A hypernova (sometimes called a collapsar) is a very energetic supernova thought to result from an extreme core-collapse scenario. In this case a massive star (>30 solar masses) collapses to form a rotating black hole emitting twin energetic jets and surrounded by an accretion disk. It is a type of stellar explosion which ejects material with an unusually high kinetic energy, an order of magnitude higher than most supernovae. They usually appear similar to a type Ic supernova, but with unusually broad spectral lines indicating an extremely high expansion velocity. Hypernovae are one of the mechanisms for producing long gamma ray bursts (GRBs), which range from 2 seconds to over a minute in duration.


In the 1980s, the term hypernova was used to describe a theoretical type of supernova now known as a pair-instability supernova. It referred to the extremely high energy of the explosion compared to typical core collapse supernovae.[1][2][3] The term had previously been used to describe hypothetical explosions from diverse events such as hyperstars, extremely massive population III stars in the early universe,[4] or from events such as black hole mergers.[5]

GRBs were initially detected on July 2, 1967 by US military satellites in high orbit, which were meant to detect gamma radiation. The US had suspected the USSR of conducting secret nuclear tests despite signing the Nuclear Test Ban Treaty of 1963, and the Vela satellites were capable of detecting explosions behind the moon. The satellites detected a signal, but it was unlike that of a nuclear weapon signature, nor could it be correlated to solar flares.[6] Over the next few decades, the GRBs posed a compelling mystery. Gamma rays require highly energetic events to be produced, yet GRBs could not be correlated to supernovae, solar flares, or any other activity in the sky. Their brevity made them difficult to trace. Once their direction could be determined, it was found that they were evenly spread across the sky. Thus they were not originating in the Milky Way or nearby galaxies, but from deep space.

In February 1997, Dutch-Italian satellite BeppoSAX was able to trace GRB 970508 to a faint galaxy roughly 6 billion light years away.[7] From analyzing the spectroscopic data for both the GRB 970508 and its host galaxy, Bloom et al. concluded in 1998 that a hypernova was the likely cause.[7] That same year, hypernovae were hypothesized in greater detail by Polish astronomer Bohdan Paczyński as supernovae from rapidly-spinning stars.[8]

The usage of the term hypernova from the late 20th century has since been refined to refer to those supernovae with unusually large kinetic energy.[9] The first hypernova observed was SN 1998bw, with a luminosity 100 times higher than a standard Type Ib.[10] This supernova was the first to be associated with a gamma-ray burst (GRB) and it produced a shockwave containing an order of magnitude more energy than a normal supernova. Other scientists prefer to call these objects simply broad-lined type Ic supernovae.[11] Since then the term has been applied to a variety of objects, not all of which meet the standard definition; for example ASASSN-15lh.[12]

Hypernovae are now widely accepted to be supernovae with ejecta having a kinetic energy larger than about 1052 erg, an order of magnitude higher than a typical core collapse supernova. The ejected nickel masses are large and the ejection velocity up to 99% of the speed of light. These are typically of type Ic, and some are associated with long-duration gamma-ray bursts. The electromagnetic energy released by these events varies from comparable to other type Ic supernova, to some of the most luminous supernovae known such as SN 1999as.[13][14]

The archetypal hypernova, SN 1998bw, was associated with GRB 980425. Its spectrum showed no hydrogen and no clear helium features, but strong silicon lines identified it as a type Ic supernova. The main absorption lines were extremely broadened and the light curve showed a very rapid brightening phase, reaching the brightness of a type Ia supernova at day 16. The total ejected mass was about 10 M☉ and the mass of nickel ejected about 0.4 M☉.[13] All supernovae associated with GRBs have shown the high-energy ejecta that characterises them as hypernovae.[15]

Unusually bright radio supernovae have been observed as counterparts to hypernovae, and have been termed radio hypernovae.[16]
Astrophysical models

Models for hypernova focus on the efficient transfer of energy into the ejecta. In normal core collapse supernovae, 99% of neutrinos generated in the collapsing core escape without driving the ejection of material. It is thought that rotation of the supernova progenitor drives a jet that accelerates material away from the explosion at close to the speed of light. Binary systems are increasingly being studied as the best method for both stripping stellar envelopes to leave a bare carbon-oxygen core, and for inducing the necessary spin conditions to drive a hypernova.
Collapsar model
For a completely collapsed star, see stellar black hole.

The collapsar model describes a type of supernova that produces a gravitationally collapsed object, or black hole. The word "collapsar", short for "collapsed star", was formerly used to refer to the end product of stellar gravitational collapse, a stellar-mass black hole. The word is now sometimes used to refer to a specific model for the collapse of a fast-rotating star. When core collapse occurs in a star with a core at least around fifteen times the sun's mass (M☉)—though chemical composition and rotational rate are also significant—the explosion energy is insufficient to expel the outer layers of the star, and it will collapse into a black hole without producing a visible supernova outburst.

