:
393:
was discovered 2 December 2013 and so far is the brightest nova of this millennium, reaching magnitude 3.3.
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4193:
3990:
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3033:
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1349:
221:
2572:
4022:
4014:
3964:
3823:
3810:
3601:
3505:
3311:
2707:
2632:
1879:
Robert, Gilmozzi; Della Valle, Massimo (2003). "Novae as
Distance Indicators". In Alloin, D.; Gieren, W. (eds.).
1667:
114:
4198:
3959:
3232:
3227:
2592:
1627:
406:
133:
71:
2672:
3995:
3849:
3828:
3532:
3252:
2657:
2647:
1245:
1161:
748:
636:
302:
2072:
4222:
3926:
3879:
3875:
3844:
3795:
3257:
3207:
3161:
2997:
2870:
2850:
1916:
Schaefer, Bradley E. (2010). "Comprehensive
Photometric Histories of All Known Galactic Recurrent Novae".
1141:
1131:
940:
644:
512:: fast novae, with a rapid brightness increase, followed by a brightness decline of 3 magnitudes—to about
370:
35:
31:
3285:
1196:
4070:
3854:
3762:
3646:
3565:
3409:
3048:
2702:
1663:"Carbon–Oxygen Classical Novae Are Galactic 7Li Producers as well as Potential Supernova Ia Progenitors"
717:
191:
39:
3101:
2022:
1751:
971:
4130:
3785:
3780:
3737:
3725:
3636:
3421:
3304:
2860:
2697:
2516:
2469:
2422:
2322:
2178:
2121:
1988:
1935:
1888:
1861:
1686:
1540:
1499:
1456:
1378:
1288:
595:
4000:
2882:
2497:
Massimo Della Valle; Luca Izzo (30 April 2020). "Observations of
Galactic and Extragalactic Novae".
1631:
1490:
Rosenbush, A. E. (17–21 September 2007). Klaus Werner; Thomas Rauch (eds.). "List of Helium Novae".
895:
4188:
4161:
3741:
3445:
3341:
3275:
2892:
2865:
2800:
2729:
2585:
1437:
Kato, Mariko; Hachisu, Izumi (December 2005). "V445 Puppis: Helium Nova on a
Massive White Dwarf".
648:
557:
449:
359:
1045:
4271:
4048:
3936:
3520:
3416:
3028:
2937:
2913:
2805:
2765:
2627:
2532:
2506:
2485:
2459:
2438:
2412:
2312:
2219:
2168:
2111:
2004:
1978:
1951:
1925:
1851:
1704:
1676:
1558:
1530:
1472:
1446:
1304:
1278:
1171:
1106:
1050:
976:
864:
787:
686:
661:
591:
390:
386:
378:
263:
156:
137:
712:
656:
1892:
1776:
317:
25 days to decay by 2 magnitudes, while slow novae will take more than 80 days.
4032:
3943:
3887:
3752:
3745:
3696:
3575:
3549:
3382:
3351:
3064:
2908:
2838:
2775:
2687:
2637:
2622:
2403:
Schaefer (2010). "Comprehensive
Photometric Histories of All Known Galactic Recurrent Novae".
1896:
1731:
1658:
1382:
1353:
1249:
1114:
753:
355:
287:
275:
164:
46:
4247:
4088:
4075:
3705:
3596:
2947:
2755:
2745:
2524:
2520:
2477:
2430:
2330:
2269:
2229:
2207:
2186:
2129:
1996:
1943:
1880:
1694:
1548:
1464:
1296:
1102:
1095:
900:
640:
431:
306:
2257:
338:
from a few times solar to 50,000–100,000 times solar. In 2010 scientists using NASA's
3898:
3732:
3450:
2855:
2760:
2567:
1827:
1801:
1332:
587:
310:
175:
141:
2473:
2426:
2326:
2182:
2125:
1992:
1939:
1865:
1690:
1544:
1503:
1460:
1292:
4287:
4183:
4081:
3892:
3716:
3500:
2887:
2843:
2817:
2450:
Shafter; et al. (2011). "A Spectroscopic and
Photometric Survey of Novae in M31".
603:
535:
195:
144:
129:
2434:
2000:
1947:
1553:
1518:
1269:
M.J. Darnley; et al. (10 February 2012). "On the Progenitors of Galactic Novae".
255:
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4135:
3818:
3688:
3539:
3483:
3455:
3361:
3091:
2536:
2489:
2481:
2442:
2335:
2300:
2008:
1955:
1881:
1708:
1562:
1308:
1300:
1176:
610:
410:
382:
320:
Despite its violence, usually the amount of material ejected in a nova is only about
271:
218:
121:
2099:
2045:
1476:
4259:
4042:
3905:
3570:
3544:
3527:
3478:
3428:
3394:
3346:
3069:
2969:
2942:
2920:
1011:
828:
569:
437:
402:
148:
2550:
2258:"Spectroscopy of the recurrent nova V3890 Sagittarii 18 d after the 1990 outburst"
178:
in Sagittarius; however, they can appear anywhere in the sky. They occur far more
505:
decay speed, referred to as either type A, B, C and R, or using the prefix "N":
243:
Although the term "stella nova" means "new star", novae most often take place on
4217:
4175:
3510:
3438:
3377:
3327:
3171:
3079:
2974:
2964:
2952:
2877:
2790:
1636:
1136:
859:
502:
484:
414:
366:
351:
244:
207:
106:
102:
2351:
2191:
2156:
2100:"A Theoretical Light-Curve Model for the Recurrent Nova V394 Coronae Australis"
1699:
1662:
4027:
3985:
3490:
3433:
3186:
3181:
3176:
3156:
2957:
2833:
2795:
2692:
2560:
2528:
2274:
1325:
1118:
680:
575:
490:
477:
335:
331:
283:
259:
110:
75:
17:
2234:
1581:
4062:
4056:
3495:
3166:
3146:
3141:
3136:
3131:
3086:
2780:
2717:
2712:
2642:
2608:
1602:
1410:
1166:
1156:
1146:
1006:
935:
823:
561:
538:, staying at maximum light for a decade or more and then fading very slowly.
