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iPTF14hls

May 13, 2024

iPTF14hls is an unusual supernova star that erupted continuously for about 1,000 days beginning in September 2014[2] before becoming a remnant nebula.[3] It had previously erupted in 1954.[4] None of the theories nor proposed hypotheses fully explain all the aspects of the object.

iPTF14hls

Supernova iPTF14hls before and after detection
Observation data
Epoch J2000[1]      Equinox
Constellation Ursa Major
Right ascension 09h 20m 34.30s[1]
Declination +50° 41′ 46.80″[1]
Apparent magnitude (V) 17.716 (R)[1]
Astrometry
Distance156,200,000 pc (509,000,000 ly)[1] pc
Database references
SIMBADdata

Observations edit

The star iPTF14hls was discovered in September 2014 by the Intermediate Palomar Transient Factory,[5] and it was first made public in November 2014 by the CRTS survey[6] as CSS141118:092034+504148.[7] Based on that information, it was confirmed as an exploding star in January 2015.[8][4] It was thought then that it was a single supernova event (Type II-P) that would dim in about 100 days, but instead, it continued its eruption for about 1,000 days[3] while fluctuating in brightness at least five times.[1] The brightness varied by as much as 50%,[4] going through five peaks.[5] Also, rather than cooling down with time as expected of a Type II-P supernova, the object maintains a near-constant temperature of about 5000–6000 K.[1] Checks of photographs from the past found one from 1954 showing an explosion in the same location.[4] Since 1954, the star has exploded six times.[9]

The principal investigator[10] is Iair Arcavi. His international team used the Low-Resolution Imaging Spectrometer (LRIS) on the Keck I telescope to obtain the spectrum of the star's host galaxy, and the Deep Imaging and Multi-Object Spectrograph (DEIMOS) on Keck II to obtain high-resolution spectra of the unusual supernova itself.[11]

The host galaxy of iPTF14hls is a star-forming dwarf galaxy, implying low metal content, and the weak iron-line absorption seen in the supernova spectra are consistent with a low metallicity progenitor.[1] The study estimates that the star that exploded was at least 50 times more massive than the Sun.[12] The researchers also remark that the debris expansion rate is slower than any other known supernova by a factor of 6, as if exploding in slow motion. However, if this were due to relativistic time dilation, then the spectrum would be red-shifted by the same factor of 6, which is inconsistent with their observations.[1] In 2017, the expansion speed was constrained to approximately 1,000 km/s.[13][14]

Ongoing observations edit

Arcavi's team continue monitoring the object in other bands of the spectrum in collaboration with additional international telescopes and observatories.[15] These facilities include the Nordic Optical Telescope and NASA's Swift space telescope, the Fermi Gamma-ray Space Telescope,[16] while the Hubble Space Telescope began to image the location in December 2017.[15][17]

iPTF14hls was an ongoing event into 2018, when after about 1,000 days, its light displayed a dramatic drop, but the event remained visible,[3] and by November 2018 its spectra had become a remnant nebula.[3] A high-resolution image of this latest phase was obtained with the Hubble Space Telescope during Cycle 25 (October 1, 2017 to September 30, 2018).[3]

Hypotheses edit

Current theory predicts that the star would consume all its hydrogen in the first supernova explosion and, depending on the initial size of the star, the remnants of the core should form a neutron star or a black hole.[1][5][4] However, these mechanisms are unable to reproduce the observed light curve with its very long bright plateau and multiple brighter peaks.[17][18] None of the hypotheses published before early 2018 — the first three listed below — could explain the continued presence of hydrogen or the energetics observed.[19][20] According to Iair Arcavi, this discovery requires refinement of existing explosion scenarios, or the development of a new scenario, that can:[1]

  1. produce the same spectral signatures as common Type IIP supernovae but with an evolution slowed by a factor of 6 to 10.
  2. provide energy to prolong the light curve by a factor of ~6 while not introducing narrow-line spectral features or strong radio and X-ray emission indicative of circumstellar material interaction.
  3. produce at least five peaks in the light curve.
  4. decouple the deduced line-forming photosphere from the continuum photosphere.
  5. maintain a photospheric phase with a constant line velocity gradient for over 600 days.

