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supernova
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{{short description|Star exploding at the end of its stellar lifespan}}{{Other uses}}
missing image!
- SN1994D.jpg -
right|upright=1.2|SN 1994D (bright spot on the lower left), a Type Ia supernova outshining its home galaxy, NGC 4526
A supernova ({{IPAc-en||ˌ|s|uː|p|ɚ|n|oʊ|v|ə}} plural: supernovae {{IPAc-en|ˌ|s|uː|p|ɚ|n|oʊ|v|iː}} or supernovas, abbreviations: SN and SNe) is an event that occurs upon the death of certain types of stars.Supernovae are more energetic than novae. In Latin, nova means "new", referring astronomically to what appears to be a temporary new bright star. Adding the prefix "super-" distinguishes supernovae from ordinary novae, which are far less luminous. The word supernova was coined by Walter Baade and Fritz Zwicky in 1931.Only three, Milky Way naked-eye supernova events have been observed during the last thousand years, though many have been seen in other galaxies using telescopes. The most recent directly observed supernova in the Milky Way was Kepler's Supernova in 1604, but two more recent supernova remnants have also been found. Statistical observations of supernovae in other galaxies suggest they occur on average about three times every century in the Milky Way, and that any galactic supernova would almost certainly be observable with modern astronomical telescopes.Supernovae may expel much, if not all, of the material away from a star at velocities up to {{val|30000|fmt=commas|u=km/s}} or 10% of the speed of light. This drives an expanding and fast-moving shock waveJOURNAL
, Schawinski, K.
, Justham, S.
, Wolf, C.
, Podsiadlowski, P.
, Sullivan, M.
, Steenbrugge, K. C.
, Bell, T.
, Röser, H.-J.
, Walker, E. S.
, Astier, P.
, Balam, D.
, Balland, C.
, Carlberg, R. G.
, Conley, A. J.
, Fouchez, D.
, Guy, J.
, Hardin, D.
, Hook, I. M.
, Howell, D. A.
, Pain, R.
, Perrett, K. M.
, Pritchet, C. J.
, Regnault, N.
, Yi, S. K.
, 1
, 2008
, Supernova Shock Breakout from a Red Supergiant
, Science (journal), Science
, 321, 5886, 223–226
, 0803.3596
, 2008Sci...321..223S
, 10.1126/science.1160456
, 18556514
, into the surrounding interstellar medium, and in turn, sweeping up an expanding shell of gas and dust, which is observed as a supernova remnant. Supernovae create, fuse and eject the bulk of the chemical elements produced by nucleosynthesis.JOURNAL
, Timmes, F. X.
, Woosley, S. E.
, Weaver, T. A.
, 1995
, Galactic chemical evolution: Hydrogen through zinc
, Astrophysical Journal Supplement Series
, 98, 617
, astro-ph/9411003
, 1995ApJS...98..617T
, 10.1086/192172
, Supernovae play a significant role in enriching the interstellar medium with the heavier atomic mass chemical elements.BOOK
, Whittet, D. C. B.
, 2003
, Dust in the Galactic Environment
, 45–46
, CRC Press
, 978-0-7503-0624-9
, Furthermore, the expanding shock waves from supernovae can trigger the formation of new stars.JOURNAL
, Boss, A. P.
, Ipatov, S. I.
, Keiser, S. A.
, Myhill, E. A.
, Vanhala, H. A. T.
, 2008
, Simultaneous Triggered Collapse of the Presolar Dense Cloud Core and Injection of Short-Lived Radioisotopes by a Supernova Shock Wave
, The Astrophysical Journal Letters
, 686, 2, L119–L122
, 0809.3045
, 2008ApJ...686L.119B
, 10.1086/593057
, Supernova remnants are expected to accelerate a large fraction of galactic primary cosmic rays, but direct evidence for cosmic ray production was found only in a few of them so far.JOURNAL
, Ackermann, M.
, Ajello, M.
, Allafort, A.
, Baldini, L.
, Ballet, J.
, Barbiellini, G.
, Baring, M. G.
, Bastieri, D.
, Bechtol, K.
, Bellazzini, R.
, Blandford, R. D.
, Bloom, E. D.
, Bonamente, E.
, Borgland, A. W.
, Bottacini, E.
, Brandt, T. J.
, Bregeon, J.
, Brigida, M.
, Bruel, P.
, Buehler, R.
, Busetto, G.
, Buson, S.
, Caliandro, G. A.
, Cameron, R. A.
, Caraveo, P. A.
, Casandjian, J. M.
, Cecchi, C.
, Celik, O.
, Charles, E.
, Chaty, S.
, 1
, Detection of the Characteristic Pion-Decay Signature in Supernova Remnants
, Science (journal), Science
, 339, 6121, 807–11
, 2013
, 1302.3307
, 2013Sci...339..807A
, 10.1126/science.1231160
, 23413352
, They are also potentially strong galactic sources of gravitational waves.JOURNAL
, Ott, C. D.
, O'Connor, E. P.
, Gossan, S. E.
, Abdikamalov, E.
, Gamma, U. C. T.
, Drasco, S.
, 1
, 2012
, Core-Collapse Supernovae, Neutrinos, and Gravitational Waves
, (Nuclear Physics B: Proceedings Supplements)
, 235, 381–387
, 1212.4250
, 2013NuPhS.235..381O
, 10.1016/j.nuclphysbps.2013.04.036
, Theoretical studies indicate that most supernovae are triggered by one of two basic mechanisms: the sudden re-ignition of nuclear fusion in a degenerate star or the sudden gravitational collapse of a massive star's core. In the first instance, a degenerate white dwarf may accumulate sufficient material from a binary companion, either through accretion or via a merger, to raise its core temperature enough to trigger runaway nuclear fusion, completely disrupting the star. In the second case, the core of a massive star may undergo sudden gravitational collapse, releasing gravitational potential energy as a supernova. While some observed supernovae are more complex than these two simplified theories, the astrophysical collapse mechanics have been established and accepted by most astronomers for some time.Due to the wide range of astrophysical consequences of these events, astronomers now deem supernova research, across the fields of stellar and galactic evolution, as an especially important area for investigation.

Observation history

{{multiple image
|align=right
|direction=vertical
|width=200
|image1=Crab Nebula.jpg
|alt1=
|caption1=The Crab Nebula is a pulsar wind nebula associated with the 1054 supernova
|image2=Chinese report of guest star identified as the supernova of 1054 (SN 1054) in the Lidai mingchen zouyi (历代名臣奏议).jpg
|alt2=
|caption2=The highlighted passages refer to the Chinese observation of SN 1054
}}The earliest recorded supernova, SN 185, was viewed by Chinese astronomers in 185 AD. The brightest recorded supernova was SN 1006, which occurred in 1006 AD and was described by observers across China, Japan, Iraq, Egypt, and Europe.BOOK, Murdin, Paul, Murdin, Lesley, Supernovae, Cambridge University Press,weblink 1985, 978-0521300384, 14–16, BOOK, Burnham, Robert Jr., Robert Burnham Jr., The Celestial handbook, Dover, 1978, 1117–1122, Celestial handbook, JOURNAL
, Winkler, P. F.
, Gupta, G.
, Long, K. S.
, 2003
, The SN 1006 Remnant: Optical Proper Motions, Deep Imaging, Distance, and Brightness at Maximum
, Astrophysical Journal
, 585, 1, 324–335
, astro-ph/0208415
, 2003ApJ...585..324W
, 10.1086/345985
, The widely observed supernova SN 1054 produced the Crab Nebula. Supernovae SN 1572 and SN 1604, the latest to be observed with the naked eye in the Milky Way galaxy, had notable effects on the development of astronomy in Europe because they were used to argue against the Aristotelian idea that the universe beyond the Moon and planets was static and unchanging.CONFERENCE
, Clark, D. H.
, Stephenson, F. R.
, 1982
, The Historical Supernovae
, Supernovae: A survey of current research; Proceedings of the Advanced Study Institute, Cambridge, England, June 29 – July 10, 1981
, 355–370
, D. Reidel
, Dordrecht
, 1982ASIC...90..355C
, Johannes Kepler began observing SN 1604 at its peak on October 17, 1604, and continued to make estimates of its brightness until it faded from naked eye view a year later.JOURNAL
, Baade, W.
, 1943
, No. 675. Nova Ophiuchi of 1604 as a supernova
, Contributions from the Mount Wilson Observatory / Carnegie Institution of Washington
, 675, 1–9
, 1943CMWCI.675....1B
, It was the second supernova to be observed in a generation (after SN 1572 seen by Tycho Brahe in Cassiopeia).BOOK
, Motz, L.
, Weaver, J. H.
, 2001
, The Story of Astronomy
,weblink
, Basic Books
, 76
, 978-0-7382-0586-1
, There is some evidence that the youngest galactic supernova, G1.9+0.3, occurred in the late 19th century, considerably more recently than Cassiopeia A from around 1680.JOURNAL, Chakraborti, S., Childs, F., Soderberg, A., February 25, 2016, Young Remnants of Type Ia Supernovae and Their Progenitors: A Study Of SNR G1.9+0.3, 1510.08851v1, The Astrophysical Journal, 819, 1, 37, 10.3847/0004-637X/819/1/37, 2016ApJ...819...37C, Neither supernova was noted at the time. In the case of G1.9+0.3, high extinction along the plane of the galaxy could have dimmed the event sufficiently to go unnoticed. The situation for Cassiopeia A is less clear. Infrared light echos have been detected showing that it was a type IIb supernova and was not in a region of especially high extinction.JOURNAL, Krause, O., The Cassiopeia A Supernova was of Type IIb, Science (journal), Science, 320, 5880, 2008, 1195–1197, 10.1126/science.1155788, 18511684, 2008Sci...320.1195K, 0805.4557, Before the development of the telescope, only five supernovae were seen in the last millennium. Compared to a star's entire history, the visual appearance of a galactic supernova is very brief, perhaps spanning several months, so that the chances of observing one is roughly once in a lifetime. Only a tiny fraction of the 100 billion stars in a typical galaxy have the capacity to become a supernova, restricted to either those having large mass or extraordinarily rare kinds of binary stars containing white dwarfs.BOOK, Supernovae, Murdin, P., Murdin, L., Press Syndicate of the University of Cambridge, 1978, 978-0521300384, New York, NY, 1–3, However, observation and discovery of extragalactic supernovae are now far more common. The first such observation was of SN 1885A in the Andromeda galaxy. Today, amateur and professional astronomers are finding several hundred every year, some when near maximum brightness, others on old astronomical photographs or plates. American astronomers Rudolph Minkowski and Fritz Zwicky developed the modern supernova classification scheme beginning in 1941.JOURNAL
, da Silva, L. A. L.
, 1993
, The Classification of Supernovae
, Astrophysics and Space Science
, 202, 2, 215–236
, 1993Ap&SS.202..215D
, 10.1007/BF00626878
, During the 1960s, astronomers found that the maximum intensities of supernovae could be used as standard candles, hence indicators of astronomical distances.JOURNAL
, Kowal, C. T.
, 1968
, Absolute magnitudes of supernovae
, Astronomical Journal
, 73, 1021–1024
, 1968AJ.....73.1021K
, 10.1086/110763
, Some of the most distant supernovae observed in 2003, appeared dimmer than expected. This supports the view that the expansion of the universe is accelerating.JOURNAL
, Leibundgut, B.
, Aldering, G.
, Amanullah, R.
, Astier, P.
, Blanc, G.
, Burns, M. S.
, Conley, A. J.
, Deustua, S. E.
, Doi, M.
, Ellis, R.
, Fabbro, S.
, Folatelli, G.
, Fruchter, A. S.
, Garavini, G.
, Garmond, S.
, Garton, K.
, Gibbons, R.
, Goldhaber, G.
, Goobar, A.
, Groom, D. E.
, Hardin, D.
, Hook, I. M.
, Howell, D. A.
, Kim, A. G.
, Lee, B. C.
, Lidman, C.
, Mendez, J.
, Nobili, S.
, Nugent, P. E.
, Pain, R.
, 1
, 2003
, A cosmological surprise: The universe accelerates
, The Astrophysical Journal
, 32, 4, 121
, 2001ENews..32..121L
, 10.1086/378560, astro-ph/0309368, Techniques were developed for reconstructing supernovae events that have no written records of being observed. The date of the Cassiopeia A supernova event was determined from light echoes off nebulae,
JOURNAL
, Fabian, A. C.
, 2008
, A Blast from the Past
, Science (journal), Science
, 320, 5880, 1167–1168
, 10.1126/science.1158538
, 18511676
, while the age of supernova remnant RX J0852.0-4622 was estimated from temperature measurementsJOURNAL
, Aschenbach, B.
, 1998
, Discovery of a young nearby supernova remnant
, Nature (journal), Nature
, 396, 6707, 141–142
, 1998Natur.396..141A
, 10.1038/24103
, and the gamma ray emissions from the radioactive decay of titanium-44.JOURNAL
, Iyudin, A. F.
, Schönfelder, V.
, Bennett, K.
, Bloemen, H.
, Diehl, R.
, Hermsen, W.
, Lichti, G. G.
, Van Der Meulen, R. D.
, Ryan, J.
, Winkler, C.
, 1
, 1998
, Emission from 44Ti associated with a previously unknown Galactic supernova
, Nature (journal), Nature
, 396, 6707, 142–144
, 1998Natur.396..142I
, 10.1038/24106
, (File:One galaxy, three supernovae RXC J0949.8+1707.jpg|thumb|left|SN Antikythera, SN Eleanor and SN Alexander at galaxy cluster RXC J0949.8+1707.WEB, One galaxy, three supernovae,weblink www.spacetelescope.org, 18 June 2018, )The most luminous supernova ever recorded is ASASSN-15lh. It was first detected in June 2015 and peaked at {{solar luminosity|570 billion|link=y}}, which is twice the bolometric luminosity of any other known supernova."MEMBERWIDE">FIRST1=B. J., etal, 2016, ASASSN-15lh: A highly super-luminous supernova, Science, 351, 6270, 257–260, 10.1126/science.aac9613, 26816375, 1507.03010FIRST=G., 2016, The superluminous transient ASASSN-15lh as a tidal disruption event from a Kerr black hole, Nature Astronomy, 1, 2, 10.1038/s41550-016-0002, 1609.02927, 2016NatAs...1E...2L
, 0002,
Among the earliest detected since time of detonation, and for which the earliest spectra have been obtained (beginning at 6 hours after the actual explosion), is the Type II SN 2013fs (iPTF13dqy) which was recorded 3 hours after the supernova event on 6 October 2013 by the Intermediate Palomar Transient Factory (iPTF). The star is located in a spiral galaxy named NGC 7610, 160 million light years away in the constellation of Pegasus.NEWS,weblink Massive supernova visible millions of light years from Earth, Sample, I., 2017-02-13, The Guardian, 2017-02-13, no,weblink 2017-02-13, JOURNAL, Yaron, O., Perley, D. A., Gal-Yam, A., Groh, J. H., Horesh, A., Ofek, E. O., Kulkarni, S. R., Sollerman, J., Fransson, C., 2017-02-13, Confined dense circumstellar material surrounding a regular type II supernova, Nature Physics, advance online publication, 5, 10.1038/nphys4025, 510–517, 1701.02596, 2017NatPh..13..510Y, On 20 September 2016, amateur astronomer Victor Buso from Rosario, Argentina was testing out his new 16 inch telescope.WEB, Amateur astronomer makes once-in-lifetime discovery, Astronomy Now journalist,weblink Pole Star Publications Limited, 23 February 2018, 15 May 2018, JOURNAL, A surge of light at the birth of a supernova, M.C. Bersten, G. Folatelli, F. García, S.D. Van Dyk, O.G. Benvenuto, M. Orellana, V. Buso, J.L. Sánchez, M. Tanaka, K. Maeda, A.V. Filippenko, W. Zheng, T.G. Brink, S.B. Cenko, T. de Jaeger, S. Kumar, T.J. Moriya, K. Nomoto, D.A. Perley, I. Shivvers, N. Smith, Nature (journal), Nature, 21 February 2018, 554, 7693, 497–499, 1802.09360, 2018Natur.554..497B, 10.1038/nature25151, 29469097, When taking several twenty second exposures of galaxy NGC 613, Buso chanced upon a supernova that had just become visible on earth. After examining the images he contacted the Instituto de Astrofísica de La Plata. "It was the first time anyone had ever captured the initial moments of the “shock breakout” from an optical supernova, one not associated with a gamma-ray or X-ray burst." The odds of capturing such an event were put between one in ten million to one in a hundred million, according to astronomer Melina Bersten from the Instituto de Astrofísica.The supernova Buso observed was a Type IIb made by a star twenty times the mass of the sun. Astronomer Alex Filippenko from the University of California remarked that professional astronomers had been searching for such an event for a long time. He stated: "Observations of stars in the first moments they begin exploding provide information that cannot be directly obtained in any other way."