528:: slow novae, with a brightness decline of 3 magnitudes in 150 days or more.
473:
426:
417:, in 2000. Since then, four other novae have been proposed as helium novae.
343:
295:
279:
211:
187:
183:
171:
58:
50:
1498:. Eberhard Karls University, Tübingen, Germany (published July 2008): 271.
66:
3404:
3151:
3116:
3111:
3106:
2930:
2770:
2301:"THE UBV COLOR EVOLUTION OF CLASSICAL NOVAE. II. COLOR–MAGNITUDE DIAGRAM"
2116:
1451:
1151:
125:
54:
1752:"Binary star V Sagittae to explode as very bright nova by century's end"
1090:
232:
for "concerning the new star"), giving rise to the adoption of the name
3126:
3096:
3074:
1632:"Class of stellar explosions found to be galactic producers of lithium"
1415:
607:
445:
441:
214:
4156:
3399:
3121:
2925:
599:
578:, material expelled in the nova explosion or in multiple explosions.
291:
606:
have been shown to be of comparable accuracy to those measured with
4254:
4212:
2511:
2317:
2224:
2173:
2133:
1681:
1535:
1468:
590:
measurements of distances. For instance, the distribution of their
2464:
2417:
2155:
Lemay, Damien; Cejudo, David; Knigge, Christian (1 January 2022).
1983:
1930:
1856:
1411:"Fermi detects 'shocking' surprise from supernova's little cousin"
1321:
1283:
1089:
556:
374:
369:. This nova appeared on 29 August 1975, in the constellation
254:
229:
65:
3657:
385:, which reached magnitude 3.7 on 17 February 2007, and
1832:
VizieR archive server, Strasbourg astronomical Data Center (CDS)
1406:
1197:"Nova Centauri 2013: Another bright, naked-eye nova | aavso.org"
3661:
3300:
2581:
3296:
1802:"Ritter Cataclysmic Binaries Catalog (7th Edition, Rev. 7.13)"
1402:
2577:
2208:"The orbital period of the recurrent nova V2487 Oph revealed"
194:
occur only a few times per century. The last bright nova was
381: 2.0 (nearly as bright as Deneb). The most recent were
1850:. ASP Conference Series. Vol. 490. pp. 109–115.
462:
as much material to the galaxy as do supernovae, and only
2157:"IM Normae: The Death Spiral of a Cataclysmic Variable?"
2073:"T Coronae Borealis nova event guide and how to prepare"
1806:
High Energy Astrophysics Science Archive Research Center
170:
Novae most often occur in the sky along the path of the
3619:
Timeline of white dwarfs, neutron stars, and supernovae
3008:
Timeline of white dwarfs, neutron stars, and supernovae
30:"Novas" and "Novae" redirect here. For other uses, see
1236:
Prialnik, Dina (2001). "Novae". In Paul Murdin (ed.).
1034:
1863, 1906, 1917, 1936, 1979, 1987, 1999, 2010, 2022,
136:
matter onto its surface, creating a dense but shallow
4231:
667:
1883:
Stellar Candles for the Extragalactic Distance Scale
4174:
4144:
4123:
4107:
4100:
4013:
3978:
3952:
3917:
3874:
3867:
3837:
3809:
3771:
3704:
3695:
3589:
3558:
3464:
3370:
3334:
3195:
3057:
3016:
2990:
2901:
2826:
2738:
2680:
2615:
198:, which reached 3.3 magnitude on 14 December 2013.
405:) is a proposed category of nova event that lacks
2561:AAVSO Variable Star of the Month. Novae: May 2001
2262:Monthly Notices of the Royal Astronomical Society
2212:Monthly Notices of the Royal Astronomical Society
2052:. American Association of Variable Star Observers
1777:"Overview: Long-term visual light curves | aavso"
651:, erupts as frequently as once every 12 months.
2098:Hachisu, Izumi; Kato, Mariko (September 2000).
884:1898, 1907, 1933, 1958, 1967, 1985, 2006, 2021
2294:
2292:
2044:Schaefer, B.E.; Kloppenborg, B.; Waagen, E.O.
421:Occurrence rate and astrophysical significance
3673:
3312:
2593:
2299:Hachisu, Izumi; Kato, Mariko (1 April 2016).
270:Evolution of potential novae begins with two
247:, which are remnants of extremely old stars.