A star with a core mass slightly below this level—in the range of 5–15 M☉—will undergo a supernova explosion, but so much of the ejected mass falls back onto the core remnant that it still collapses into a black hole. If such a star is rotating slowly, then it will produce a faint supernova, but if the star is rotating quickly enough, then the fallback to the black hole will produce relativistic jets. The energy that these jets transfer into the ejected shell renders the visible outburst substantially more luminous than a standard supernova. The jets also beam high energy particles and gamma rays directly outward and thereby produce x-ray or gamma-ray bursts; the jets can last for several seconds or longer and correspond to long-duration gamma-ray bursts, but they do not appear to explain short-duration gamma-ray bursts.[17][18]
Binary models

The mechanism for producing the stripped progenitor, a carbon-oxygen star lacking any significant hydrogen or helium, of type Ic supernovae was once thought to be an extremely evolved massive star, for example a type WO Wolf-Rayet star whose dense stellar wind expelled all its outer layers. Observations have failed to detect any such progenitors. It is still not conclusively shown that the progenitors are actually a different type of object, but several cases suggest that lower-mass "helium giants" are the progenitors. These stars are not sufficiently massive to expel their envelopes simply by stellar winds, and they would be stripped by mass transfer to a binary companion. Helium giants are increasingly favoured as the progenitors of type Ib supernovae, but the progenitors of type Ic supernovae is still uncertain.[19]

One proposed mechanism for producing gamma-ray bursts is induced gravitational collapse, where a neutron star is triggered to collapse into a black hole by the core collapse of a close companion consisting of a stripped carbon-oxygen core. The induced neutron star collapse allows for the formation of jets and high-energy ejecta that have been difficult to model from a single star.[20]
See also

Astronomy portal

Gamma-ray burst progenitors – Types of celestial objects that can emit gamma-ray bursts
Quark star – Compact exotic star which forms matter consisting mostly of quarks
Quark-nova – Hypothetical violent explosion resulting from conversion of a neutron star to a quark star