Discovery

File:NASA-SNR0519690-ChandraXRayObservatory-20150122.jpg|thumb|upright=1.0|right|A supernova remnantsupernova remnantEarly work on what was originally believed to be simply a new category of novae was performed during the 1930s by two astronomers named Walter Baade and Fritz Zwicky at Mount Wilson Observatory.JOURNAL
, Baade, W.
, Zwicky, F.
, 1934
, On Super-novae
, Proceedings of the National Academy of Sciences
, 20, 5, 254–259
, 1934PNAS...20..254B
, 10.1073/pnas.20.5.254
, 1076395
, 16587881
, The name super-novae was first used during 1931 lectures held at Caltech by Baade and Zwicky, then used publicly in 1933 at a meeting of the American Physical Society.JOURNAL
, Osterbrock, D. E.
, 2001
, Who Really Coined the Word Supernova? Who First Predicted Neutron Stars?
, Bulletin of the American Astronomical Society
, 33, 1330
, 2001AAS...199.1501O
, By 1938, the hyphen had been lost and the modern name was in use.BOOK
, Murdin, P.
, Murdin, L.
, 1985
, Supernovae
, 42, 2nd
, Cambridge University Press
, 978-0-521-30038-4
, Because supernovae are relatively rare events within a galaxy, occurring about three times a century in the Milky Way,JOURNAL
, Reynolds, S. P.
, Borkowski, K. J.
, Green, D. A.
, Hwang, U.
, Harrus, I. M.
, Petre, R.
, 1
, 2008
, The Youngest Galactic Supernova Remnant: G1.9+0.3
, The Astrophysical Journal Letters
, 680, 1, L41–L44
, 0803.1487
, 2008ApJ...680L..41R
, 10.1086/589570
, obtaining a good sample of supernovae to study requires regular monitoring of many galaxies.Supernovae in other galaxies cannot be predicted with any meaningful accuracy. Normally, when they are discovered, they are already in progress.JOURNAL
, Colgate, S. A.
, McKee, C.
, 1969
, Early Supernova Luminosity
, The Astrophysical Journal
, 157, 623
, 1969ApJ...157..623C
, 10.1086/150102
, Most scientific interest in supernovae—as standard candles for measuring distance, for example—require an observation of their peak luminosity. It is therefore important to discover them well before they reach their maximum. Amateur astronomers, who greatly outnumber professional astronomers, have played an important role in finding supernovae, typically by looking at some of the closer galaxies through an optical telescope and comparing them to earlier photographs.BOOK
, Zuckerman, B.
, Malkan, M. A.
, 1996
, The Origin and Evolution of the Universe
,weblink
, Jones & Bartlett Learning
, 68
, 978-0-7637-0030-0
, no
,weblink
, 2016-08-20
,
, Toward the end of the 20th century astronomers increasingly turned to computer-controlled telescopes and CCDs for hunting supernovae. While such systems are popular with amateurs, there are also professional installations such as the Katzman Automatic Imaging Telescope.CONFERENCE
, Filippenko, A. V.
, Li, W.-D.
, Treffers, R. R.
, Modjaz, M.
, 2001
, The Lick Observatory Supernova Search with the Katzman Automatic Imaging Telescope
, Paczynski, B.
, Chen, W.-P.
, Lemme, C.
, Small Telescope Astronomy on Global Scale
, 246, 121
, ASP Conference Series
, Astronomical Society of the Pacific
, San Francisco
, 2001ASPC..246..121F
, 978-1-58381-084-2
, The Supernova Early Warning System (SNEWS) project uses a network of neutrino detectors to give early warning of a supernova in the Milky Way galaxy.JOURNAL
, Antonioli, P.
, Fienberg, R. T.
, Fleurot, F.
, Fukuda, Y.
, Fulgione, W.
, Habig, A.
, Heise, J.
, McDonald, A. B.
, Mills, C.
, Namba, T.
, Robinson, L. J.
, Scholberg, K.
, Schwendener, M.
, Sinnott, R. W.
, Stacey, B.
, Suzuki, Y.
, Tafirout, R.
, Vigorito, C.
, Viren, B.
, Virtue, C.
, Zichichi, A.
, 1
, 2004
, SNEWS: The SuperNova Early Warning System
, New Journal of Physics
, 6, 114
, astro-ph/0406214
, 2004NJPh....6..114A
, 10.1088/1367-2630/6/1/114
,
JOURNAL
, Scholberg, K.
, 2000
, SNEWS: The supernova early warning system
, AIP Conference Proceedings
, 523, 355–361
, astro-ph/9911359
, 2000AIPC..523..355S
, 10.1063/1.1291879, 10.1.1.314.8663
, Neutrinos are particles that are produced in great quantities by a supernova,
JOURNAL
, Beacom, J. F.
, 1999
, Supernova neutrinos and the neutrino masses
, Revista Mexicana de Fisica
, 45, 2, 36
, hep-ph/9901300
, 1999RMxF...45...36B
, and they are not significantly absorbed by the interstellar gas and dust of the galactic disk.File:A star set to explode.jpg|thumbnail|left|upright=1.2|"A star set to explode", the SBW1 nebula surrounds a massive blue supergiant in the Carina NebulaCarina NebulaSupernova searches fall into two classes: those focused on relatively nearby events and those looking farther away. Because of the expansion of the universe, the distance to a remote object with a known emission spectrum can be estimated by measuring its Doppler shift (or redshift); on average, more-distant objects recede with greater velocity than those nearby, and so have a higher redshift. Thus the search is split between high redshift and low redshift, with the boundary falling around a redshift range of z=0.1–0.3JOURNAL
, Frieman, J. A.
, Bassett, B.
, Becker, A.
, Choi, C.
, Cinabro, D.
, Dejongh, F.
, Depoy, D. L.
, Dilday, B.
, Doi, M.
, Garnavich, P. M.
, Hogan, C. J.
, Holtzman, J.
, Im, M.
, Jha, S.
, Kessler, R.
, Konishi, K.
, Lampeitl, H.
, Marriner, J.
, Marshall, J. L.
, McGinnis, D.
, Miknaitis, G.
, Nichol, R. C.
, Prieto, J. L.
, Riess, A. G.
, Richmond, M. W.
, Romani, R.
, Sako, M.
, Schneider, D. P.
, Smith, M.
, Takanashi, N.
, 1
, 2008
, The Sloan Digital Sky Survey-Ii Supernova Survey: Technical Summary
, The Astronomical Journal
, 135, 1
, 338–347
, 0708.2749
, 2008AJ....135..338F
, 10.1088/0004-6256/135/1/338
, —where z is a dimensionless measure of the spectrum's frequency shift.High redshift searches for supernovae usually involve the observation of supernova light curves. These are useful for standard or calibrated candles to generate Hubble diagrams and make cosmological predictions. Supernova spectroscopy, used to study the physics and environments of supernovae, is more practical at low than at high redshift.CONFERENCE
, Perlmutter, S. A.
, etal
, 1997
, Scheduled discovery of 7+ high-redshift SNe: First cosmology results and bounds on q0
, Ruiz-Lapuente, P.
, Canal, R.
, Isern, J.
, Thermonuclear Supernovae, Proceedings of the NATO Advanced Study Institute
, NATO Advanced Science Institutes Series C
, 486, 749
, Kluwer Academic Publishers
, Dordrecth
, astro-ph/9602122
, 1997ASIC..486..749P, 10.1007/978-94-011-5710-0_46,
JOURNAL
, Linder, E. V.
, Huterer, D.
, 2003
, Importance of supernovae at z > 1.5 to probe dark energy
, Physical Review D
, 67, 8
, 081303
, astro-ph/0208138
, 2003PhRvD..67h1303L
, 10.1103/PhysRevD.67.081303
, Low redshift observations also anchor the low-distance end of the Hubble curve, which is a plot of distance versus redshift for visible galaxies.JOURNAL
, Perlmutter, S. A.
, Gabi, S.
, Goldhaber, G.
, Goobar, A.
, Groom, D. E.
, Hook, I. M.
, Kim, A. G.
, Kim, M. Y.
, Lee, J. C.
, Pain, R.
, Pennypacker, C. R.
, Small, I. A.
, Ellis, R. S.
, McMahon, R. G.
, Boyle, B. J.
, Bunclark, P. S.
, Carter, D.
, Irwin, M. J.
, Glazebrook, K.
, Newberg, H. J. M.
, Filippenko, A. V.
, Matheson, T.
, Dopita, M.
, Couch, W. J.
, 1997
, 1
, Measurements of the Cosmological Parameters Ω and Λ from the First Seven Supernovae at z ≥ 0.35
, The Astrophysical Journal
, 483, 2, 565
, astro-ph/9608192
, 1997ApJ...483..565P
, 10.1086/304265
,
JOURNAL
, Copin, Y.
, Blanc, N.
, Bongard, S.
, Gangler, E.
, Saugé, L.
, Smadja, G.
, Antilogus, P.
, Garavini, G.
, Gilles, S.
, Pain, R.
, Aldering, G.
, Bailey, S.
, Lee, B.C.
, Loken, S.
, Nugent, P. E.
, Perlmutter, S. A.
, Scalzo, R.
, Thomas, R.C.
, Wang, L.
, Weaver, B.A.
, Pécontal, E.
, Kessler, R., Baltay
, C., Rabinowitz, D.
, Bauer, A.
, 1
, 2006
, The Nearby Supernova Factory
,weblink
, New Astronomy Reviews
, 50, 4–5, 637–640
, 2006NewAR..50..436C
, 10.1016/j.newar.2006.02.035
citeseerx=10.1.1.316.4895
, (See also Hubble's law).

Naming convention

missing image!
- Keplers supernova.jpg -
Multiwavelength X-ray, infrared, and optical compilation image of Kepler's supernova remnant, SN 1604.
Supernova discoveries are reported to the International Astronomical Union's Central Bureau for Astronomical Telegrams, which sends out a circular with the name it assigns to that supernova. The name is the marker SN followed by the year of discovery, suffixed with a one or two-letter designation. The first 26 supernovae of the year are designated with a capital letter from A to Z. Afterward pairs of lower-case letters are used: aa, ab, and so on. Hence, for example, SN 2003C designates the third supernova reported in the year 2003.JOURNAL
, Kirshner, R. P.
, 1980
, Type I supernovae: An observer's view
, AIP Conference Proceedings
, 63, 33–37
, 1980AIPC...63...33K
, 10.1063/1.32212, AIP Conference Proceedings
, The last supernova of 2005 was SN 2005nc, indicating that it was the 367thThe value is obtained by converting the suffix "nc" from bijective base-26, with a=1, b=2, c=3, ... z=26. Thus nc=n × 26 + c=14 × 26 + 3=367. supernova found in 2005. Since 2000, professional and amateur astronomers have been finding several hundreds of supernovae each year (572 in 2007, 261 in 2008, 390 in 2009; 231 in 2013).
WEB
, List of Supernovae
,weblink
, International Astronomical Union, IAU Central Bureau for Astronomical Telegrams
, 2010-10-25
, no
,weblink" title="web.archive.org/web/20101112022554weblink">weblink
, 2010-11-12
,
, WEB
, The Padova-Asiago supernova catalogue
,weblink
, Asiago Astrophysical Observatory, Osservatorio Astronomico di Padova
, 2014-01-10
, no
,weblink" title="web.archive.org/web/20140110184455weblink">weblink
, 2014-01-10
,
, Historical supernovae are known simply by the year they occurred: SN 185, SN 1006, SN 1054, SN 1572 (called Tycho's Nova) and SN 1604 (Kepler's Star). Since 1885 the additional letter notation has been used, even if there was only one supernova discovered that year (e.g. SN 1885A, SN 1907A, etc.) — this last happened with SN 1947A. SN, for SuperNova, is a standard prefix. Until 1987, two-letter designations were rarely needed; since 1988, however, they have been needed every year.