70:Artist's conception of a white dwarf, right,
8:
3223:Monte Agliale Supernovae and Asteroid Survey
2025:. Sky & Telescope website. 20 April 2016
1576:
1574:
1572:
660:website reported a sustained brightening of
2405:The Astrophysical Journal Supplement Series
2305:The Astrophysical Journal Supplement Series
1918:The Astrophysical Journal Supplement Series
1597:
1595:
190:visibility. Novae reaching first or second
4104:
3871:
3701:
3680:
3666:
3658:
3632:
3319:
3305:
3297:
2600:
2586:
2578:
1238:Encyclopedia of Astronomy and Astrophysics
1109:+20) are discovered in M31 each year. The
1105:(M31); several dozen novae (brighter than
639:recurrent novae have been observed in the
2510:
2463:
2416:
2334:
2316:
2273:
2256:Anupama, G. C.; Sethi, S. (1 July 1994).
2233:
2223:
2190:
2172:
2115:
1982:
1929:
1855:
1698:
1680:
1607:Central Bureau for Astronomical Telegrams
1586:Central Bureau for Astronomical Telegrams
1552:
1534:
1450:
1282:
1111:Central Bureau for Astronomical Telegrams
274:stars in a binary system. One of the two
206:During the sixteenth century, astronomer
151:, lasting for perhaps several centuries.
4238:
1231:
1229:
1227:
1225:
1223:
1221:
1219:
1217:
1188:
27:Nuclear explosion in a white dwarf star
1848:Stellar Novae: Past and Future Decades
501:Novae are classified according to the
2638:Type II (IIP, IIL, IIn, and IIb)
1582:"CBAT List of Novae in the Milky Way"
342:discovered that a nova also can emit
294:, initiating nuclear burning via the
7:
3281:
647:. One of these extragalactic novae,
425:Astronomers have estimated that the
3218:Katzman Automatic Imaging Telescope
2046:"Announcing T CrB pre-eruption dip"
1101:Novae are relatively common in the
960:1890, 1902, 1920, 1944, 1967, 2011
586:Novae have some promise for use as
448:. The contribution of novae to the
87:
2354:. International Supernovae Network
1519:"The Galactic Nova Rate Revisited"
25:
2551:General Catalog of Variable Stars
2499:Astronomy and Astrophysics Review
2023:"Is T CrB About to Blow its Top?"
1113:(CBAT) has tracked novae in M31,
534:: very slow novae, also known as
483:Observed recurrent novae such as
4265:
4253:
4241:
4211:
3642:
3641:
3631:
3280:
3271:
3270:
3003:History of supernova observation
2671:
2555:Sternberg Astronomical Institute
2389:. American Institute of Physics.
1724:Horizons: Exploring the Universe
574:Some novae leave behind visible
452:is not great; novae supply only
113:. They are all considered to be
3614:White dwarf luminosity function
1242:Institute of Physics Publishing
1078:
1039:
1000:
965:
929:
889:
853:
817:
781:
742:
340:Fermi Gamma-ray Space Telescope
174:, especially near the observed
3248:SuperNova Early Warning System
2663:Common envelope jets supernova
2394:Bode, M.F.; Evans, E. (2008).
2385:Hernanz, M.; Josè, J. (2002).
2380:. North Holland Publishing Co.
1517:Shafter, A.W. (January 2017).
224:. He described it in his book
1:
3801:Blue large-amplitude pulsator
2398:. Cambridge University Press.
2376:Payne-Gaposchkin, C. (1957).
1661:; et al. (27 May 2020).
3238:Supernova/Acceleration Probe
3213:High-Z Supernova Search Team
2811:pulsational pair-instability
1728:Wadsworth Publishing Company
1324:Variable Star Of The Month:
707:Years since latest eruption
582:Novae as distance indicators
401:A helium nova (undergoing a
99:transient astronomical event
78:of its larger companion star
3581:Quasi-periodic oscillations
3357:Hertzsprung–Russell diagram
3243:Supernova Cosmology Project
2751:Fast blue optical transient
2435:10.1088/0067-0049/187/2/275
2001:10.1088/0004-637X/788/2/164
1948:10.1088/0067-0049/187/2/275
1603:"M31 (Apparent) Novae Page"
1554:10.3847/1538-4357/834/2/196
522:brightness—within 100 days.
440:observation of nova ejecta
4314:
3576:Electron-degenerate matter
2482:10.1088/0004-637X/734/1/12
2336:10.3847/0067-0049/223/2/21
1722:Seeds, Michael A. (1998).
1350:Cambridge University Press
1346:Cataclysmic Variable Stars
1301:10.1088/0004-637x/746/1/61
567:
251:Stellar evolution of novae
115:cataclysmic variable stars
44:
29:
4207:
3627:
3506:Cataclysmic variable star
3266:
2669:
2529:10.1007/s00159-020-0124-6
2452:The Astrophysical Journal
2387:Classical Nova Explosions
2161:The Astrophysical Journal
2104:The Astrophysical Journal
1971:The Astrophysical Journal
1668:The Astrophysical Journal
1523:The Astrophysical Journal
1439:The Astrophysical Journal
1271:The Astrophysical Journal
373:about 5 degrees north of
3228:Nearby Supernova Factory
2192:10.3847/1538-4357/abec87
1700:10.3847/1538-4357/ab8d23
1628:Arizona State University
1492:Hydrogen-Deficient Stars
1373:Zeilik, Michael (1993).