Antimatter edit

One hypothesis involves burning antimatter in a stellar core;[5] this hypothesis holds that massive stars become so hot in their cores that energy is converted into matter and antimatter, causing the star to become extremely unstable, and undergo repeated bright eruptions over periods of years.[21] Antimatter in contact with matter would cause an explosion that blows off the outer layers of the star and leaves the core intact; this process can repeat over decades before the large final explosion and collapse to a black hole.[12]

Pulsational pair-instability supernova edit

Another hypothesis is the pulsational pair-instability supernova, a massive star that may lose about half its mass before a series of violent pulses begins.[1][19] On every pulse, material rushing away from the star can catch up with earlier ejected material, producing bright flashes of light as it collides, simulating an additional explosion (see supernova impostor). However, the energy released by the iPTF14hls supernova is more than the theory predicts.[12]

Magnetar edit

Magnetar models can also explain many of the observed features, but give a smooth light curve and may require an evolving magnetic field strength.[20][22]

Shock interaction edit

Jennifer E Andrews and Nathan Smith hypothesised that the observed light spectrum is a clear signature of shock interaction of ejected material with dense circumstellar material (CSM). They proposed that a typical explosion energy, with "enveloped" or "swallowed" CSM interaction — as seen in some recent supernovae, including SN 1998S, SN 2009ip, and SN 1993J — could "explain the peculiar evolution of iPTF14hls."[23]

In December 2017, a team using the Fermi Gamma-ray Space Telescope reported that they may have detected in iPTF14hls, for the first time, high energy gamma-ray emission from a supernova.[16] The gamma-ray source appears ~ 300 days after the explosion of iPTF14hls, and is still observable, but more observations are needed to verify that iPTF14hls is the exact source of the observed gamma-ray emission.[16] If the association between the gamma-ray source and iPTF14hls is real, there are difficulties to model its gamma-ray emission in the framework of particle acceleration in supernova ejecta produced shock. The energy conversion efficiency needs to be very high, so it is suggested that a jet (anisotropic emission) from a close companion may be necessary to explain some of the observed data.[16] No X-ray emissions have been detected, which makes the interpretation of the gamma-ray emission a difficult task.[24]

Common envelope jets edit

This hypothesis suggests common envelope jets supernova (CEJSN) impostors resulting from a neutron star companion. It proposes "a new type of repeating transient outburst initiated by a neutron star entering the envelope of an evolved massive star, accreting envelope material and subsequently launching jets which interact with their surroundings."[25][26] The ejecta could reach velocities of 10,000 km/s despite not being a supernova.[25]

Fall-back accretion edit

One team suggests the possibility that the observed slow expansion may be an effect of fall-back accretion, and presented a model.[3][27]

Variable hyper-wind edit

A long-term outflow similar to stellar winds with variable mass-loss rates rather than a sudden outburst like supernovae could fit the data of the light curve not only of iPTF14hls, but also of Eta Carinae. The observations could be a result of extreme wind from very massive stars.[28]