Classification

File:Artist's impression of supernova 1993J.jpg|thumb|Artist's impression of supernova 1993J.WEB , Artist's impression of supernova 1993J
,
weblink
, SpaceTelescope.org
, 2014-09-12
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,weblink" title="web.archive.org/web/20140913090541weblink">weblink
, 2014-09-13
,
, ">
, Artist's impression of supernova 1993J
,weblink
, SpaceTelescope.org
, 2014-09-12
, no
,weblink" title="web.archive.org/web/20140913090541weblink">weblink
, 2014-09-13
,
, As part of the attempt to understand supernovae, astronomers have classified them according to their light curves and the absorption lines of different chemical elements that appear in their spectra. The first element for division is the presence or absence of a line caused by hydrogen. If a supernova's spectrum contains lines of hydrogen (known as the Balmer series in the visual portion of the spectrum) it is classified Type II; otherwise it is Type I. In each of these two types there are subdivisions according to the presence of lines from other elements or the shape of the light curve (a graph of the supernova's apparent magnitude as a function of time).CONFERENCE
, Cappellaro, E.
, Turatto, M.
, 2001
, Supernova Types and Rates
, Influence of Binaries on Stellar Population Studies
, 264, 199
, Kluwer Academic Publishers
, Dordrecht
, astro-ph/0012455
, 2001ASSL..264..199C
, 10.1007/978-94-015-9723-4_16
, 978-0-7923-7104-5
, {|class="wikitable"|+Supernova taxonomyType INo hydrogenType Ia supernovaPresents a singly ionization>ionized silicon (Si II) line at 615.0 nm (nanometers), near peak lightThermal runawayType Ib/cWeak or no silicon absorption featureType IbShows a non-ionized helium (He I) line at 587.6 nmCore collapseType IcWeak or no heliumType IIShows hydrogenType II-P/L/NType II spectrum throughoutType II-P/LNo narrow linesType II supernova#Light curves for Type II-L and Type II-P supernovae>Type II-PReaches a "plateau" in its light curveType II supernova#Light curves for Type II-L and Type II-P supernovae>Type II-LDisplays a "linear" decrease in its light curve (linear in magnitude versus time).Type IInSome narrow linesType IIbSpectrum changes to become like Type Ib

Type I

Type I supernovae are subdivided on the basis of their spectra, with Type Ia showing a strong ionised silicon absorption line. Type I supernovae without this strong line are classified as Type Ib and Ic, with Type Ib showing strong neutral helium lines and Type Ic lacking them. The light curves are all similar, although Type Ia are generally brighter at peak luminosity, but the light curve is not important for classification of Type I supernovae.A small number of Type Ia supernovae exhibit unusual features such as non-standard luminosity or broadened light curves, and these are typically classified by referring to the earliest example showing similar features. For example, the sub-luminous SN 2008ha is often referred to as SN 2002cx-like or class Ia-2002cx.A small proportion of type Ic supernovae show highly broadened and blended emission lines which are taken to indicate very high expansion velocities for the ejecta. These have been classified as type Ic-BL or Ic-bl.JOURNAL, 2014ApJS..213...19B, 1405.1428, Multi-color Optical and Near-infrared Light Curves of 64 Stripped-envelope Core-Collapse Supernovae, The Astrophysical Journal Supplement, 213, 2, 19, Bianco, F. B., Modjaz, M., Hicken, M., Friedman, A., Kirshner, R. P., Bloom, J. S., Challis, P., Marion, G. H., Wood-Vasey, W. M., Rest, A., 2014, 10.1088/0067-0049/213/2/19,

Type II

thumb|Light curves are used to classify Type II-P and Type II-L supernovaeThe supernovae of Type II can also be sub-divided based on their spectra. While most Type II supernovae show very broad emission lines which indicate expansion velocities of many thousands of kilometres per second, some, such as SN 2005gl, have relatively narrow features in their spectra. These are called Type IIn, where the 'n' stands for 'narrow'.A few supernovae, such as SN 1987K and SN 1993J, appear to change types: they show lines of hydrogen at early times, but, over a period of weeks to months, become dominated by lines of helium. The term "Type IIb" is used to describe the combination of features normally associated with Types II and Ib.Type II supernovae with normal spectra dominated by broad hydrogen lines that remain for the life of the decline are classified on the basis of their light curves. The most common type shows a distinctive "plateau" in the light curve shortly after peak brightness where the visual luminosity stays relatively constant for several months before the decline resumes. These are called Type II-P referring to the plateau. Less common are Type II-L supernovae that lack a distinct plateau. The "L" signifies "linear" although the light curve is not actually a straight line.Supernovae that do not fit into the normal classifications are designated peculiar, or 'pec'.BOOK
, Turatto, M.
, 2003
, Classification of Supernovae
, Supernovae and Gamma-Ray Bursters
, 598, 21–36
, Lecture Notes in Physics
, 10.1007/3-540-45863-8_3
, 978-3-540-44053-6citeseerx=10.1.1.256.2965
,

Types III, IV, and V

Fritz Zwicky defined additional supernovae types, although based on a very few examples that did not cleanly fit the parameters for a Type I or Type II supernova. SN 1961i in NGC 4303 was the prototype and only member of the Type III supernova class, noted for its broad light curve maximum and broad hydrogen Balmer lines that were slow to develop in the spectrum. SN 1961f in NGC 3003 was the prototype and only member of the Type IV class, with a light curve similar to a Type II-P supernova, with hydrogen absorption lines but weak hydrogen emission lines. The Type V class was coined for SN 1961V in NGC 1058, an unusual faint supernova or supernova impostor with a slow rise to brightness, a maximum lasting many months, and an unusual emission spectrum. The similarity of SN 1961V to the Eta Carinae Great Outburst was noted.JOURNAL
, Zwicky, F.
, 1964
, NGC 1058 and its Supernova 1961
, The Astrophysical Journal
, 139, 514
, 1964ApJ...139..514Z
, 10.1086/147779
, Supernovae in M101 (1909) and M83 (1923 and 1957) were also suggested as possible Type IV or Type V supernovae.CONFERENCE
, Zwicky, F.
, 1962
, New Observations of Importance to Cosmology
, McVittie, G. C.
, Problems of Extra-Galactic Research, Proceedings from IAU Symposium
, 15, 347
, Macmillan Press
, New York
, 1962IAUS...15..347Z
, These types would now all be treated as peculiar Type II supernovae, of which many more examples have been discovered, although it is still debated whether SN 1961V was a true supernova following an LBV outburst or an impostor.JOURNAL
, Doggett, J. B.
, Branch, D.
, 1985
, A comparative study of supernova light curves
, The Astronomical Journal
, 90, 2303
, 1985AJ.....90.2303D
, 10.1086/113934
,

Current models

File:The Rise and Fall of a Supernova.jpg|thumb|upright=1.2|Sequence shows the rapid brightening and slower fading of a supernova in the galaxy NGC 1365 (the bright dot close to the upper part of the galactic center)NEWS NGC 1365The type codes, described above given to supernovae, are taxonomic in nature: the type number describes the light observed from the supernova, not necessarily its cause. For example, Type Ia supernovae are produced by runaway fusion ignited on degenerate white dwarf progenitors while the spectrally similar Type Ib/c are produced from massive Wolf–Rayet progenitors by core collapse. The following summarizes what is currently believed to be the most plausible explanations for supernovae.

Thermal runaway

(File:Progenitor IA supernova.svg|thumb|Formation of a Type Ia supernova)A white dwarf star may accumulate sufficient material from a stellar companion to raise its core temperature enough to ignite carbon fusion, at which point it undergoes runaway nuclear fusion, completely disrupting it. There are three avenues by which this detonation is theorized to happen: stable accretion of material from a companion, the collision of two white dwarfs, or accretion that causes ignition in a shell that then ignites. The dominant mechanism by which Type Ia supernovae are produced remains unclear.JOURNAL
, Piro, A. L.
, Thompson, T. A.
, Kochanek, C. S.
, 2014
, Reconciling 56Ni production in Type Ia supernovae with double degenerate scenarios
, Monthly Notices of the Royal Astronomical Society
, 438, 4, 3456
, 1308.0334
, 2014MNRAS.438.3456P
, 10.1093/mnras/stt2451
, Despite this uncertainty in how Type Ia supernovae are produced, Type Ia supernovae have very uniform properties, and are useful standard candles over intergalactic distances. Some calibrations are required to compensate for the gradual change in properties or different frequencies of abnormal luminosity supernovae at high red shift, and for small variations in brightness identified by light curve shape or spectrum.JOURNAL
, Chen, W.-C.
, Li, X.-D.
, 2009
, On the Progenitors of Super-Chandrasekhar Mass Type Ia Supernovae
, The Astrophysical Journal
, 702, 1, 686–691
, 0907.0057
, 2009ApJ...702..686C
, 10.1088/0004-637X/702/1/686
, JOURNAL
, Howell, D. A.
, Sullivan, M.
, Conley, A. J.
, Carlberg, R. G.
, 2007
, Predicted and Observed Evolution in the Mean Properties of Type Ia Supernovae with Redshift
, Astrophysical Journal Letters
, 667, 1, L37–L40
, astro-ph/0701912
, 2007ApJ...667L..37H
, 10.1086/522030
,

Normal Type Ia

There are several means by which a supernova of this type can form, but they share a common underlying mechanism. If a carbon-oxygenFor a core primarily composed of oxygen, neon and magnesium, the collapsing white dwarf will typically form a neutron star. In this case, only a fraction of the star's mass will be ejected during the collapse. white dwarf accreted enough matter to reach the Chandrasekhar limit of about 1.44 solar masses ({{Solar mass|link=y}})JOURNAL
, Mazzali, P. A.
, Röpke, F. K.
, Benetti, S.
, Hillebrandt, W.
, 2007
, A Common Explosion Mechanism for Type Ia Supernovae
, Science (journal), Science
, 315, 5813, 825–828
, astro-ph/0702351
, 2007Sci...315..825M
, 10.1126/science.1136259
, 17289993
, (for a non-rotating star), it would no longer be able to support the bulk of its mass through electron degeneracy pressureJOURNAL
, Lieb, E. H.
, Yau, H.-T.
, 1987
, A rigorous examination of the Chandrasekhar theory of stellar collapse
, The Astrophysical Journal
, 323, 1, 140–144
, 1987ApJ...323..140L
, 10.1086/165813
, BOOK
, Canal, R.
, Gutiérrez, J. L.
, 1997
, The possible white dwarf-neutron star connection
, Isern, J.
, Hernanz, M.
, Gracia-Berro, E.
, White Dwarfs, Proceedings of the 10th European Workshop on White Dwarfs
,
, 214, 49
, Kluwer Academic Publishers
, Dordrecht
, 1997ASSL..214...49C
, 978-0-7923-4585-5
doi=10.1007/978-94-011-5542-7_7, and would begin to collapse. However, the current view is that this limit is not normally attained; increasing temperature and density inside the core Carbon detonation Carbon burning process>carbon fusion as the star approaches the limit (to within about 1%BOOK
, Wheeler, J. C.
, 2000
, Cosmic Catastrophes: Supernovae, Gamma-Ray Bursts, and Adventures in Hyperspace
,weblink
, 96
, Cambridge University Press
, 978-0-521-65195-0
, no
,weblink
, 2015-09-10
,
, ), before collapse is initiated.Within a few seconds, a substantial fraction of the matter in the white dwarf undergoes nuclear fusion, releasing enough energy (1–{{val|2|e=44|ul=J}})JOURNAL
, Khokhlov, A. M.
, Mueller, E.
, Höflich, P. A.
, 1993
, Light curves of Type IA supernova models with different explosion mechanisms
, Astronomy and Astrophysics
, 270, 1–2, 223–248
, 1993A&A...270..223K
,
, to unbind the star in a supernova.JOURNAL
, Röpke, F. K.
, Hillebrandt, W.
, 2004
, The case against the progenitor's carbon-to-oxygen ratio as a source of peak luminosity variations in Type Ia supernovae
, Astronomy and Astrophysics Letters
, 420, 1, L1–L4
, astro-ph/0403509
, 2004A&A...420L...1R
, 10.1051/0004-6361:20040135
, An outwardly expanding shock wave is generated, with matter reaching velocities on the order of 5,000–20,000 km/s, or roughly 3% of the speed of light. There is also a significant increase in luminosity, reaching an absolute magnitude of −19.3 (or 5 billion times brighter than the Sun), with little variation.JOURNAL
, Hillebrandt, W.
, Niemeyer, J. C.
, 2000
, Type IA Supernova Explosion Models
, Annual Review of Astronomy and Astrophysics
, 38, 1, 191–230
, astro-ph/0006305
, 2000ARA&A..38..191H
, 10.1146/annurev.astro.38.1.191
, The model for the formation of this category of supernova is a closed binary star system. The larger of the two stars is the first to evolve off the main sequence, and it expands to form a red giant. The two stars now share a common envelope, causing their mutual orbit to shrink. The giant star then sheds most of its envelope, losing mass until it can no longer continue nuclear fusion. At this point it becomes a white dwarf star, composed primarily of carbon and oxygen.CONFERENCE
, Paczyński, B.
, 1976
, Common Envelope Binaries
, Structure and Evolution of Close Binary Systems
, IAU Symposium No. 73
, Eggleton, P.
, Mitton, S.
, Whelan, J.
, 75–80
, D. Reidel
, Dordrecht
, 1976IAUS...73...75P
, Eventually the secondary star also evolves off the main sequence to form a red giant. Matter from the giant is accreted by the white dwarf, causing the latter to increase in mass. Despite widespread acceptance of the basic model, the exact details of initiation and of the heavy elements produced in the catastrophic event are still unclear.Type Ia supernovae follow a characteristic light curve—the graph of luminosity as a function of time—after the event. This luminosity is generated by the radioactive decay of nickel-56 through cobalt-56 to iron-56. The peak luminosity of the light curve is extremely consistent across normal Type Ia supernovae, having a maximum absolute magnitude of about −19.3. This allows them to be used as a secondaryJOURNAL
, Macri, L. M.
, Stanek, K. Z.
, Bersier, D.
, Greenhill, L. J.
, Reid, M. J.
, 2006
, A New Cepheid Distance to the Maser-Host Galaxy NGC 4258 and Its Implications for the Hubble Constant
, The Astrophysical Journal
, 652, 2, 1133–1149
, astro-ph/0608211
, 2006ApJ...652.1133M
, 10.1086/508530
, standard candle to measure the distance to their host galaxies.JOURNAL
, Colgate, S. A.
, 1979
, Supernovae as a standard candle for cosmology
, The Astrophysical Journal
, 232, 1, 404–408
, 1979ApJ...232..404C
, 10.1086/157300
,