45:Not to be confused with
3850:Solar-like oscillations
3791:Slowly pulsating B-type
3533:Super soft X-ray source
3253:Supernova Legacy Survey
2566:6 November 2003 at the
2521:2020A&ARv..28....3D
2275:10.1093/mnras/269.1.105
1331:6 November 2003 at the
1246:Nature Publishing Group
1162:Superluminous supernova
812:1217, 1787, 1866, 1946
3927:Luminous blue variable
3758:Rapidly oscillating Ap
3258:Texas Supernova Search
3233:Sloan Supernova Survey
2851:Luminous blue variable
2235:10.1093/mnras/stad3124
1344:Warner, Brian (1995).
1248:. pp. 1846–1856.
1142:Guest star (astronomy)
1132:Cosmic distance ladder
1098:
749:V394 Coronae Australis
654:On 20 April 2016, the
645:Large Magellanic Cloud
565:
356:Type Ia supernova
303:supersoft X-ray source
267:
79:
36:Novae (disambiguation)
32:Novas (disambiguation)
2703:Phillips relationship
2352:"Extragalactic Novae"
2077:Sky at Night Magazine
1379:John Wiley & Sons
1093:
701:Known eruption years
560:
358:if it approaches the
258:
69:
40:Nova (disambiguation)
4115:Rotating ellipsoidal
4023:AM Canum Venaticorum
3970:RS Canum Venaticorum
1375:Conceptual Astronomy
346:(>100 MeV).
4293:Astronomical events
4152:α Canum Venaticorum
3446:Extreme helium star
3342:Chandrasekhar limit
3276:Category:Supernovae
3208:Calán/Tololo Survey
2893:Population III star
2801:Soft gamma repeater
2633:Type Ib and Ic
2573:Extragalactic Novae
2474:2011ApJ...734...12S
2427:2010ApJS..187..275S
2327:2016ApJS..223...21H
2183:2022ApJ...924...27P
2126:2000ApJ...540..447H
1993:2014ApJ...788..164P
1940:2010ApJS..187..275S
1866:2014ASPC..490..109L
1691:2020ApJ...895...70S
1545:2017ApJ...834..196S
1504:2008ASPC..391..271R
1461:2003ApJ...598L.107K
1293:2012ApJ...746...61D
1086:Extragalactic novae
657:Sky & Telescope
450:interstellar medium
360:Chandrasekhar limit
4136:FK Comae Berenices
3932:R Coronae Borealis
3722:Classical cepheids
3521:Intermediate polar
3417:Stellar black hole
3286:Commons:Supernovae
2938:Stellar black hole
2914:Pulsar wind nebula
2766:Gravitational wave
2378:The Galactic Novae
1659:Starrfield, Sumner
1409:(12 August 2010).
1172:Supernova impostor
1107:apparent magnitude
1099:
788:T Coronae Borealis
662:T Coronae Borealis
592:absolute magnitude
566:
391:Nova Centauri 2013
387:Nova Delphini 2013
268:
264:apparent magnitude
157:T Coronae Borealis
80:
74:hydrogen from the
4298:Stellar phenomena
4229:
4228:
4194:Planetary transit
4170:
4169:
4091:
4084:
4065:
4051:
4033:Luminous red nova
4009:
4008:
3991:Gamma Cassiopeiae
3944:Yellow hypergiant
3940:
3908:
3901:
3863:
3862:
3749:
3729:
3655:
3654:
3550:Carbon detonation
3383:Type Ia supernova
3352:Stellar evolution
3294:
3293:
2909:Supernova remnant
2776:Luminous red nova
2688:Carbon detonation
1902:978-3-540-20128-1
1737:978-0-534-52434-0
1388:978-0-471-50996-7
1359:978-0-521-41231-5
1255:978-1-56159-268-5
1083:
1082:
1073:1937, 1989, 2014
995:1962, 1990, 2019
737:1917, 1941, 2000
704:Interval (years)
307:chemical elements
288:degenerate matter
260:Nova Eridani 2009
165:Type Ia supernova
47:luminous red nova
16:(Redirected from
4305:
4270:
4269:
4268:
4258:
4257:
4246:
4245:
4244:
4237:
4216:
4215:
4105:
4087:
4080:
4061:
4047:
3965:FS Canis Majoris
3934:
3904:
3897:
3872:
3735:
3719:
3702:
3682:
3675:
3668:
3659:
3645:
3644:
3635:
3634:
3597:Planetary nebula
3321:
3314:
3307:
3298:
3284:
3283:
3274:
3273:
3137:Remnant G1.9+0.3
2756:Fast radio burst
2675:
2653:Pair-instability
2602:
2595:
2588:
2579:
2540:
2514:
2493:
2467:
2446:
2420:
2399:
2390:
2381:
2364:
2363:
2361:
2359:
2347:
2341:
2340:
2338:
2320:
2296:
2287:
2286:
2284:
2282:
2277:
2253:
2247:
2246:
2244:
2242:
2237:
2227:
2218:(4): 4961–4975.
2203:
2197:
2196:
2194:
2176:
2151:
2145:
2144:
2142:
2140:
2119:
2117:astro-ph/0003471
2095:
2089:
2088:
2086:
2084:
2068:
2062:
2061:
2059:
2057:
2041:
2035:
2034:
2032:
2030:
2019:
2013:
2012:
1986:
1966:
1960:
1959:
1933:
1913:
1907:
1906:
1886:
1876:
1870:
1869:
1859:
1842:
1836:
1835:
1824:
1818:
1817:
1815:
1813:
1798:
1792:
1791:
1789:
1787:
1773:
1767:
1766:
1764:
1762:
1748:
1742:
1741:
1726:(5th ed.).