See also edit

  • Eta Carinae, a massive star undergoing similar eruptions

References edit

  1. ^ a b c d e f g h i j k l Arcavi, Iair; et al. (2017). "Energetic eruptions leading to a peculiar hydrogen-rich explosion of a massive star" (PDF). Nature. 551 (7679): 210–213. arXiv:1711.02671. Bibcode:2017Natur.551..210A. doi:10.1038/nature24030. PMID 29120417. S2CID 205260551.
  2. ^ Tasoff, H. (9 November 2017). "Bizarre Supernova Defies Understanding". Scientific American. Retrieved 2010-08-20.
  3. ^ a b c d e f Sollerman, J.; Taddia, F.; Arcavi, I.; Fremling, C.; Fransson, C.; Burke, J.; Cenko, S. B.; Andersen, O.; Andreoni, I.; Barbarino, C.; Blagorodova, N.; Brink, T. G.; Filippenko, A. V.; Gal-Yam, A.; Hiramatsu, D.; Hosseinzadeh, G.; Howell, D. A.; De Jaeger, T.; Lunnan, R.; McCully, C.; Perley, D. A.; Tartaglia, L.; Terreran, G.; Valenti, S.; Wang, X. (2019). "Late-time observations of the extraordinary Type II supernova iPTF14hls". Astronomy and Astrophysics. 621: A30. arXiv:1806.10001. Bibcode:2019A&A...621A..30S. doi:10.1051/0004-6361/201833689. S2CID 119218055.
  4. ^ a b c d e Paul Rincon (8 November 2017). "'Zombie' star survived going supernova". BBC News. Retrieved 2019-11-11.
  5. ^ a b c d Lisa Grossman (2017-11-07). "This star cheated death, exploding again and again". Science News. Retrieved 2019-11-11.
  6. ^ "The CRTS Survey". crts.caltech.edu. Retrieved 2017-11-15.
  7. ^ "Detection of CSS141118:092034+504148". Retrieved 2019-11-11.
  8. ^ Li, Wenxiong; Wang, Xiaofeng; Zhang, Tianmeng (2015-01-01). "Spectroscopic Classification of CSS141118:092034+504148 as a Type II-P Supernova". The Astronomer's Telegram. 6898: 1. Bibcode:2015ATel.6898....1L.
  9. ^ Joel Hruska (2017-11-10). "Astronomers Find Star That Has Exploded Six Times". Extremetech. Retrieved 2017-11-26.
  10. ^ Arcavi, I.; et al. (2017). "Supplementary Information to Arcavi, Iair; et al. (2017)" (PDF). Nature. 551 (7679): 210–213. arXiv:1711.02671. Bibcode:2017Natur.551..210A. doi:10.1038/nature24030. PMID 29120417. S2CID 205260551.
  11. ^ "Astronomers Discover A Star That Would Not Die". W. M. Keck Observatory. 2017-11-08. Retrieved 2019-11-11.
  12. ^ a b c "Astronomers discover a star that would not die". Astronomy Now. 2017-11-07. Retrieved 2019-11-11.
  13. ^ Milisavljevic, Dan; Margutti, Raffaella (2018). "Peculiar Supernovae". Space Science Reviews. 214 (4): 68. arXiv:1805.03655. Bibcode:2018SSRv..214...68M. doi:10.1007/s11214-018-0500-y. S2CID 118946200.
  14. ^ Andrews, Jennifer E.; Smith, Nathan (2018). "Strong late-time circumstellar interaction in the peculiar supernova iPTF14hls". Monthly Notices of the Royal Astronomical Society. 477 (1): 74. arXiv:1712.00514. Bibcode:2018MNRAS.477...74A. doi:10.1093/mnras/sty584. S2CID 119254457.
  15. ^ a b Harrison Tasoff (2017-11-08). "Bizarre 3-Year-Long Supernova Defies Our Understanding of How Stars Die". Space. Retrieved 2019-11-11.
  16. ^ a b c d Yuan, Qiang; Liao, Neng-Hui; Xin, Yu-Liang; Li, Ye; Fan, Yi-Zhong; Zhang, Bing; Hu, Hong-Bo; Bi, Xiao-Jun (2018). "Fermi Large Area Telescope Detection of Gamma-Ray Emission from the Direction of Supernova iPTF14hls". The Astrophysical Journal. 854 (2): L18. arXiv:1712.01043. Bibcode:2018ApJ...854L..18Y. doi:10.3847/2041-8213/aaacc9. S2CID 59932302.