Non-standard Type Ia

Another model for the formation of Type Ia supernovae involves the merger of two white dwarf stars, with the combined mass momentarily exceeding the Chandrasekhar limit.JOURNAL
, Ruiz-Lapuente, P.
, Blinnikov, S.
, Canal, R.
, Mendez, J.
, Sorokina, E.
, Visco, A.
, Walton, N.
, 1
, 2000
, Type IA supernova progenitors
, Memorie della Societa Astronomica Italiana
, 71, 435
, 2000MmSAI..71..435R
, There is much variation in this type of event,JOURNAL
, Dan, M.
, Rosswog, S.
, Guillochon, J.
, Ramirez-Ruiz, E.
, 2012
, How the merger of two white dwarfs depends on their mass ratio: Orbital stability and detonations at contact
, Monthly Notices of the Royal Astronomical Society
, 422, 3, 2417
, 1201.2406
, 2012MNRAS.422.2417D
, 10.1111/j.1365-2966.2012.20794.x
, and in many cases there may be no supernova at all, but it is expected that they will have a broader and less luminous light curve than the more normal SN Type Ia.Abnormally bright Type Ia supernovae are expected when the white dwarf already has a mass higher than the Chandrasekhar limit,JOURNAL
, Howell, D. A.
, Sullivan, M.
, Nugent, P. E.
, Ellis, R. S.
, Conley, A. J.
, Le Borgne, D.
, Carlberg, R. G.
, Guy, J.
, Balam, D.
, Basa, S.
, Fouchez, D.
, Hook, I. M.
, Hsiao, E. Y.
, Neill, J. D.
, Pain, R.
, Perrett, K. M.
, Pritchet, C. J.
, 1
, 2006
, The type Ia supernova SNLS-03D3bb from a super-Chandrasekhar-mass white dwarf star
, Nature (journal), Nature
, 443, 7109, 308–311
, astro-ph/0609616
, 2006Natur.443..308H
, 10.1038/nature05103
, 16988705
, possibly enhanced further by asymmetry,JOURNAL
, Tanaka, M.
, Kawabata, K. S.
, Yamanaka, M.
, Maeda, K.
, Hattori, T.
, Aoki, K.
, Nomoto, K. I.
, Iye, M.
, Sasaki, T.
, Mazzali, P. A.
, Pian, E.
, 1
, 2010
, Spectropolarimetry of Extremely Luminous Type Ia Supernova 2009dc: Nearly Spherical Explosion of Super-Chandrasekhar Mass White Dwarf
, The Astrophysical Journal
, 714, 2, 1209
, 0908.2057
, 2010ApJ...714.1209T
, 10.1088/0004-637X/714/2/1209
, but the ejected material will have less than normal kinetic energy.There is no formal sub-classification for the non-standard Type Ia supernovae. It has been proposed that a group of sub-luminous supernovae that occur when helium accretes onto a white dwarf should be classified as Type Iax.JOURNAL
, Wang, B.
, Liu, D.
, Jia, S.
, Han, Z.
, 2014
, Helium double-detonation explosions for the progenitors of type Ia supernovae
, Proceedings of the International Astronomical Union
, 9, S298, 442
, 1301.1047
, 2014IAUS..298..442W
, 10.1017/S1743921313007072
, JOURNAL
, Foley, R. J.
, Challis, P. J.
, Chornock, R.
, Ganeshalingam, M.
, Li, W.
, Marion, G. H.
, Morrell, N. I.
, Pignata, G.
, Stritzinger, M. D.
, Silverman, J. M.
, Wang, X.
, Anderson, J. P.
, Filippenko, A. V.
, Freedman, W. L.
, Hamuy, M.
, Jha, S. W.
, Kirshner, R. P.
, McCully, C.
, Persson, S. E.
, Phillips, M. M.
, Reichart, D. E.
, Soderberg, A. M.
, 1
, 2013
, Type Iax Supernovae: A New Class of Stellar Explosion
, The Astrophysical Journal
, 767, 1, 57
, 1212.2209
, 2013ApJ...767...57F
, 10.1088/0004-637X/767/1/57
, This type of supernova may not always completely destroy the white dwarf progenitor and could leave behind a zombie star.JOURNAL
, McCully, C.
, Jha, S. W.
, Foley, R. J.
, Bildsten, L.
, Fong, W.-F.
, Kirshner, R. P.
, Marion, G. H.
, Riess, A. G.
, Stritzinger, M. D.
, 1
, 2014
, A luminous, blue progenitor system for the type Iax supernova 2012Z
, Nature (journal), Nature
, 512, 7512, 54–56
, 1408.1089
, 2014Natur.512...54M
, 10.1038/nature13615
, 25100479
, One specific type of non-standard Type Ia supernova develops hydrogen, and other, emission lines and gives the appearance of mixture between a normal Type Ia and a Type IIn supernova. Examples are SN 2002ic and SN 2005gj. These supernova have been dubbed Type Ia/IIn, Type Ian, Type IIa and Type IIan.JOURNAL
, Silverman, J. M.
, Nugent, P. E.
, Gal-Yam, A.
, Sullivan, M.
, Howell, D. A.
, Filippenko, A. V.
, Arcavi, I.
, Ben-Ami, S.
, Bloom, J. S.
, Cenko, S. B.
, Cao, Y.
, Chornock, R.
, Clubb, K. I.
, Coil, A. L.
, Foley, R. J.
, Graham, M. L.
, Griffith, C. V.
, Horesh, A.
, Kasliwal, M. M.
, Kulkarni, S. R.
, Leonard, D. C.
, Li, W.
, Matheson, T.
, Miller, A. A.
, Modjaz, M.
, Ofek, E. O.
, Pan, Y.-C.
, Perley, D. A.
, Poznanski, D.
, Quimby, R. M.
, 1
, 2013
, Type Ia Supernovae strongle interaction with their circumstellar medium
, The Astrophysical Journal Supplement Series
, 207, 1, 3
, 1304.0763
, 2013ApJS..207....3S
, 10.1088/0067-0049/207/1/3
,

Core collapse

(File:Supernovae as initial mass-metallicity.svg|upright=1.2|left|thumb|Supernova types by initial mass-metallicity)thumb|The layers of a massive, evolved star just prior to core collapse (Not to scale)Very massive stars can undergo core collapse when nuclear fusion becomes unable to sustain the core against its own gravity; passing this threshold is the cause of all types of supernova except Type Ia. The collapse may cause violent expulsion of the outer layers of the star resulting in a supernova, or the release of gravitational potential energy may be insufficient and the star may collapse into a black hole or neutron star with little radiated energy.Core collapse can be caused by several different mechanisms: electron capture; exceeding the Chandrasekhar limit; pair-instability; or photodisintegration.JOURNAL
, Heger, A.
, Fryer, C. L.
, Woosley, S. E.
, Langer, N.
, Hartmann, D. H.
, 2003
, How Massive Single Stars End Their Life
, Astrophysical Journal
, 591, 1, 288–300
, astro-ph/0212469
, 2003ApJ...591..288H
, 10.1086/375341
, JOURNAL
, Nomoto, K.
, Tanaka, M.
, Tominaga, N.
, Maeda, K.
, 2010
, Hypernovae, gamma-ray bursts, and first stars
, New Astronomy Reviews
, 54, 3–6, 191
, 2010NewAR..54..191N
, 10.1016/j.newar.2010.09.022
, When a massive star develops an iron core larger than the Chandrasekhar mass it will no longer be able to support itself by electron degeneracy pressure and will collapse further to a neutron star or black hole. Electron capture by magnesium in a degenerate O/Ne/Mg core causes gravitational collapse followed by explosive oxygen fusion, with very similar results. Electron-positron pair production in a large post-helium burning core removes thermodynamic support and causes initial collapse followed by runaway fusion, resulting in a pair-instability supernova. A sufficiently large and hot stellar core may generate gamma-rays energetic enough to initiate photodisintegration directly, which will cause a complete collapse of the core.The table below lists the known reasons for core collapse in massive stars, the types of star that they occur in, their associated supernova type, and the remnant produced. The metallicity is the proportion of elements other than hydrogen or helium, as compared to the Sun. The initial mass is the mass of the star prior to the supernova event, given in multiples of the Sun's mass, although the mass at the time of the supernova may be much lower.Type IIn supernovae are not listed in the table. They can potentially be produced by various types of core collapse in different progenitor stars, possibly even by Type Ia white dwarf ignitions, although it seems that most will be from iron core collapse in luminous supergiants or hypergiants (including LBVs). The narrow spectral lines for which they are named occur because the supernova is expanding into a small dense cloud of circumstellar material.JOURNAL
, Moriya, T. J.
, 2012
, Progenitors of Recombining Supernova Remnants
, The Astrophysical Journal
, 750, 1, L13
, 1203.5799
, 2012ApJ...750L..13M
, 10.1088/2041-8205/750/1/L13
, It appears that a significant proportion of supposed Type IIn supernovae are actually supernova impostors, massive eruptions of LBV-like stars similar to the Great Eruption of Eta Carinae. In these events, material previously ejected from the star creates the narrow absorption lines and causes a shock wave through interaction with the newly ejected material.JOURNAL
, Smith, N.
, Ganeshalingam, M.
, Chornock, R.
, Filippenko, A. V.
, Li, W.
, Silverman, J. M.
, Steele, T. N.
, Griffith, C. V.
, Joubert, N.
, Lee, N. Y.
, Lowe, T. B.
, Mobberley, M. P.
, Winslow, D. M.
, 1
, 2009
, Sn 2008S: A Cool Super-Eddington Wind in a Supernova Impostor
, The Astrophysical Journal
, 697, 1, L49
, 0811.3929
, 2009ApJ...697L..49S
, 10.1088/0004-637X/697/1/L49
, {|class="wikitable"|+ Core collapse scenarios by mass and metallicity! Cause of collapse !! Progenitor star approximate initial mass (solar masses) !! Supernova type !! Remnant|Neutron starIron core collapse 10–25 Faint II-P Neutron star|Black hole after fallback of material onto an initial neutron star|Neutron star|Black holegamma-ray burst (GRB) >|Black hole after fallback of material onto an initial neutron star|Neutron star|Black hole|No remnant|Massive black hole(File:Remnants of single massive stars.svg|left|upright=1.2|thumb|Remnants of single massive stars)upright=1.4|thumb|Within a massive, evolved star (a) the onion-layered shells of elements undergo fusion, forming an iron core (b) that reaches Chandrasekhar-mass and starts to collapse. The inner part of the core is compressed into neutrons (c), causing infalling material to bounce (d) and form an outward-propagating shock front (red). The shock starts to stall (e), but it is re-invigorated by a process that may include neutrino interaction. The surrounding material is blasted away (f), leaving only a degenerate remnant.When a stellar core is no longer supported against gravity, it collapses in on itself with velocities reaching 70,000 km/s (0.23c),JOURNAL
, Fryer, C. L.
, New, K. C. B.
, 2003
, Gravitational Waves from Gravitational Collapse
, Living Reviews in Relativity
, 6, 1, 2
, gr-qc/0206041
, 2003LRR.....6....2F
, 10.12942/lrr-2003-2, 28163639
, 5253977
, resulting in a rapid increase in temperature and density. What follows next depends on the mass and structure of the collapsing core, with low mass degenerate cores forming neutron stars, higher mass degenerate cores mostly collapsing completely to black holes, and non-degenerate cores undergoing runaway fusion.
The initial collapse of degenerate cores is accelerated by beta decay, photodisintegration and electron capture, which causes a burst of electron neutrinos. As the density increases, neutrino emission is cut off as they become trapped in the core. The inner core eventually reaches typically 30 km diameter and a density comparable to that of an atomic nucleus, and neutron degeneracy pressure tries to halt the collapse. If the core mass is more than about {{Solar mass|15|link=y}} then neutron degeneracy is insufficient to stop the collapse and a black hole forms directly with no supernova.In lower mass cores the collapse is stopped and the newly formed neutron core has an initial temperature of about 100 billion kelvin, 6000 times the temperature of the sun's core.JOURNAL
, Janka, H.-T.
, Langanke, K.
, Marek, A.
, Martínez-Pinedo, G.
, Müller, B.
, Theory of core-collapse supernovae
, Physics Reports
, 442, 1–6
, 38–74, 2007
, astro-ph/0612072
, 2007PhR...442...38J
, 10.1016/j.physrep.2007.02.002
, At this temperature, neutrino-antineutrino pairs of all flavors are efficiently formed by thermal emission. These thermal neutrinos are several times more abundant than the electron-capture neutrinos.BOOK
, Gribbin, J. R.
, Gribbin, M.
, 2000
, Stardust: Supernovae and Life – The Cosmic Connection
, Yale University Press
, 173
, 978-0-300-09097-0
, About 1046 joules, approximately 10% of the star's rest mass, is converted into a ten-second burst of neutrinos which is the main output of the event.ARXIV
, Barwick, S. W
, Beacom, J. F
, Cianciolo, V.
, Dodelson, S.
, Feng, J. L
, Fuller, G. M
, Kaplinghat, M.
, McKay, D. W
, Meszaros, P.
, Mezzacappa, A.
, Murayama, H.
, Olive, K. A
, Stanev, T.
, Walker, T. P
, 2004
, APS Neutrino Study: Report of the Neutrino Astrophysics and Cosmology Working Group
, astro-ph/0412544
, The suddenly halted core collapse rebounds and produces a shock wave that stalls within millisecondsJOURNAL
, Myra, E. S.
, Burrows, A.
, 1990
, Neutrinos from type II supernovae- The first 100 milliseconds
, Astrophysical Journal
, 364, 222–231
, 1990ApJ...364..222M
, 10.1086/169405
, in the outer core as energy is lost through the dissociation of heavy elements. A process that is {{As of|2010|alt=not clearly understood}} is necessary to allow the outer layers of the core to reabsorb around 1044 joules (1 foe) from the neutrino pulse, producing the visible brightness, although there are also other theories on how to power the explosion.Some material from the outer envelope falls back onto the neutron star, and for cores beyond about {{Solar mass|8}} there is sufficient fallback to form a black hole. This fallback will reduce the kinetic energy created and the mass of expelled radioactive material, but in some situations it may also generate relativistic jets that result in a gamma-ray burst or an exceptionally luminous supernova.Collapse of massive non-degenerate cores will ignite further fusion. When the core collapse is initiated by pair instability, oxygen fusion begins and the collapse may be halted. For core masses of {{Solar mass|40–60}}, the collapse halts and the star remains intact, but core collapse will occur again when a larger core has formed. For cores of around {{Solar mass|60–130}}, the fusion of oxygen and heavier elements is so energetic that the entire star is disrupted, causing a supernova. At the upper end of the mass range, the supernova is unusually luminous and extremely long-lived due to many solar masses of ejected 56Ni. For even larger core masses, the core temperature becomes high enough to allow photodisintegration and the core collapses completely into a black hole.JOURNAL
, Kasen, D.
, Woosley, S. E.
, Heger, A.
, 2011
, Pair Instability Supernovae: Light Curves, Spectra, and Shock Breakout
, The Astrophysical Journal
, 734, 2, 102
, 1101.3336
, 2011ApJ...734..102K
, 10.1088/0004-637X/734/2/102
,