1719:
1713:
1712:
1702:
1684:
1655:
1649:
1648:
1646:
1644:
1624:
1618:
1617:
1615:
1613:
1599:
1590:
1589:
1578:
1567:
1566:
1556:
1538:
1514:
1508:
1507:
1487:
1481:
1480:
1454:
1452:astro-ph/0310351
1445:(2): L107–L110.
1434:
1428:
1427:
1425:
1423:
1399:
1393:
1392:
1370:
1364:
1363:
1341:
1335:
1319:
1313:
1312:
1286:
1266:
1260:
1259:
1233:
1212:
1211:
1209:
1207:
1193:
1103:Andromeda Galaxy
1096:Andromeda Galaxy
1064:
1062:
1059:
1025:
1023:
1020:
986:
985:
972:V3890 Sagittarii
951:
949:
915:
913:
910:
875:
873:
839:
837:
803:
801:
767:
765:
762:
728:
726:
668:
641:Andromeda Galaxy
521:
520:
516:
471:
470:
466:
461:
460:
456:
432:Andromeda Galaxy
329:
328:
324:
89:
21:
4313:
4312:
4308:
4307:
4306:
4304:
4303:
4302:
4278:
4277:
4276:
4266:
4264:
4252:
4242:
4240:
4232:
4230:
4225:
4218:Star portal
4210:
4203:
4199:W Ursae Majoris
4166:
4145:Magnetic fields
4140:
4119:
4096:
4005:
3974:
3960:Double periodic
3953:Eruptive binary
3948:
3919:
3913:
3859:
3833:
3805:
3773:
3772:Blue-white with
3767:
3709:
3691:
3686:
3656:
3651:
3623:
3585:
3554:
3466:
3460:
3451:Subdwarf B star
3366:
3330:
3325:
3295:
3290:
3262:
3191:
3177:SN 2016aps
3157:SN Refsdal
3053:
3012:
2986:
2897:
2883:Wolf–Rayet star
2822:
2761:Gamma-ray burst
2734:
2708:Nucleosynthesis
2676:
2667:
2611:
2606:
2568:Wayback Machine
2547:
2496:
2449:
2402:
2396:Classical Novae
2393:
2384:
2375:
2372:
2370:Further reading
2367:
2357:
2355:
2350:Bishop, David.
2349:
2348:
2344:
2298:
2297:
2290:
2280:
2278:
2255:
2254:
2250:
2240:
2238:
2205:
2204:
2200:
2153:
2152:
2148:
2138:
2136:
2097:
2096:
2092:
2082:
2080:
2070:
2069:
2065:
2055:
2053:
2043:
2042:
2038:
2028:
2026:
2021:
2020:
2016:
1968:
1967:
1963:
1915:
1914:
1910:
1903:
1878:
1877:
1873:
1844:
1843:
1839:
1826:
1825:
1821:
1811:
1809:
1808:. 31 March 2010
1800:
1799:
1795:
1785:
1783:
1775:
1774:
1770:
1760:
1758:
1750:
1749:
1745:
1738:
1730:. p. 194.
1721:
1720:
1716:
1657:
1656:
1652:
1642:
1640:
1630:(1 June 2020).
1626:
1625:
1621:
1611:
1609:
1601:
1600:
1593:
1580:
1579:
1570:
1516:
1515:
1511:
1489:
1488:
1484:
1436:
1435:
1431:
1421:
1419:
1401:
1400:
1396:
1389:
1372:
1371:
1367:
1360:
1343:
1342:
1338:
1333:Wayback Machine
1326:May 2001: Novae
1320:
1316:
1268:
1267:
1263:
1256:
1235:
1234:
1215:
1205:
1203:
1195:
1194:
1190:
1186:
1181:
1127:
1088:
1060:
1057:
1055:
1021:
1018:
1016:
983:
981:
947:
945:
911:
908:
906:
871:
869:
835:
833:
799:
797:
763:
760:
758:
724:
722:
697:
695:
691:
689:
676:
672:
619:
617:Recurrent novae
604:galaxy clusters
588:standard candle
584:
572:
555:
536:symbiotic novae
518:
514:
513:
499:
468:
464:
463:
458:
454:
453:
423:
399:
367:Nova Cygni 1975
326:
322:
321:
253:
238:classical novae
204:
176:Galactic Center
62:
43:
28:
23:
22:
15:
12:
11:
5:
4311:
4309:
4301:
4300:
4295:
4290:
4280:
4279:
4275:
4274:
4262:
4250:
4227:
4226:
4208:
4205:
4204:
4202:
4201:
4196:
4191:
4186:
4180:
4178:
4172:
4171:
4168:
4167:
4165:
4164:
4159:
4154:
4148:
4146:
4142:
4141:
4139:
4138:
4133:
4127:
4125:
4121:
4120:
4118:
4117:
4111:
4109:
4102:
4098:
4097:
4095:
4094:
4093:
4092:
4085:
4082:Symbiotic nova
4073:
4068:
4067:
4066:
4054:
4053:
4052:
4040:
4035:
4030:
4025:
4019:
4017:
4011:
4010:
4007:
4006:
4004:
4003:
3998:
3996:Lambda Eridani
3993:
3988:
3982:
3980:
3976:
3975:
3973:
3972:
3967:
3962:
3956:
3954:
3950:
3949:
3947:
3946:
3941:
3929:
3923:
3921:
3915:
3914:
3912:
3911:
3910:
3909:
3902:
3890:
3884:
3882:
3869:
3865:
3864:
3861:
3860:
3858:
3857:
3852:
3847:
3841:
3839:
3835:
3834:
3832:
3831:
3829:Slow irregular
3826:
3821:
3815:
3813:
3807:
3806:
3804:
3803:
3798:
3793:
3788:
3783:
3777:
3775:
3769:
3768:
3766:
3765:
3760:
3755:
3750:
3730:
3713:
3711:
3699:
3693:
3692:
3689:Variable stars
3687:
3685:
3684:
3677:
3670:
3662:
3653:
3652:
3650:
3649:
3639:
3628:
3625:
3624:
3622:
3621:
3616:
3611:
3606:
3605:
3604:
3593:
3591:
3587:
3586:
3584:
3583:
3578:
3573:
3568:
3562:
3560:
3556:
3555:
3553:
3552:
3547:
3542:
3537:
3536:
3535:
3525:
3524:
3523:
3518:
3513:
3503:
3501:Symbiotic nova
3498:
3493:
3488:
3487:
3486:
3481:
3470:
3468:
3462:
3461:
3459:
3458:
3453:
3448:
3443:
3442:
3441:
3436:
3426:
3425:
3424:
3414:
3413:
3412:
3407:
3402:
3392:
3391:
3390:
3380:
3374:
3372:
3368:
3367:
3365:
3364:
3359:
3354:
3349:
3344:
3338:
3336:
3332:
3331:
3326:
3324:
3323:
3316:
3309:
3301:
3292:
3291:
3289:
3288:
3278:
3267:
3264:
3263:
3261:
3260:
3255:
3250:
3245:
3240:
3235:
3230:
3225:
3220:
3215:
3210:
3205:
3199:
3197:
3193:
3192:
3190:
3189:
3184:
3179:
3174:
3169:
3167:SN 2006gy
3164:
3159:
3154:
3149:
3147:SN 2011fe
3144:
3142:SN 2007bi
3139:
3134:
3132:SN 2003fg
3129:
3124:
3119:
3114:
3109:
3104:
3099:
3094:
3089:
3084:
3083:
3082:
3072:
3067:
3065:Barnard's Loop
3061:
3059:
3055:
3054:
3052:
3051:
3046:
3041:
3036:
3031:
3026:
3020:
3018:
3014:
3013:
3011:
3010:
3005:
3000:
2994:
2992:
2988:
2987:
2985:
2984:
2983:
2982:
2980:Orion–Eridanus
2972:
2967:
2962:
2961:
2960:
2955:
2950:
2940:
2935:
2934:
2933:
2928:
2918:
2917:
2916:
2905:
2903:
2899:
2898:
2896:
2895:
2890:
2888:Super-AGB star
2885:
2880:
2875:
2874:
2873:
2868:
2863:
2853:
2848:
2847:
2846:
2841:
2830:
2828:
2824:
2823:
2821:
2820:
2818:Symbiotic nova
2815:
2814:
2813:
2803:
2798:
2793:
2788:
2783:
2778:
2773:
2768:
2763:
2758:
2753:
2748:
2742:
2740:
2736:
2735:
2733:
2732:
2727:
2726:
2725:
2720:
2715:
2705:
2700:
2695:
2690:
2684:
2682:
2678:
2677:
2670:
2668:
2666:
2665:
2660:
2655:
2650:
2645:
2640:
2635:
2630:
2625:
2619:
2617:
2613:
2612:
2607:
2605:
2604:
2597:
2590:
2582:
2576:
2575:
2570:
2558:
2546:
2545:External links
2543:
2542:
2541:
2494:
2447:
2411:(2): 275–373.
2400:
2391:
2382:
2371:
2368:
2366:
2365:
2342:
2288:
2268:(1): 105–109.
2248:
2198:
2146:
2134:10.1086/309338
2110:(1): 447–451.
2090:
2063:
2036:
2014:
1961:
1924:(2): 275–373.
1908:
1901:
1871:
1837:
1819:
1793:
1768:
1743:
1736:
1714:
1650:
1619:
1591:
1568:
1529:(2): 192–203.