Woosley, S. E.; Weaver, T. A. (1981). "Theoretical models for supernovae". NASA Sti/Recon Technical Report N. 83: 16268. Bibcode:1981STIN...8316268W.
Janka, Hans-Thomas (2012). "Explosion Mechanisms of Core-Collapse Supernovae". Annual Review of Nuclear and Particle Science. 62 (1): 407–451.arXiv:1206.2503. Bibcode:2012ARNPS..62..407J. doi:10.1146/annurev-nucl-102711-094901. S2CID 118417333.
Gass, H.; Liebert, J.; Wehrse, R. (1988). "Spectrum analysis of the extremely metal-poor carbon dwarf star G 77-61". Astronomy and Astrophysics. 189: 194. Bibcode:1988A&A...189..194G.
Barrington, R. E.; Belrose, J. S. (1963). "Preliminary Results from the Very-Low Frequency Receiver Aboard Canada's Alouette Satellite". Nature. 198 (4881): 651–656. Bibcode:1963Natur.198..651B. doi:10.1038/198651a0. S2CID 41012117.
Park, Seok J.; Vishniac, Ethan T. (1991). "Are Hypernovae Detectable?". The Astrophysical Journal. 375: 565. Bibcode:1991ApJ...375..565P. doi:10.1086/170217.
Jonathan I. Katz (2002). The Biggest Bangs: The Mystery of Gamma-ray Bursts, the Most Violent Explosions in the Universe. Oxford University Press. ISBN 978-0-19-514570-0.
Bloom (1998). "The Host Galaxy of GRB 970508". The Astrophysical Journal. 507 (507): L25–28.arXiv:astro-ph/9807315. Bibcode:1998ApJ...507L..25B. doi:10.1086/311682. S2CID 18107687.
Paczynski (1997). "GRBs as Hypernovae".arXiv:astro-ph/9712123.
David S. Stevenson (5 September 2013). Extreme Explosions: Supernovae, Hypernovae, Magnetars, and Other Unusual Cosmic Blasts. Springer Science & Business Media. ISBN 978-1-4614-8136-2.
Woosley (1999). "Gamma-Ray Bursts and Type Ic Supernovae: SN 1998bw". The Astrophysical Journal. 516 (2): 788–796.arXiv:astro-ph/9806299. Bibcode:1999ApJ...516..788W. doi:10.1086/307131. S2CID 17690696.
Moriya, Takashi J.; Sorokina, Elena I.; Chevalier, Roger A. (2018). "Superluminous Supernovae". Space Science Reviews. 214 (2): 59.arXiv:1803.01875. Bibcode:2018SSRv..214...59M. doi:10.1007/s11214-018-0493-6. S2CID 119199790.
Jessica Orwig (January 14, 2016). "Astronomers are baffled by a newly discovered cosmic explosion that shines 570 billion times brighter than the sun". Retrieved March 22, 2016.
Nomoto, Ken'Ichi; Maeda, Keiichi; Mazzali, Paolo A.; Umeda, Hideyuki; Deng, Jinsong; Iwamoto, Koichi (2004). "Hypernovae and Other Black-Hole-Forming Supernovae". Astrophysics and Space Science Library. 302: 277–325.arXiv:astro-ph/0308136. Bibcode:2004ASSL..302..277N. doi:10.1007/978-0-306-48599-2_10. ISBN 978-90-481-6567-4. S2CID 119421669.
Mazzali, P. A.; Nomoto, K.; Deng, J.; Maeda, K.; Tominaga, N. (2005). "The Properties of Hypernovae in Gamma Ray Bursts". 1604-2004: Supernovae as Cosmological Lighthouses. 342: 366. Bibcode:2005ASPC..342..366M.
Mösta, Philipp; Richers, Sherwood; Ott, Christian D.; Haas, Roland; Piro, Anthony L.; Boydstun, Kristen; Abdikamalov, Ernazar; Reisswig, Christian; Schnetter, Erik (2014). "Magnetorotational Core-Collapse Supernovae in Three Dimensions". The Astrophysical Journal. 785 (2): L29.arXiv:1403.1230. Bibcode:2014ApJ...785L..29M. doi:10.1088/2041-8205/785/2/L29. S2CID 17989552.
Nakauchi, Daisuke; Kashiyama, Kazumi; Nagakura, Hiroki; Suwa, Yudai; Nakamura, Takashi (2015). "Optical Synchrotron Precursors of Radio Hypernovae". The Astrophysical Journal. 805 (2): 164.arXiv:1411.1603. Bibcode:2015ApJ...805..164N. doi:10.1088/0004-637X/805/2/164. S2CID 118228337.
Nomoto, Ken'Ichi; Moriya, Takashi; Tominaga, Nozomu (2009). "Nucleosynthesis of the Elements in Faint Supernovae and Hypernovae". Proceedings of the International Astronomical Union. 5: 34–41. doi:10.1017/S1743921310000128.
Fujimoto, S. I.; Nishimura, N.; Hashimoto, M. A. (2008). "Nucleosynthesis in Magnetically Driven Jets from Collapsars". The Astrophysical Journal. 680 (2): 1350–1358.arXiv:0804.0969. Bibcode:2008ApJ...680.1350F. doi:10.1086/529416. S2CID 118559576.
Tauris, T. M.; Langer, N.; Moriya, T. J.; Podsiadlowski, Ph.; Yoon, S.-C.; Blinnikov, S. I. (2013). "ULTRA-STRIPPED TYPE Ic SUPERNOVAE FROM CLOSE BINARY EVOLUTION". The Astrophysical Journal. 778 (2): L23.arXiv:1310.6356. Bibcode:2013ApJ...778L..23T. doi:10.1088/2041-8205/778/2/L23. S2CID 50835291.

Ruffini, R.; Karlica, M.; Sahakyan, N.; Rueda, J. A.; Wang, Y.; Mathews, G. J.; Bianco, C. L.; Muccino, M. (2018). "A GRB Afterglow Model Consistent with Hypernova Observations". The Astrophysical Journal. 869 (2): 101.arXiv:1712.05000. Bibcode:2018ApJ...869..101R. doi:10.3847/1538-4357/aaeac8. S2CID 119449351.

Further reading

MacFadyen, A. I.; Woosley, S. E. (1999). "Collapsars: Gamma-Ray Bursts and Explosions in 'Failed Supernovae'". Astrophysical Journal. 524 (1): 262–289.arXiv:astro-ph/9810274. Bibcode:1999ApJ...524..262M. doi:10.1086/307790. S2CID 15534333.
Woosley, S. E. (1993). "Gamma-ray bursts from stellar mass accretion disks around black holes". Astrophysical Journal. 405 (1): 273–277. Bibcode:1993ApJ...405..273W. doi:10.1086/172359.
Piran, T. (2004). "The Physics of Gamma-Ray Bursts". Reviews of Modern Physics. 76 (4): 1143–1210.arXiv:astro-ph/0405503v1. Bibcode:2004RvMP...76.1143P. doi:10.1103/RevModPhys.76.1143. S2CID 118941182.
Hjorth, Jens; Sollerman, Jesper; Møller, Palle; Fynbo, Johan P. U.; Woosley, Stan E.; Kouveliotou, Chryssa; Tanvir, Nial R.; Greiner, Jochen; Andersen, Michael I.; et al. (2003). "A very energetic supernova associated with the γ-ray burst of 29 March 2003". Nature. 423 (6942): 847–50.arXiv:astro-ph/0306347. Bibcode:2003Natur.423..847H. doi:10.1038/nature01750. PMID 12815425. S2CID 4405772.