Type II

missing image!
- SN 1997D.jpg -
The atypical subluminous Type II SN 1997D
Stars with initial masses less than about eight times the sun never develop a core large enough to collapse and they eventually lose their atmospheres to become white dwarfs. Stars with at least {{Solar mass|9}} (possibly as much as {{Solar mass|12}}JOURNAL
, Poelarends, A. J. T.
, Herwig, F.
, Langer, N.
, Heger, A.
, 2008
, The Supernova Channel of Super‐AGB Stars
, The Astrophysical Journal
, 675, 1, 614–625
, 0705.4643
, 2008ApJ...675..614P
, 10.1086/520872
, ) evolve in a complex fashion, progressively burning heavier elements at hotter temperatures in their cores.JOURNAL
, Woosley, S. E.
, Janka, H.-T.
, 2005
, The Physics of Core-Collapse Supernovae
, Nature Physics
, 1, 3, 147–154
, astro-ph/0601261
, 2005NatPh...1..147W
, 10.1038/nphys172, 10.1.1.336.2176
,
JOURNAL
, Gilmore, G.
, 2004
, ASTRONOMY: The Short Spectacular Life of a Superstar
, Science (journal), Science
, 304, 5679, 1915–1916
, 10.1126/science.1100370
, 15218132
, The star becomes layered like an onion, with the burning of more easily fused elements occurring in larger shells.BOOK
, Faure, G.
, Mensing, T. M.
, 2007
, Life and Death of Stars
, Introduction to Planetary Science
, 35–48
, 10.1007/978-1-4020-5544-7_4
, 978-1-4020-5233-0
, Although popularly described as an onion with an iron core, the least massive supernova progenitors only have oxygen-neon(-magnesium) cores. These super AGB stars may form the majority of core collapse supernovae, although less luminous and so less commonly observed than those from more massive progenitors.If core collapse occurs during a supergiant phase when the star still has a hydrogen envelope, the result is a Type II supernova. The rate of mass loss for luminous stars depends on the metallicity and luminosity. Extremely luminous stars at near solar metallicity will lose all their hydrogen before they reach core collapse and so will not form a Type II supernova. At low metallicity, all stars will reach core collapse with a hydrogen envelope but sufficiently massive stars collapse directly to a black hole without producing a visible supernova.Stars with an initial mass up to about 90 times the sun, or a little less at high metallicity, are expected to result in a Type II-P supernova which is the most commonly observed type. At moderate to high metallicity, stars near the upper end of that mass range will have lost most of their hydrogen when core collapse occurs and the result will be a Type II-L supernova. At very low metallicity, stars of around {{Solar mass|140–250}} will reach core collapse by pair instability while they still have a hydrogen atmosphere and an oxygen core and the result will be a supernova with Type II characteristics but a very large mass of ejected 56Ni and high luminosity.

Type Ib and Ic

Image:Supernova 2008D.jpg|thumb|upright=1.2|SN 2008D, a Type IbJOURNAL
, Malesani, D.
, Fynbo, J. P. U.
, Hjorth, J.
, Leloudas, G.
, Sollerman, J.
, Stritzinger, M. D.
, Vreeswijk, P. M.
, Watson, D. J.
, Gorosabel, J.
, Michałowski, M. J.
, Thöne, C. C.
, Augusteijn, T.
, Bersier, D.
, Jakobsson, P.
, Jaunsen, A. O.
, Ledoux, C.
, Levan, A. J.
, Milvang-Jensen, B.
, Rol, E.
, Tanvir, N. R.
, Wiersema, K.
, Xu, D.
, Albert, L.
, Bayliss, M. B.
, Gall, C.
, Grove, L. F.
, Koester, B. P.
, Leitet, E.
, Pursimo, T.
, Skillen, I.
, 1
, 2009
, Early Spectroscopic Identification of SN 2008D
, The Astrophysical Journal Letters
, 692, 2, L84
, 0805.1188
, 2009ApJ...692L..84M
, 10.1088/0004-637X/692/2/L84
, supernova, shown in X-ray (left) and visible light (right) at the far upper end of the galaxyJOURNAL
, Svirski, G.
, Nakar, E.
, 2014
, Sn 2008D: A Wolf-Rayet Explosion Through a Thick Wind
, The Astrophysical Journal
, 788, 1, L14
, 1403.3400
, 2014ApJ...788L..14S
, 10.1088/2041-8205/788/1/L14 The Astrophysical JournalThese supernovae, like those of Type II, are massive stars that undergo core collapse. However the stars which become Types Ib and Ic supernovae have lost most of their outer (hydrogen) envelopes due to strong stellar winds or else from interaction with a companion.CONFERENCE
, Pols, O.
, 1997
, Close Binary Progenitors of Type Ib/Ic and IIb/II-L Supernovae
, Leung, K.-C.
, Proceedings of the Third Pacific Rim Conference on Recent Development on Binary Star Research
, 130, 153–158
, ASP Conference Series
, 1997ASPC..130..153P
, These stars are known as Wolf–Rayet stars, and they occur at moderate to high metallicity where continuum driven winds cause sufficiently high mass loss rates. Observations of Type Ib/c supernova do not match the observed or expected occurrence of Wolf–Rayet stars and alternate explanations for this type of core collapse supernova involve stars stripped of their hydrogen by binary interactions. Binary models provide a better match for the observed supernovae, with the proviso that no suitable binary helium stars have ever been observed.JOURNAL
, Eldridge, J. J.
, Fraser, M.
, Smartt, S. J.
, Maund, J. R.
, Crockett, R. Mark
, 2013
, The death of massive stars – II. Observational constraints on the progenitors of Type Ibc supernovae
, Monthly Notices of the Royal Astronomical Society
, 436, 1, 774
, 1301.1975
, 2013MNRAS.436..774E
, 10.1093/mnras/stt1612
, Since a supernova can occur whenever the mass of the star at the time of core collapse is low enough not to cause complete fallback to a black hole, any massive star may result in a supernova if it loses enough mass before core collapse occurs.Type Ib supernovae are the more common and result from Wolf–Rayet stars of Type WC which still have helium in their atmospheres. For a narrow range of masses, stars evolve further before reaching core collapse to become WO stars with very little helium remaining and these are the progenitors of Type Ic supernovae.A few percent of the Type Ic supernovae are associated with gamma-ray bursts (GRB), though it is also believed that any hydrogen-stripped Type Ib or Ic supernova could produce a GRB, depending on the circumstances of the geometry.JOURNAL
, Ryder, S. D.
, Sadler, E. M.
, Subrahmanyan, R.
, Weiler, K. W.
, Panagia, N.
, Stockdale, C. J.
, 1
, 2004
, Modulations in the radio light curve of the Type IIb supernova 2001ig: evidence for a Wolf-Rayet binary progenitor?
, Monthly Notices of the Royal Astronomical Society
, 349, 3, 1093–1100
, astro-ph/0401135
, 2004MNRAS.349.1093R
, 10.1111/j.1365-2966.2004.07589.x
, The mechanism for producing this type of GRB is the jets produced by the magnetic field of the rapidly spinning magnetar formed at the collapsing core of the star. The jets would also transfer energy into the expanding outer shell, producing a super-luminous supernova.JOURNAL
, Inserra, C.
, Smartt, S. J.
, Jerkstrand, A.
, Valenti, S.
, Fraser, M.
, Wright, D.
, Smith, K.
, Chen, T.-W.
, Kotak, R.
, Pastorello, A.
, Nicholl, M.
, Bresolin, S. F.
, Kudritzki, R. P.
, Benetti, S.
, Botticella, M. T.
, Burgett, W. S.
, Chambers, K. C.
, Ergon, M.
, Flewelling, H.
, Fynbo, J. P. U.
, Geier, S.
, Hodapp, K. W.
, Howell, D. A.
, Huber, M.
, Kaiser, N.
, Leloudas, G.
, Magill, L.
, Magnier, E. A.
, McCrum, M. G.
, Metcalfe, N.
, Price, P. A.
, Rest, A.
, Sollerman, J.
, Sweeney, W.
, Taddia, F.
, Taubenberger, S.
, Tonry, J. L.
, Wainscoat, R. J.
, Waters, C.
, Young, D.
, 1
, 2013
, Super-luminous Type Ic Supernovae: Catching a Magnetar by the Tail
, The Astrophysical Journal
, 770, 2, 28
, 1304.3320
, 2013ApJ...770..128I
, 10.1088/0004-637X/770/2/128
, JOURNAL
, Nicholl, M.
, Smartt, S. J.
, Jerkstrand, A.
, Inserra, C.
, McCrum, M.
, Kotak, R.
, Fraser, M.
, Wright, D.
, Chen, T. W.
, Smith, K.
, Young, D. R.
, Sim, S. A.
, Valenti, S.
, Howell, D. A.
, Bresolin, F.
, Kudritzki, R. P.
, Tonry, J. L.
, Huber, M. E.
, Rest, A.
, Pastorello, A.
, Tomasella, L.
, Cappellaro, E.
, Benetti, S.
, Mattila, S.
, Kankare, E.
, Kangas, T.
, Leloudas, G.
, Sollerman, J.
, Taddia, F.
, Berger, E.
, 1
, 2013
, Slowly fading super-luminous supernovae that are not pair-instability explosions
, Nature (journal), Nature
, 502, 7471, 346–349
, 1310.4446
, 2013Natur.502..346N
, 10.1038/nature12569
, 24132291
, Ultra-stripped supernovae occur when the exploding star has been stripped (almost) all the way to the metal core, via mass transfer in a close binary.JOURNAL
, 2013
, T. M., Tauris
, N., Langer
, T. J., Moriya
, P., Podsiadlowski
, S.-C., Yoon
, S. I., Blinnikov
, Ultra-stripped Type Ic supernovae from close binary evolution
, Astrophysical Journal Letters
, 778
, 2, L23, 1310.6356
, 2013ApJ...778L..23T
, 10.1088/2041-8205/778/2/L23
, As a result, very little material is ejected from the exploding star (c. {{solar mass|0.1}}). In the most extreme cases, ultra-stripped supernovae can occur in naked metal cores, barely above the Chandrasekhar mass limit. SN 2005ekJOURNAL
, 2013
, M. R., Drout
, A. M., Soderberg
, P. A., Mazzali
, J. T., Parrent
, R., Margutti
, D., Milisavljevic
, N. E., Sanders
, R., Chornock
, R. J., Foley
, R. P., Kirshner
, A. V., Filippenko
, W., Li
, P. J., Brown
, S. B., Cenko
, S., Chakraborti
, P., Challis
, A., Friedman
, M., Ganeshalingam
, M., Hicken
, C., Jensen
, M., Modjaz
, H. B., Perets
, J. M., Silverman
, D. S., Wong
, The Fast and Furious Decay of the Peculiar Type Ic Supernova 2005ek
, Astrophysical Journal
, 774, 58, 44
, 1306.2337
, 2013ApJ...774...58D
, 10.1088/0004-637X/774/1/58
, might be an observational example of an ultra-stripped supernova, giving rise to a relatively dim and fast decaying light curve. The nature of ultra-stripped supernovae can be both iron core-collapse and electron capture supernovae, depending on the mass of the collapsing core.