1509:
1482:
1469:10.1086/380597
1429:
1394:
1387:
1365:
1358:
1336:
1314:
1261:
1254:
1213:
1187:
1185:
1182:
1180:
1179:
1174:
1169:
1164:
1159:
1154:
1149:
1144:
1139:
1134:
1128:
1126:
1123:
1087:
1084:
1081:
1080:
1077:
1074:
1071:
1068:
1065:
1053:
1048:
1042:
1041:
1038:
1035:
1032:
1029:
1026:
1014:
1009:
1003:
1002:
999:
996:
993:
990:
987:
979:
974:
968:
967:
964:
961:
958:
955:
952:
943:
938:
932:
931:
928:
925:
922:
919:
916:
904:
898:
896:V2487 Ophiuchi
892:
891:
888:
885:
882:
879:
876:
867:
862:
856:
855:
852:
849:
846:
843:
840:
831:
826:
820:
819:
816:
813:
810:
807:
804:
795:
790:
784:
783:
780:
777:
774:
771:
768:
756:
751:
745:
744:
741:
738:
735:
732:
729:
720:
715:
709:
708:
705:
702:
699:
692:
684:
677:
673:
643:(M31) and the
623:recurrent nova
618:
615:
611:variable stars
583:
580:
568:Main article:
564:: Nova of 1901
554:
551:
550:
549:
539:
529:
523:
498:
495:
422:
419:
407:hydrogen lines
398:
395:
377:, and reached
252:
249:
226:De nova stella
203:
200:
196:V1369 Centauri
182:than galactic
130:red giant star
107:binary systems
26:
24:
18:Recurrent nova
14:
13:
10:
9:
6:
4:
3:
2:
4310:
4299:
4296:
4294:
4291:
4289:
4286:
4285:
4283:
4273:
4263:
4261:
4256:
4251:
4249:
4239:
4235:
4224:
4220:
4219:
4214:
4206:
4200:
4197:
4195:
4192:
4190:
4187:
4185:
4182:
4181:
4179:
4177:
4173:
4163:
4160:
4158:
4155:
4153:
4150:
4149:
4147:
4143:
4137:
4134:
4132:
4129:
4128:
4126:
4124:Stellar spots
4122:
4116:
4113:
4112:
4110:
4108:Non-spherical
4106:
4103:
4099:
4090:
4086:
4083:
4079:
4078:
4077:
4074:
4072:
4069:
4064:
4060:
4059:
4058:
4055:
4050:
4046:
4045:
4044:
4041:
4039:
4036:
4034:
4031:
4029:
4026:
4024:
4021:
4020:
4018:
4016:
4012:
4002:
3999:
3997:
3994:
3992:
3989:
3987:
3984:
3983:
3981:
3977:
3971:
3968:
3966:
3963:
3961:
3958:
3957:
3955:
3951:
3945:
3942:
3938:
3933:
3930:
3928:
3925:
3924:
3922:
3916:
3907:
3903:
3900:
3896:
3895:
3894:
3891:
3889:
3886:
3885:
3883:
3881:
3877:
3873:
3870:
3866:
3856:
3853:
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3845:Gamma Doradus
3843:
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3796:PV Telescopii
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3774:early spectra
3770:
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3540:Binary pulsar
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3456:Helium planet
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3408:
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3117:SN 1994D
3115:
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3112:SN 1987A
3110:
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3107:SN 1885A
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1201:www.aavso.org
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1177:X-ray burster
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901:K. Takamizawa
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649:M31N 2008-12a
646:
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637:extragalactic
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438:Spectroscopic
435:
433:
428:
420:
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416:
412:
408:
404:
396:
394:
392:
388:
384:
383:V1280 Scorpii
380:
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368:
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333:
318:
314:
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281:
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273:
272:main sequence
265:
261:
257:
250:
248:
246:
241:
239:
235:
231:
227:
223:
220:
219:constellation
216:
213:
210:observed the
209:
201:
199:
197:
193:
189:
185:
181:
177:
173:
168:
166:
160:
158:
152:
150:
149:nova remnants
146:
143:
139:
135:
131:
127:
123:
122:main sequence
118:
116:
112:
108:
104:
100:
96:
92:
85:
77:
73:
68:
64:
60:
56:
52:
48:
41:
37:
33:
19:
4209:
4089:Z Andromedae
4071:SW Sextantis
4049:Intermediate
4037:
3888:Herbig Ae/Be
3763:SX Phoenicis
3710:cepheid-like
3571:Urca process
3545:Helium flash
3528:X-ray binary
3473:
3429:Compact star
3395:Neutron star
3347:PG 1159 star
3162:Vela Remnant
3127:SN 1006
3092:SN 1000+0216
3070:Cassiopeia A
3039:Most distant
2970:Local Bubble
2943:Compact star
2921:Neutron star
2785:
2658:Calcium-rich
2623:Type Ia
2502:
2498:
2455:
2451:
2408:
2404:
2395:
2386:
2377:
2358:11 September
2356:. Retrieved
2345:
2308:
2304:
2279:. Retrieved
2265:
2261:
2251:
2239:. Retrieved
2215:
2211:
2201:
2164:
2160:
2149:
2137:. Retrieved
2107:
2103:
2093:
2081:. Retrieved
2076:
2066:
2054:. Retrieved
2049:
2039:
2027:. Retrieved
2017:
1974:
1970:
1964:
1921:
1917:
1911:
1882:
1874:
1847:
1840:
1831:
1822:
1812:25 September
1810:. Retrieved
1796:
1784:. Retrieved
1780:
1771:
1759:. Retrieved
1755:
1746:
1723:
1717:
1672:
1666:
1653:
1641:. Retrieved
1635:
1622:
1610:. Retrieved
1526:
1522:
1512:
1495:
1491:
1485:
1442:
1438:
1432:
1420:. Retrieved
1414:
1397:
1374:
1368:
1345:
1339:
1317:
1274:
1270:
1264:
1237:
1204:. Retrieved
1200:
1191:
1100:
1046:V745 Scorpii
1012:N. R. Pogson
696:3 magnitudes
694:Days to drop
655:
653:
634:
631:
626:
622:
620:
585:
573:
570:Nova remnant
545:
541:
531:
525:
509:
500:
489:
482:
436:
424:
403:helium flash
400:
397:Helium novae
364:
348:
319:
315:
300:
269:
245:white dwarfs
242:
237:
233:
225:
205:
169:
161:
153:
119:
103:white dwarfs
94:
90:
83:
81:
63:
4272:Outer space
4131:BY Draconis
4015:Cataclysmic
3920:supergiants
3855:White dwarf
3824:Semiregular
3811:Long-period
3786:Beta Cephei
3781:Alpha Cygni
3738:BL Herculis
3726:Delta Scuti
3511:AM CVn star
3439:Exotic star
3378:Black dwarf
3328:White dwarf
3172:ASASSN-15lh
3122:SN 185
3080:Crab Nebula
2975:Superbubble
2965:Zombie star
2948:electroweak
2878:White dwarf
2827:Progenitors
2791:Pulsar kick
2071:Todd, Ian.