Type Ia Type Ib and Ic Type II (IIP, IIL, IIn, and IIb) Hypernova Superluminous Pair-instability

Physics of

Calcium-rich Carbon detonation Foe Near-Earth Phillips relationship Nucleosynthesis
P-process R-process Neutrinos


pulsational pair-instability Failed Gamma-ray burst Kilonova Luminous red nova Nova Pulsar kick Quark-nova Symbiotic nova


yellow Luminous blue variable Supergiant
blue red yellow White dwarf
related links Wolf–Rayet star


Supernova remnant
Pulsar wind nebula Neutron star
pulsar magnetar related links Stellar black hole
related links Compact star
quark star exotic star Zombie star Local Bubble Superbubble


Guest star History of supernova observation Timeline of white dwarfs, neutron stars, and supernovae


Candidates Notable Massive stars Most distant Remnants In fiction


Barnard's Loop Cassiopeia A Crab
Crab Nebula iPTF14hls Tycho's Kepler's SN 1987A SN 185 SN 1006 SN 2003fg Remnant G1.9+0.3 SN 2007bi SN 2011fe SN 2014J SN Refsdal Vela Remnant


ASAS-SN Calán/Tololo Survey High-Z Supernova Search Team Katzman Automatic Imaging Telescope Monte Agliale Supernovae and Asteroid Survey Nearby Supernova Factory Sloan Supernova Survey Supernova/Acceleration Probe Supernova Cosmology Project SuperNova Early Warning System Supernova Legacy Survey Texas Supernova Search



Accretion Molecular cloud Bok globule Young stellar object
Protostar Pre-main-sequence Herbig Ae/Be T Tauri FU Orionis Herbig–Haro object Hayashi track Henyey track


Main sequence Red-giant branch Horizontal branch
Red clump Asymptotic giant branch
super-AGB Blue loop Protoplanetary nebula Planetary nebula PG1159 Dredge-up OH/IR Instability strip Luminous blue variable Blue straggler Stellar population Supernova Superluminous supernova / Hypernova

Spectral classification

Early Late Main sequence
O B A F G K M Brown dwarf WR OB Subdwarf
O B Subgiant Giant
Blue Red Yellow Bright giant Supergiant
Blue Red Yellow Hypergiant
Yellow Carbon
S CN CH White dwarf Chemically peculiar
Am Ap/Bp HgMn Helium-weak Barium Extreme helium Lambda Boötis Lead Technetium Be
Shell B[e]


White dwarf
Helium planet Black dwarf Neutron
Radio-quiet Pulsar
Binary X-ray Magnetar Stellar black hole X-ray binary


Blue dwarf Green Black dwarf Exotic
Boson Electroweak Strange Preon Planck Dark Dark-energy Quark Q Black Gravastar Frozen Quasi-star Thorne–Żytkow object Iron Blitzar

Stellar nucleosynthesis

Deuterium burning Lithium burning Proton–proton chain CNO cycle Helium flash Triple-alpha process Alpha process Carbon burning Neon burning Oxygen burning Silicon burning S-process R-process Fusor Nova
Symbiotic Remnant Luminous red nova


Core Convection zone
Microturbulence Oscillations Radiation zone Atmosphere
Photosphere Starspot Chromosphere Stellar corona Stellar wind
Bubble Bipolar outflow Accretion disk Asteroseismology
Helioseismology Eddington luminosity Kelvin–Helmholtz mechanism


Designation Dynamics Effective temperature Luminosity Kinematics Magnetic field Absolute magnitude Mass Metallicity Rotation Starlight Variable Photometric system Color index Hertzsprung–Russell diagram Color–color diagram

Star systems

Contact Common envelope Eclipsing Symbiotic Multiple Cluster
Open Globular Super Planetary system


Solar System Sunlight Pole star Circumpolar Constellation Asterism Magnitude
Apparent Extinction Photographic Radial velocity Proper motion Parallax Photometric-standard


Proper names
Arabic Chinese Extremes Most massive Highest temperature Lowest temperature Largest volume Smallest volume Brightest
Historical Most luminous Nearest
Nearest bright With exoplanets Brown dwarfs White dwarfs Milky Way novae Supernovae
Candidates Remnants Planetary nebulae Timeline of stellar astronomy

Related articles

Substellar object
Brown dwarf Sub-brown dwarf Planet Galactic year Galaxy Guest Gravity Intergalactic Planet-hosting stars Tidal disruption event

Physics Encyclopedia



Hellenica World - Scientific Library

Retrieved from ""
All text is available under the terms of the GNU Free Documentation License