Failed

The core collapse of some massive stars may not result in a visible supernova. The main model for this is a sufficiently massive core that the kinetic energy is insufficient to reverse the infall of the outer layers onto a black hole. These events are difficult to detect, but large surveys have detected possible candidates.JOURNAL, Reynolds, T. M., Fraser, M., Gilmore, G., Gone without a bang: an archivalHSTsurvey for disappearing massive stars, Monthly Notices of the Royal Astronomical Society, 453, 3, 2015, 2886–2901, 10.1093/mnras/stv1809, 1507.05823, 2015MNRAS.453.2885R, GERKE >FIRST1=J. R.FIRST2=C. S.FIRST3=K. Z., The search for failed supernovae with the Large Binocular Telescope: first candidates, Monthly Notices of the Royal Astronomical Societyissue=3 pages=3289–3305
, 10.1093/mnras/stv776, 1411.1761, 2015MNRAS.450.3289G, The red supergiant N6946-BH1 in NGC 6946 underwent a modest outburst in March 2009, before fading from view. Only a faint infrared source remains at the star's location.

Light curves

missing image!
- Comparative supernova type light curves.png -
Comparative supernova type light curves
A historic puzzle concerned the source of energy that can maintain the optical supernova glow for months. Although the energy that disrupts each type of supernovae is delivered promptly, the light curves are mostly dominated by subsequent radioactive heating of the rapidly expanding ejecta. Some have considered rotational energy from the central pulsar. The ejecta gases would dim quickly without some energy input to keep it hot. The intensely radioactive nature of the ejecta gases, which is now known to be correct for most supernovae, was first calculated on sound nucleosynthesis grounds in the late 1960s.JOURNAL, 10.1103/PhysRevLett.20.161, Nucleosynthesis During Silicon Burning, Physical Review Letters, 20, 4, 161, 1968, Bodansky, D., Clayton, D. D., Fowler, W. A., 1968PhRvL..20..161B, It was not until SN 1987A that direct observation of gamma-ray lines unambiguously identified the major radioactive nuclei.JOURNAL, 1988Natur.331..416M, Gamma-ray line emission from SN1987A, Nature, 331, 6155, 416, Matz, S. M., Share, G. H., Leising, M. D., Chupp, E. L., Vestrand, W. T., Purcell, W.R., Strickman, M.S., Reppin, C., 1988, 10.1038/331416a0, It is now known by direct observation that much of the light curve (the graph of luminosity as a function of time) after the occurrence of a Type II Supernova, such as SN 1987A, is explained by those predicted radioactive decays. Although the luminous emission consists of optical photons, it is the radioactive power absorbed by the ejected gases that keeps the remnant hot enough to radiate light. The radioactive decay of 56Ni through its daughters 56Co to 56Fe produces gamma-ray photons, primarily of 847keV and 1238keV, that are absorbed and dominate the heating and thus the luminosity of the ejecta at intermediate times (several weeks) to late times (several months).JOURNAL, 0910.1590, 2009ApJ...703.2205K, 10.1088/0004-637X/703/2/2205, Type Ii Supernovae: Model Light Curves and Standard Candle Relationships, The Astrophysical Journal, 703, 2, 2205, 2009, Kasen, D., Woosley, S. E., Energy for the peak of the light curve of SN1987A was provided by the decay of 56Ni to 56Co (half life 6 days) while energy for the later light curve in particular fit very closely with the 77.3 day half-life of 56Co decaying to 56Fe. Later measurements by space gamma-ray telescopes of the small fraction of the 56Co and 57Co gamma rays that escaped the SN 1987A remnant without absorption confirmed earlier predictions that those two radioactive nuclei were the power sources.The visual light curves of the different supernova types all depend at late times on radioactive heating, but they vary in shape and amplitude because of the underlying mechanisms, the way that visible radiation is produced, the epoch of its observation, and the transparency of the ejected material. The light curves can be significantly different at other wavelengths. For example, at ultraviolet wavelengths there is an early extremely luminous peak lasting only a few hours corresponding to the breakout of the shock launched by the initial event, but that breakout is hardly detectable optically.The light curves for Type Ia are mostly very uniform, with a consistent maximum absolute magnitude and a relatively steep decline in luminosity. Their optical energy output is driven by radioactive decay of ejected nickel-56 (half life 6 days), which then decays to radioactive cobalt-56 (half life 77 days). These radioisotopes excite the surrounding material to incandescence. Studies of cosmology today rely on 56Ni radioactivity providing the energy for the optical brightness of supernovae of Type Ia, which are the "standard candles" of cosmology but whose diagnostic 847keV and 1238keV gamma rays were first detected only in 2014.JOURNAL, 10.1038/nature13672, 25164750, Cobalt-56 γ-ray emission lines from the Type Ia supernova 2014J, Nature, 512, 7515, 406–8, 2014, Churazov, E., Sunyaev, R., Isern, J., Knödlseder, J., Jean, P., Lebrun, F., Chugai, N., Grebenev, S., Bravo, E., Sazonov, S., Renaud, M., 1405.3332, 2014Natur.512..406C, The initial phases of the light curve decline steeply as the effective size of the photosphere decreases and trapped electromagnetic radiation is depleted. The light curve continues to decline in the B band while it may show a small shoulder in the visual at about 40 days, but this is only a hint of a secondary maximum that occurs in the infra-red as certain ionised heavy elements recombine to produce infra-red radiation and the ejecta become transparent to it. The visual light curve continues to decline at a rate slightly greater than the decay rate of the radioactive cobalt (which has the longer half life and controls the later curve), because the ejected material becomes more diffuse and less able to convert the high energy radiation into visual radiation. After several months, the light curve changes its decline rate again as positron emission becomes dominant from the remaining cobalt-56, although this portion of the light curve has been little-studied.Type Ib and Ic light curves are basically similar to Type Ia although with a lower average peak luminosity. The visual light output is again due to radioactive decay being converted into visual radiation, but there is a much lower mass of the created nickel-56. The peak luminosity varies considerably and there are even occasional Type Ib/c supernovae orders of magnitude more and less luminous than the norm. The most luminous Type Ic supernovae are referred to as hypernovae and tend to have broadened light curves in addition to the increased peak luminosity. The source of the extra energy is thought to be relativistic jets driven by the formation of a rotating black hole, which also produce gamma-ray bursts.The light curves for Type II supernovae are characterised by a much slower decline than Type I, on the order of 0.05 magnitudes per day,JOURNAL, 1979A&A....72..287B, Photometric properties of type II supernovae, Astronomy and Astrophysicspages=287first1=R.first2=F.first3=L., 1979, excluding the plateau phase. The visual light output is dominated by kinetic energy rather than radioactive decay for several months, due primarily to the existence of hydrogen in the ejecta from the atmosphere of the supergiant progenitor star. In the initial destruction this hydrogen becomes heated and ionised. The majority of Type II supernovae show a prolonged plateau in their light curves as this hydrogen recombines, emitting visible light and becoming more transparent. This is then followed by a declining light curve driven by radioactive decay although slower than in Type I supernovae, due to the efficiency of conversion into light by all the hydrogen.In Type II-L the plateau is absent because the progenitor had relatively little hydrogen left in its atmosphere, sufficient to appear in the spectrum but insufficient to produce a noticeable plateau in the light output. In Type IIb supernovae the hydrogen atmosphere of the progenitor is so depleted (thought to be due to tidal stripping by a companion star) that the light curve is closer to a Type I supernova and the hydrogen even disappears from the spectrum after several weeks.Type IIn supernovae are characterised by additional narrow spectral lines produced in a dense shell of circumstellar material. Their light curves are generally very broad and extended, occasionally also extremely luminous and referred to as a superluminous supernova. These light curves are produced by the highly efficient conversion of kinetic energy of the ejecta into electromagnetic radiation by interaction with the dense shell of material. This only occurs when the material is sufficiently dense and compact, indicating that it has been produced by the progenitor star itself only shortly before the supernova occurs.Large numbers of supernovae have been catalogued and classified to provide distance candles and test models. Average characteristics vary somewhat with distance and type of host galaxy, but can broadly be specified for each supernova type.{|class="wikitable" style="max-width: 600px"absolute magnitude{{ref|b|b}} !!Approximate energy (foe){{ref|c|c}} !!Days to peak luminosity !!Days from peak to 10% luminosity−19 style="text-align:right"approx. 19 style="text-align:right"|around 60around −15 style="text-align:right"15–25 style="text-align:right"|unknownaround −17 style="text-align:right"15–25 style="text-align:right"|40–100around −16 style="text-align:right"15–25 style="text-align:right"|40–100to −22 style="text-align:right"roughly 25 style="text-align:right"|roughly 100around −17 style="text-align:right"around 20 style="text-align:right"|around 100around −17 style="text-align:right"around 13 style="text-align:right"|around 150around −14 style="text-align:right"roughly 15 style="text-align:right"|unknownaround −16 style="text-align:right"around 15 style="text-align:right"|Plateau then around 50daround −17 style="text-align:right"12–30 or more style="text-align:right"|50–150to −22 style="text-align:right"above 50 style="text-align:right"|above 100Notes:{{Plainlist|
  • a. {{note|a}}Faint types may be a distinct sub-class. Bright types may be a continuum from slightly over-luminous to hypernovae.
  • b. {{note|b}}These magnitudes are measured in the R band. Measurements in V or B bands are common and will be around half a magnitude brighter for supernovae.
  • c. {{note|c}}Order of magnitude kinetic energy. Total electromagnetic radiated energy is usually lower, (theoretical) neutrino energy much higher.
  • d. {{note|d}}Probably a heterogeneous group, any of the other types embedded in nebulosity.
}}

Asymmetry

Image:Chandra-crab.jpg|thumb|The pulsar in the Crab nebula is travelling at 375 km/s relative to the nebula.JOURNAL
, Frail, D. A.
, Giacani, E. B.
, Goss, W. Miller
, Dubner, G. M.
, 1996
, The Pulsar Wind Nebula Around PSR B1853+01 in the Supernova Remnant W44
, Astrophysical Journal LettersAstrophysical Journal Letters
A long-standing puzzle surrounding Type II supernovae is why the remaining compact object receives a large velocity away from the epicentre;BOOK
, Höflich, P. A.
, Kumar, P.
, Wheeler, J. Craig
, 2004
, Neutron star kicks and supernova asymmetry
, Cosmic explosions in three dimensions: Asymmetries in supernovae and gamma-ray bursts
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, 276
, Cambridge University Press
, 2004cetd.conf..276Lpulsars, and thus neutron stars, are observed to have high velocities, and black holes presumably do as well, although they are far harder to observe in isolation. The initial impetus can be substantial, propelling an object of more than a solar mass at a velocity of 500 km/s or greater. This indicates an expansion asymmetry, but the mechanism by which momentum is transferred to the compact object {{As of>2010|alt=remains}} a puzzle. Proposed explanations for this kick include convection in the collapsing star and jet production during neutron star formation.
One possible explanation for this asymmetry is a large-scale convection above the core. The convection can create variations in the local abundances of elements, resulting in uneven nuclear burning during the collapse, bounce and resulting expansion.JOURNAL
, Fryer, C. L.
, 2004
, Neutron Star Kicks from Asymmetric Collapse
, Astrophysical Journal
, 601, 2, L175–L178
, 2004ApJ...601L.175F
, 10.1086/382044, astro-ph/0312265,
Another possible explanation is that accretion of gas onto the central neutron star can create a disk that drives highly directional jets, propelling matter at a high velocity out of the star, and driving transverse shocks that completely disrupt the star. These jets might play a crucial role in the resulting supernova.JOURNAL, Implications of turbulence for jets in core-collapse supernova explosionsfirst1=A.first2=N., 2014, 1412.4984
, 10.1088/0004-637X/806/1/28
, 806
, 1, The Astrophysical Journal
, 28
, 2015ApJ...806...28G, JOURNAL, 10.1086/312305, Jet-induced Explosions of Core Collapse Supernovae, The Astrophysical Journal
issue=2 year=1999first1=A. M.first2=P. A.first3=E. S.first4=J. Craigfirst5=L.first6=A. Yu.bibcode=1999ApJ...524L.107K, astro-ph/9904419, (A similar model is now favored for explaining long gamma-ray bursts.)Initial asymmetries have also been confirmed in Type Ia supernovae through observation. This result may mean that the initial luminosity of this type of supernova depends on the viewing angle. However, the expansion becomes more symmetrical with the passage of time. Early asymmetries are detectable by measuring the polarization of the emitted light.JOURNAL, 10.1086/375444, Spectropolarimetry of SN 2001el in NGC 1448: Asphericity of a Normal Type Ia Supernova, The Astrophysical Journalissue=2, 1110–1128, 2003first1=L.first2=D.first3=P. A.first4=A. M.first5=J. C.first6=D.first7=P. E.first8=S. A.first9=C.first10=P.bibcode=2003ApJ...591.1110W, astro-ph/0303397,