1891:. pp.
1637:EurekAlert!
1612:24 February
1137:Crab Nebula
924:1900, 1998
860:RS Ophiuchi
848:1920, 2002
829:I. E. Woods
776:1949, 1987
718:K. Reinmuth
503:light curve
485:RS Ophiuchi
472:as much as
415:V445 Puppis
352:RS Ophiuchi
208:Tycho Brahe
111:dwarf novae
4282:Categories
4189:Beta Lyrae
4162:SX Arietis
4028:Dwarf nova
4001:Wolf–Rayet
3918:Giants and
3899:FU Orionis
3742:W Virginis
3559:Properties
3491:Dwarf nova
3434:Quark star
3388:Candidates
3187:SN 2022jli
3182:SN 2018cow
3049:In fiction
3024:Candidates
2998:Guest star
2856:Supergiant
2834:Hypergiant
2796:Quark-nova
2698:Near-Earth
2681:Physics of
2609:Supernovae
2512:2004.06540
2318:1602.01195
2225:2310.05877
2174:2010.07812
2056:18 January
1977:(2): 164.
1761:20 January
1682:1910.00575
1536:1606.02358
1277:(61): 61.
1206:2 November
1184:References
941:H. Leavitt
865:W. Fleming
754:L. E. Erro
713:CI Aquilae
698:from peak
679:Distance (
675:Discoverer
576:nebulosity
491:V Sagittae
478:supergiant
344:gamma rays
336:luminosity
332:solar mass
284:Roche lobe
222:Cassiopeia
184:supernovae
180:frequently
138:atmosphere
76:Roche lobe
4248:Astronomy
4176:Eclipsing
4076:Symbiotic
4063:Hypernova
4057:Supernova
3937:DY Persei
3876:Protostar
3697:Pulsating
3566:Pulsating
3496:Micronova
3465:In binary
3335:Formation
3087:iPTF14hls
2991:Discovery
2781:Micronova
2730:Neutrinos
2723:γ-process
2718:r-process
2713:p-process
2693:Foe/Bethe
2643:Hypernova
2537:215754507
2490:119114867
2465:1104.0222
2458:(1): 12.
2443:119294221
2418:0912.4426
2311:(2): 21.
2167:(1): 27.
2009:118448146
1984:1405.0246
1956:119294221
1931:0912.4426
1857:1310.4488
1709:203610207
1675:(1): 70.
1563:118652484
1422:15 August
1309:119291027
1284:1112.2589
1167:Supernova
1157:Micronova
1147:Hypernova
1067:9.4–19.3
1028:7.5–17.6
1007:U Scorpii
989:8.1–18.4
954:6.4–15.5
936:T Pyxidis
918:9.5–17.5
842:8.5–18.5
824:IM Normae
806:2.5–10.8
770:7.2–19.7
731:8.6–16.3
687:Magnitude
671:Full name
562:GK Persei
474:red giant
427:Milky Way
379:magnitude
296:CNO cycle
280:red giant
212:supernova
202:Etymology
192:magnitude
188:naked-eye
172:Milky Way
105:in close
72:accreting
59:micronova
51:supernova
4101:Rotating
3868:Eruptive
3753:RR Lyrae
3746:RV Tauri
3706:Cepheids
3647:Category
3405:Magnetar
3196:Research
3102:Kepler's
3044:Remnants
2931:magnetar
2902:Remnants
2806:Imposter
2771:Kilonova
2564:Archived
2557:, Moscow
2505:(1): 3.
2083:18 March
2029:6 August
1889:Springer
1756:phys.org
1477:17055772
1329:Archived
1152:Kilonova
1125:See also
1094:Nova in
1051:L. Plaut
635:Several
600:galaxies
553:Remnants
497:Subtypes
411:spectrum
134:accreted
126:subgiant
55:kilonova
4234:Portals
3906:T Tauri
3733:Type II
3590:Related
3479:Remnant
3467:systems
3203:ASAS-SN
3097:Tycho's
3075:SN 1054
3058:Notable
3029:Notable
2739:Related
2616:Classes
2517:Bibcode
2470:Bibcode
2423:Bibcode
2323:Bibcode
2179:Bibcode
2122:Bibcode
1989:Bibcode
1936:Bibcode
1862:Bibcode
1786:14 July
1687:Bibcode
1541:Bibcode
1500:Bibcode
1457:Bibcode
1416:PhysOrg
1289:Bibcode
903:(1998)
878:4.8–11
608:Cepheid
596:bimodal
517:⁄
480:stars.
467:⁄
457:⁄
446:lithium
442:nebulae
409:in its
325:⁄
311:runaway
278:into a
276:evolves
217:in the
215:SN 1572
142:runaway
97:) is a
4157:Pulsar
3717:Type I
3609:RAMBOs
3400:Pulsar
2953:exotic
2926:pulsar
2871:yellow
2839:yellow
2746:Failed
2535:
2488:
2441:
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