Energy output

missing image!
- SNIacurva.png -
The radioactive decays of nickel-56 and cobalt-56 that produce a supernova visible light curve
Although we are used to thinking of supernovae primarily as luminous visible events, the electromagnetic radiation they release is almost a minor side-effect. Particularly in the case of core collapse supernovae, the emitted electromagnetic radiation is a tiny fraction of the total energy released during the event.There is a fundamental difference between the balance of energy production in the different types of supernova. In Type Ia white dwarf detonations, most of the energy is directed into heavy element synthesis and the kinetic energy of the ejecta. In core collapse supernovae, the vast majority of the energy is directed into neutrino emission, and while some of this apparently powers the observed destruction, 99%+ of the neutrinos escape the star in the first few minutes following the start of the collapse.Type Ia supernovae derive their energy from a runaway nuclear fusion of a carbon-oxygen white dwarf. The details of the energetics are still not fully understood, but the end result is the ejection of the entire mass of the original star at high kinetic energy. Around half a solar mass of that mass is 56Ni generated from silicon burning. 56Ni is radioactive and decays into 56Co by beta plus decay (with a half life of six days) and gamma rays. 56Co itself decays by the beta plus (positron) path with a half life of 77 days into stable 56Fe. These two processes are responsible for the electromagnetic radiation from Type Ia supernovae. In combination with the changing transparency of the ejected material, they produce the rapidly declining light curve.Core collapse supernovae are on average visually fainter than Type Ia supernovae, but the total energy released is far higher. In these type of supernovae, the gravitational potential energy is converted into kinetic energy that compresses and collapses the core, initially producing electron neutrinos from disintegrating nucleons, followed by all flavours of thermal neutrinos from the super-heated neutron star core. Around 1% of these neutrinos are thought to deposit sufficient energy into the outer layers of the star to drive the resulting catastrophe, but again the details cannot be reproduced exactly in current models. Kinetic energies and nickel yields are somewhat lower than Type Ia supernovae, hence the lower peak visual luminosity of Type II supernovae, but energy from the de-ionisation of the many solar masses of remaining hydrogen can contribute to a much slower decline in luminosity and produce the plateau phase seen in the majority of core collapse supernovae.{|class="wikitable"|+Energetics of supernovae!Supernova !!Approximate total energy1044 joules (foe){{ref|c|c}} !!Ejected Ni(solar masses) !!Neutrino energy(foe) !!Kinetic energy(foe) !!Electromagnetic radiation(foe)LAST2=NOMOTO LAST3=CAPPELLARO LAST4=NAKAMURA LAST5=UMEDA LAST6=IWAMOTO DOI=10.1086/318428 JOURNAL=THE ASTROPHYSICAL JOURNAL ISSUE=2 YEAR=2001 PMC=BIBCODE=2001APJ...547..988M CHAPTER=NEUTRINO EMISSION FROM TYPE IA SUPERNOVAE TITLE=AIP CONFERENCE PROCEEDINGS PAGES=406–408 PMID=LAST2=GARNAVICH LAST3=KESSLER LAST4=FRIEMAN LAST5=JHA LAST6=BASSETT LAST7=CINABRO LAST8=DILDAY LAST9=KASEN LAST10=MARRINER LAST11=NICHOL LAST12=RIESS LAST13=SAKO LAST14=SCHNEIDER LAST15=SMITH LAST16=SOLLERMAN TITLE=THE RISE AND FALL OF TYPE IA SUPERNOVA LIGHT CURVES IN THE SDSS-II SUPERNOVA SURVEYJOURNAL=THE ASTROPHYSICAL JOURNAL ISSUE=1 YEAR=2010 PMC=BIBCODE=2010APJ...712..350H, style="text-align:right"0.4 – 0.8 style="text-align:right"1.3 – 1.4 style="text-align:right"|~0.01JOURNAL=ANNUAL REVIEW OF NUCLEAR AND PARTICLE SCIENCEISSUE=1AUTHOR1=JANKAYEAR=2012ARXIV=1206.2503, SMARTT>TITLE=PROGENITORS OF CORE-COLLAPSE SUPERNOVAEPAGES=63–106JOURNAL=ANNUAL REVIEW OF ASTRONOMY AND ASTROPHYSICSDOI=10.1146/ANNUREV-ASTRO-082708-101737100 style="text-align:right"100 style="text-align:right"0.001 – 0.01100 style="text-align:right"1–100 style="text-align:right"~0.15–100 style="text-align:right"low? style="text-align:right"0.01 – 0.1In some core collapse supernovae, fallback onto a black hole drives relativistic jets which may produce a brief energetic and directional burst of gamma rays and also transfers substantial further energy into the ejected material. This is one scenario for producing high luminosity supernovae and is thought to be the cause of Type Ic hypernovae and long duration gamma-ray bursts. If the relativistic jets are too brief and fail to penetrate the stellar envelope then a low luminosity gamma-ray burst may be produced and the supernova may be sub-luminous.When a supernova occurs inside a small dense cloud of circumstellar material, it will produce a shock wave that can efficiently convert a high fraction of the kinetic energy into electromagnetic radiation. Even though the initial energy was entirely normal the resulting supernova will have high luminosity and extended duration since it does not rely on exponential radioactive decay. This type of event may cause Type IIn hypernovae.Although pair-instability supernovae are core collapse supernovae with spectra and light curves similar to Type II-P, the nature after core collapse is more like that of a giant Type Ia with runaway fusion of carbon, oxygen, and silicon. The total energy released by the highest mass events is comparable to other core collapse supernovae but neutrino production is thought to be very low, hence the kinetic and electromagnetic energy released is very high. The cores of these stars are much larger than any white dwarf and the amount of radioactive nickel and other heavy elements ejected from their cores can be orders of magnitude higher, with consequently high visual luminosity.

Progenitor

(File:Artist's impression time-lapse of distant supernovae.webm|thumb|Shown in this sped-up artist's impression, is a collection of distant galaxies, the occasional supernova can be seen. Each of these exploding stars briefly rivals the brightness of its host galaxy.)The supernova classification type is closely tied to the type of star at the time of the collapse. The occurrence of each type of supernova depends dramatically on the metallicity, and hence the age of the host galaxy.Type Ia supernovae are produced from white dwarf stars in binary systems and occur in all galaxy types. Core collapse supernovae are only found in galaxies undergoing current or very recent star formation, since they result from short-lived massive stars. They are most commonly found in Type Sc spirals, but also in the arms of other spiral galaxies and in irregular galaxies, especially starburst galaxies.Type Ib/c and II-L, and possibly most Type IIn, supernovae are only thought to be produced from stars having near-solar metallicity levels that result in high mass loss from massive stars, hence they are less common in older, more-distant galaxies. The table shows the expected progenitor for the main types of core collapse supernova, and the approximate proportions that have been observed in the local neighbourhood.{|class="wikitable"|+ Fraction of core collapse supernovae types by progenitor! Type !! Progenitor star !! FractionWolf–Rayet star>Wolf–Rayet or helium star 9.0%Wolf–Rayet star>Wolf–Rayet 17.0%Supergiant >|55.5%Supergiant with a depleted hydrogen shell >|3.0%Supergiant in a dense cloud of expelled material (such as Luminous blue variable>LBV)2.4%Supergiant with highly depleted hydrogen (stripped by companion?) >|12.1%Blue supergiant? >|1.0%There are a number of difficulties reconciling modelled and observed stellar evolution leading up to core collapse supernovae. Red supergiants are the expected progenitors for the vast majority of core collapse supernovae, and these have been observed but only at relatively low masses and luminosities, below about {{solar mass|18}} and {{solar luminosity|100,000}} respectively. Most progenitors of Type II supernovae are not detected and must be considerably fainter, and presumably less massive. It is now proposed that higher mass red supergiants do not explode as supernovae, but instead evolve back towards hotter temperatures. Several progenitors of Type IIb supernovae have been confirmed, and these were K and G supergiants, plus one A supergiant. Yellow hypergiants or LBVs are proposed progenitors for Type IIb supernovae, and almost all Type IIb supernovae near enough to observe have shown such progenitors.JOURNAL, Walmswell, J. J., Eldridge, J. J., 10.1111/j.1365-2966.2011.19860.x, Circumstellar dust as a solution to the red supergiant supernova progenitor problem, Monthly Notices of the Royal Astronomical Society, 419, 3, 2054, 2012, 1109.4637, 2012MNRAS.419.2054W, JOURNAL, Georgy, C., 10.1051/0004-6361/201118372, Yellow supergiants as supernova progenitors: An indication of strong mass loss for red supergiants?, Astronomy & Astrophysics, 538, L8–L2, 2012, 1111.7003, 2012A&A...538L...8G, Until just a few decades ago, hot supergiants were not considered likely to explode, but observations have shown otherwise. Blue supergiants form an unexpectedly high proportion of confirmed supernova progenitors, partly due to their high luminosity and easy detection, while not a single Wolf–Rayet progenitor has yet been clearly identified.JOURNAL, 2009ARA&A..47...63S, Progenitors of Core-Collapse Supernovae, Annual Review of Astronomy & Astrophysics, 47, 63–106, Smartt, S. J., 2009, 10.1146/annurev-astro-082708-101737, 0908.0700, JOURNAL, Yoon, S. -C., Gräfener, G., Vink, J. S., Kozyreva, A., Izzard, R. G., On the nature and detectability of Type Ib/c supernova progenitors, 10.1051/0004-6361/201219790, Astronomy & Astrophysics, 544, L11, 2012, 1207.3683, 2012A&A...544L..11Y, Models have had difficulty showing how blue supergiants lose enough mass to reach supernova without progressing to a different evolutionary stage. One study has shown a possible route for low-luminosity post-red supergiant luminous blue variables to collapse, most likely as a Type IIn supernova.JOURNAL, Groh, J. H., Meynet, G., Ekström, S., Massive star evolution: Luminous blue variables as unexpected supernova progenitors, 10.1051/0004-6361/201220741, Astronomy & Astrophysics, 550, L7, 2013, 1301.1519, 2013A&A...550L...7G, Several examples of hot luminous progenitors of Type IIn supernovae have been detected: SN 2005gy and SN 2010jl were both apparently massive luminous stars, but are very distant; and SN 2009ip had a highly luminous progenitor likely to have been an LBV, but is a peculiar supernova whose exact nature is disputed.The progenitors of Type Ib/c supernovae are not observed at all, and constraints on their possible luminosity are often lower than those of known WC stars. WO stars are extremely rare and visually relatively faint, so it is difficult to say whether such progenitors are missing or just yet to be observed. Very luminous progenitors have not been securely identified, despite numerous supernovae being observed near enough that such progenitors would have been clearly imaged.JOURNAL, 2012A&A...544L..11Y, On the nature and detectability of Type Ib/c supernova progenitors, Astronomy & Astrophysics, 544, L11, Yoon, S.-C., Gräfener, G., Vink, J. S., Kozyreva, A., Izzard, R. G., 2012, 10.1051/0004-6361/201219790, 1207.3683, Population modelling shows that the observed Type Ib/c supernovae could be reproduced by a mixture of single massive stars and stripped-envelope stars from interacting binary systems. The continued lack of unambiguous detection of progenitors for normal Type Ib and Ic supernovae may be due to most massive stars collapsing directly to a black hole without a supernova outburst. Most of these supernovae are then produced from lower-mass low-luminosity helium stars in binary systems. A small number would be from rapidly-rotating massive stars, likely corresponding to the highly-energetic Type Ic-BL events that are associated with long-duration gamma-ray bursts.

Interstellar impact

Source of heavy elements

File:An isolated neutron star in the Small Magellanic Cloud.jpg|thumb|Isolated neutron star in the Small Magellanic CloudSmall Magellanic CloudSupernovae are the major source of elements heavier than nitrogen.JOURNAL
, François, P.
, 2004
, The evolution of the Milky Way from its earliest phases: Constraints on stellar nucleosynthesis
, Astronomy and Astrophysics
, 421, 2, 613–621
, 10.1051/0004-6361:20034140
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, Matteucci
, F.
, Cayrel
, R.
, Spite
, M.
, Spite
, F.
, Chiappini
, C., These elements are produced by nuclear fusion for nuclei up to 34S, by silicon photodisintegration rearrangement and quasiequilibrium (see Supernova nucleosynthesis) during silicon burning for nuclei between 36Ar and 56Ni, and by rapid captures of neutrons during the supernova's collapse for elements heavier than iron. Nucleosynthesis during silicon burning yields nuclei roughly 1000-100,000 times more abundant than the r-process isotopes heavier than iron.
JOURNAL
, Woosley, S. E.
, Arnett, W. D.
, Clayton, D. D.
, 1973
, The Explosive Burning of Oxygen and Silicon
, Astrophysical Journal Supplement
, 26, 231–312
, 1973ApJS...26..231W
, 10.1086/190282
, Supernovae are the most likely, although not undisputed, candidate sites for the r-process, which is the rapid capture of neutrons that occurs at high temperature and high density of neutrons. Those reactions produce highly unstable nuclei that are rich in neutrons and that rapidly beta decay into more stable forms. The r-process produces about half of all the heavier isotopes of the elements beyond iron, including plutonium and uranium.JOURNAL
, Qian, Y.-Z.
, Vogel, P.
, Wasserburg, G. J.
, 1998
, Diverse Supernova Sources for the r-Process
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, 494, 1, 285–296
, 1998ApJ...494..285Q
, 10.1086/305198, astro-ph/9706120, The only other major competing process for producing elements heavier than iron is the s-process in large, old, red-giant AGB stars, which produces these elements slowly over longer epochs and which cannot produce elements heavier than lead.
JOURNAL, 2001Icar..152..185G, The Galactic Habitable Zone: Galactic Chemical Evolution, Icarus, 152, 1, 185, Gonzalez, G., Brownlee, D., Ward, P., 2001, 10.1006/icar.2001.6617, astro-ph/0103165,

Role in stellar evolution

Remnants of many supernovae consist of a compact object and a rapidly expanding shock wave of material. This cloud of material sweeps up the surrounding interstellar medium during a free expansion phase, which can last for up to two centuries. The wave then gradually undergoes a period of adiabatic expansion, and will slowly cool and mix with the surrounding interstellar medium over a period of about 10,000 years.JOURNAL, 1972ApJ...178..159C, Cooling and Evolution of a Supernova Remnant, Astrophysical Journal, 178, 159, Cox, D. P., 1972, 10.1086/151775,
missing image!
- STScl-2005-15.png -
Supernova remnant N 63A lies within a clumpy region of gas and dust in the Large Magellanic Cloud.
The Big Bang produced hydrogen, helium, and traces of lithium, while all heavier elements are synthesized in stars and supernovae. Supernovae tend to enrich the surrounding interstellar medium with elements other than hydrogen and helium, which usually astronomers refer to as "metals".These injected elements ultimately enrich the molecular clouds that are the sites of star formation.JOURNAL, 10.1088/0004-637X/696/2/2138, Measuring Dust Production in the Small Magellanic Cloud Core-Collapse Supernova Remnant 1E 0102.2–7219, The Astrophysical Journal, 696, 2, 2138–2154, 2009, Sandstrom, K. M., Bolatto, A. D., Stanimirović, S., Van Loon, J. Th., Smith, J. D. T., 2009ApJ...696.2138S, 0810.2803, Thus, each stellar generation has a slightly different composition, going from an almost pure mixture of hydrogen and helium to a more metal-rich composition. Supernovae are the dominant mechanism for distributing these heavier elements, which are formed in a star during its period of nuclear fusion. The different abundances of elements in the material that forms a star have important influences on the star's life, and may decisively influence the possibility of having planets orbiting it.The kinetic energy of an expanding supernova remnant can trigger star formation by compressing nearby, dense molecular clouds in space.JOURNAL
, 2001ASPC..243..791Ptitle=Triggered Star Formation in the Scorpius-Centaurus OB Association (Sco OB2)
volume=243 author1=Preibisch last2=Zinnecker year=2001, The increase in turbulent pressure can also prevent star formation if the cloud is unable to lose the excess energy.JOURNAL, 1983A&A...128..411K, The interaction of supernova shockfronts and nearby interstellar clouds, Astronomy and Astrophysicspages=411first1=J.first2=W., 1983, Evidence from daughter products of short-lived radioactive isotopes shows that a nearby supernova helped determine the composition of the Solar System 4.5 billion years ago, and may even have triggered the formation of this system.JOURNAL, 10.1016/0019-1035(77)90101-4, The supernova trigger for formation of the solar system, Icarus, 30, 3, 447, 1977, Cameron, A.G.W., Truran, J.W., 1977Icar...30..447C, Supernova production of heavy elements over astronomic periods of time ultimately made the chemistry of life on Earth possible.{{clear}}

Effect on Earth

A near-Earth supernova is a supernova close enough to the Earth to have noticeable effects on its biosphere. Depending upon the type and energy of the supernova, it could be as far as 3000 light-years away. Gamma rays from a supernova would induce a chemical reaction in the upper atmosphere converting molecular nitrogen into nitrogen oxides, depleting the ozone layer enough to expose the surface to harmful ultraviolet solar radiation. This has been proposed as the cause of the Ordovician–Silurian extinction, which resulted in the death of nearly 60% of the oceanic life on Earth.JOURNAL
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, Did a gamma-ray burst initiate the late Ordovician mass extinction?
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, 10.1017/S1473550404001910, 2004IJAsB...3...55M
, 1
, Lieberman, B. S.
, Laird, C. M.
, Martin, L. D.
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, Thomas, B. C.
, Cannizzo, J. K.
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, Jackman, C. H., 1808/9204
, In 1996 it was theorized that traces of past supernovae might be detectable on Earth in the form of metal isotope signatures in rock strata. Iron-60 enrichment was later reported in deep-sea rock of the Pacific Ocean.JOURNAL, 10.1086/427797, Deep‐Ocean Crusts as Telescopes: Using Live Radioisotopes to Probe Supernova Nucleosynthesis, The Astrophysical Journal, 621, 2, 902–907, 2005, Fields, B. D., Hochmuth, K. A., Ellis, J., 2005ApJ...621..902F, astro-ph/0410525, JOURNAL
, Knie, K.
, 2004
, 60Fe Anomaly in a Deep-Sea Manganese Crust and Implications for a Nearby Supernova Source
, Physical Review Letters
, 93, 17, 171103–171106
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, Korschinek, G.
, Faestermann, T.
, Dorfi, E.
, Rugel, G.
, Wallner, A.
, JOURNAL
, Fields, B. D.
, Ellis, J.
, 1999
, On Deep-Ocean Fe-60 as a Fossil of a Near-Earth Supernova
, New Astronomy (journal), New Astronomy
, 4, 6, 419–430
, astro-ph/9811457
, 10.1016/S1384-1076(99)00034-2
JOURNAL=SCIENTIFIC AMERICANISSUE=5YEAR=2009, 2009SciAm.300e..28., Type Ia supernovae are thought to be potentially the most dangerous if they occur close enough to the Earth. Because these supernovae arise from dim, common white dwarf stars in binary systems, it is likely that a supernova that can affect the Earth will occur unpredictably and in a star system that is not well studied. The closest known candidate is IK Pegasi (see below).JOURNAL
, Gorelick, M.
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, Recent estimates predict that a Type II supernova would have to be closer than eight parsecs (26 light-years) to destroy half of the Earth's ozone layer, and there are no such candidates closer than about 500 light years.JOURNAL
, Gehrels, N.
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, Ozone Depletion from Nearby Supernovae
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, 585, 2, 1169–1176
, astro-ph/0211361
, 10.1086/346127, 2003ApJ...585.1169G
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, Laird, C. M.
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, Chen, W.
,

Milky Way candidates

The next supernova in the Milky Way will likely be detectable even if it occurs on the far side of the galaxy. It is likely to be produced by the collapse of an unremarkable red supergiant and it is very probable that it will already have been catalogued in infrared surveys such as 2MASS. There is a smaller chance that the next core collapse supernova will be produced by a different type of massive star such as a yellow hypergiant, luminous blue variable, or Wolf–Rayet. The chances of the next supernova being a Type Ia produced by a white dwarf are calculated to be about a third of those for a core collapse supernova. Again it should be observable wherever it occurs, but it is less likely that the progenitor will ever have been observed. It isn't even known exactly what a Type Ia progenitor system looks like, and it is difficult to detect them beyond a few parsecs. The total supernova rate in our galaxy is estimated to be between 2 and 12 per century, although we haven't actually observed one for several centuries.JOURNAL
, Adams, S. M.
, Kochanek, C. S.
, Beacom, J. F.
, Vagins, M. R.
, Stanek, K. Z.
, 2013
, Observing the Next Galactic Supernova
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, 778, 2, 164
, 1306.0559
, 2013ApJ...778..164A
, 10.1088/0004-637X/778/2/164
,
missing image!
- Wolf rayet2.jpg -
The nebula around Wolf–Rayet star WR124, which is located at a distance of about 21,000 light years.JOURNAL, 2003A&A...398..181V, The dynamics of the nebula M1-67 around the run-away Wolf-Rayet star WR 124, Astronomy and Astrophysicspages=181–194first1=M. V.first2=H. J. G. L. M., 2003arxiv=astro-ph/0211326,
Statistically, the next supernova is likely to be produced from an otherwise unremarkable red supergiant, but it is difficult to identify which of those supergiants are in the final stages of heavy element fusion in their cores and which have millions of years left. The most-massive red supergiants are expected to shed their atmospheres and evolve to Wolf–Rayet stars before their cores collapse. All Wolf–Rayet stars are expected to end their lives from the Wolf–Rayet phase within a million years or so, but again it is difficult to identify those that are closest to core collapse. One class that is expected to have no more than a few thousand years before exploding are the WO Wolf–Rayet stars, which are known to have exhausted their core helium.JOURNAL, 2015A&A...581A.110T, 1507.00839, Massive stars on the verge of exploding: The properties of oxygen sequence Wolf-Rayet stars, Astronomy & Astrophysics, 581, A110, Tramper, F., Straal, S. M., Sanyal, D., Sana, H., De Koter, A., Gräfener, G., Langer, N., Vink, J. S., De Mink, S. E., Kaper, L., 2015, 10.1051/0004-6361/201425390, Only eight of them are known, and only four of those are in the Milky Way.JOURNAL, 2013A&A...559A..72T, 1310.2849, On the nature of WO stars: A quantitative analysis of the WO3 star DR1 in IC 1613, Astronomy & Astrophysics, 559, A72, Tramper, F., Gräfener, G., Hartoog, O. E., Sana, H., De Koter, A., Vink, J. S., Ellerbroek, L. E., Langer, N., Garcia, M., Kaper, L., De Mink, S. E., 2013, 10.1051/0004-6361/201322155, A number of close or well known stars have been identified as possible core collapse supernova candidates: the red supergiants Antares and Betelgeuse;BOOK, 10.1007/978-3-319-11644-0_12, Star Death: Supernovae, Neutron Stars & Black Holes, Astrophysics is Easy!series=The Patrick Moore Practical Astronomy Series, 2015first1=M., 978-3-319-11643-3, the yellow hypergiant Rho Cassiopeiae;JOURNAL, 2004IAUS..219..903L, Spectroscopy of the Millennium Outburst and Recent Variability of the Yellow Hypergiant Rho Cassiopeiae, Stars as Suns : Activitypages=903first1=A.first2=R. P.first3=G.first4=R. J.first5=I.first6=A. E.arxiv=astro-ph/0312074, 1, the luminous blue variable Eta Carinae that has already produced a supernova impostor;JOURNAL, 2003A&A...410L..37V, Direct measurement of the size and shape of the present-day stellar wind of eta Carinae, Astronomy and Astrophysicsissue=3, L37first1=R.first2=P.first3=M.first4=T.first5=W.first6=A.first7=L. B. F. M.first8=D. J.first9=F.first10=R.first11=A.-M., 1, 2003arxiv=astro-ph/0310399, and the brightest component, a Wolf–Rayet star, in the Regor or Gamma Velorum system,BOOK, 10.1007/978-3-642-12698-7_4, Massive Stars and Their Supernovae, Astronomy with Radioactivitiespages=153, Lecture Notes in Physics, 2011first1=F.-K.first2=R.first3=M.first4=R., 978-3-642-12697-0, Others have gained notoriety as possible, although not very likely, progenitors for a gamma-ray burst; for example WR 104.JOURNAL, 10.1086/527286, The Prototype Colliding‐Wind Pinwheel WR 104, The Astrophysical Journalissue=1, 698–710, 2008first1=P. G.first2=J. D.first3=N.first4=W. C.first5=S. P.first6=K. G.bibcode=2008ApJ...675..698T, 0712.2111, Identification of candidates for a Type Ia supernova is much more speculative. Any binary with an accreting white dwarf might produce a supernova although the exact mechanism and timescale is still debated. These systems are faint and difficult to identify, but the novae and recurrent novae are such systems that conveniently advertise themselves. One example is U Scorpii.CONFERENCE
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, but observations suggest it will be several million years before the white dwarf can accrete the critical mass required to become a Type Ia supernova.JOURNAL, 2008MNRAS.389.1367V, On the empirical evidence for the existence of ultramassive white dwarfs, Monthly Notices of the Royal Astronomical Society, 389, 3, 1367, Vennes, S., Kawka, A., 2008, 10.1111/j.1365-2966.2008.13652.x, 0806.4742,

See also

{{Wikipedia books|Supernovae}}{hide}cmn|colwidth=30em|
  • {{annotated link|List of supernovae{edih}
  • {{annotated link|List of supernova remnants}}
  • {{annotated link|Quark-nova}}
  • {{annotated link|Supernovae in fiction}}
  • {{annotated link|Timeline of white dwarfs, neutron stars, and supernovae}}
}}

References

{{Reflist|30em}}

Notes

{{Notelist}}{{Reflist|group="nb"}}

Further reading

  • WEB


, 2007-10-04
, Introduction to Supernova Remnants
,weblink
, NASA/Goddard Space Flight Center, GSFC
, 2011-03-15
,
  • JOURNAL, 1990PhT....43i..24B, Supernovae, Physics Today, 43, 9, 736–739, H. A., Bethe, 1990, 10.1063/1.881256,
  • BOOK


, Croswell, K.
, Ken Croswell
, 1996
, The Alchemy of the Heavens: Searching for Meaning in the Milky Way
, Anchor Books
, 978-0-385-47214-2
, A popular-science account.
  • JOURNAL, 1997ARA&A..35..309F, Optical Spectra of Supernovae, Annual Review of Astronomy and Astrophysics
pages=309–355first1=A. V., 1997, 10.1146/annurev.astro.35.1.309, An article describing spectral classes of supernovae.
  • JOURNAL


, Takahashi, K.
, Sato, K.
, Burrows, A.
, Thompson, T. A.
, 2003
, Supernova Neutrinos, Neutrino Oscillations, and the Mass of the Progenitor Star
, Physical Review D
, 68, 11, 77–81
, hep-ph/0306056
, 10.1103/PhysRevD.68.113009, 2003PhRvD..68k3009T, A good review of supernova events.
  • JOURNAL


, Hillebrandt, W.
, Janka, H.-T.
, Müller, E.
, 2006
, How to Blow Up a Star
, Scientific American
, 295, 4, 42–49
,weblink
, 10.1038/scientificamerican1006-42, 2006SciAm.295d..42H,
  • JOURNAL


, Woosley, S. E.
, Janka, H.-T.
, 2005
, The Physics of Core-Collapse Supernovae
, Nature Physics
, 1, 3, 147–154
, astro-ph/0601261
, 10.1038/nphys172
, 2005NatPh...1..147W, 10.1.1.336.2176
,

External links

{{Commons category|Supernovae}}
  • WEB


, RSS news feed
,weblink
, The Astronomer's Telegram
, RSS
, 2006-11-28
,
  • WEB


, Tsvetkov, D. Yu.
, Pavlyuk, N. N.
, Bartunov, O. S.
, Pskovskii, Y. P.
, Sternberg Astronomical Institute Supernova Catalogue
,weblink
, Sternberg Astronomical Institute, Moscow University
, 2006-11-28
, A searchable catalog.
  • WEB


, The Open Supernova Catalog
,weblink
, 2016-02-02
, An open-access catalog of supernova light curves and spectra.
  • WEB


, List of Supernovae with IAU Designations
,weblink
, (International Astronomical Union, IAU: Central Bureau for Astronomical Telegrams)
, 2010-10-25
,
  • NEWS


, Overbye, D.
, 2008-05-21
, Scientists See Supernova in Action
,weblink
, The New York Times
, 2008-05-21
, {{subscription required}}
  • WEB


, How to blow up a star
, Elizabeth Gibney
,weblink
, Nature (journal), Nature
, 2018-04-18
, 2018-04-20
, {{Supernovae|state=expanded}}{{Star}}{{Novae}}{{Variable star topics}}{{Featured article}}{{Authority control}}

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