  17. ^ a b Arcavi, Iair (2017). "What Type of Star Made the One-of-a-kind Supernova iPTF14hls?". HST Proposal: 15222. Bibcode:2017hst..prop15222A.
  18. ^ John Timmer (2017-11-08). "Scientists on new supernova: WTF have we been looking at?". Ars Technica. Retrieved 2019-11-11.
  19. ^ a b Ian Sample (2017-11-08). "'Zombie star' amazes astronomers by surviving multiple supernovae". The Guardian. Retrieved 2019-11-11.
  20. ^ a b Woosley, S. E. (2018). "Models for the Unusual Supernova iPTF14hls". The Astrophysical Journal. 863 (1): 105. arXiv:1801.08666. Bibcode:2018ApJ...863..105W. doi:10.3847/1538-4357/aad044. S2CID 119412234.
  21. ^ Jake Parks (2017-11-09). . Discovery Magazine. Archived from the original on 2018-05-31. Retrieved 2019-11-11.
  22. ^ Dessart, Luc (2018). "A magnetar model for the hydrogen-rich super-luminous supernova iPTF14hls". Astronomy & Astrophysics. 610: L10. arXiv:1801.05340. Bibcode:2018A&A...610L..10D. doi:10.1051/0004-6361/201732402. S2CID 119073998.
  23. ^ Andrews, Jennifer E.; Smith, Nathan (2018). "Strong late-time circumstellar interaction in the peculiar supernova iPTF14hls". Monthly Notices of the Royal Astronomical Society. 477 (1): 74–79. arXiv:1712.00514. Bibcode:2018MNRAS.477...74A. doi:10.1093/mnras/sty584. S2CID 119254457.
  24. ^ Yuan, Qiang; Liao, Neng-Hui; Xin, Yu-Liang; Li, Ye; Fan, Yi-Zhong; Zhang, Bing; Hu, Hong-Bo; Bi, Xiao-Jun (2018). "Fermi Large Area Telescope Detection of Gamma-Ray Emission from the Direction of Supernova iPTF14hls". The Astrophysical Journal. 854 (2): L18. arXiv:1712.01043. Bibcode:2018ApJ...854L..18Y. doi:10.3847/2041-8213/aaacc9. S2CID 59932302.
  25. ^ a b Gilkis, Avishai; Soker, Noam; Kashi, Amit (2019). "Common envelope jets supernova (CEJSN) impostors resulting from a neutron star companion". Monthly Notices of the Royal Astronomical Society. 482 (3): 4233. arXiv:1802.08669. Bibcode:2019MNRAS.482.4233G. doi:10.1093/mnras/sty3008. S2CID 119400775.
  26. ^ Soker, Noam; Gilkis, Avishai (2018). "Explaining iPTF14hls as a common-envelope jets supernova". Monthly Notices of the Royal Astronomical Society. 475 (1): 1198. arXiv:1711.05180. Bibcode:2018MNRAS.475.1198S. doi:10.1093/mnras/stx3287. S2CID 59330952.
  27. ^ Wang, L. J.; Wang, X. F.; Wang, S. Q.; Dai, Z. G.; Liu, L. D.; Song, L. M.; Rui, L. M.; Cano, Z.; Li, B. (2018). "A Fallback Accretion Model for the Unusual Type II-P Supernova iPTF14hls". The Astrophysical Journal. 865 (2): 95. arXiv:1802.03982. Bibcode:2018ApJ...865...95W. doi:10.3847/1538-4357/aadba4. S2CID 118940781.
  28. ^ Moriya, Takashi J.; Mazzali, Paolo A.; Pian, Elena (2020). "iPTF14hls as a variable hyper-wind from a very massive star". Monthly Notices of the Royal Astronomical Society. 491 (1). arXiv:1911.01740. doi:10.1093/mnras/stz3122.

External links edit

  • Light curves and spectra 2017-11-14 at the Wayback Machine on the Open Supernova Catalog 2016-03-03 at the Wayback Machine
  • This star refuses to die, even after it explodes - engadget
  • The star that blew up a little... Then blew up a lot - SyFyWire


May 13, 2024
iptf14hls, unusual, supernova, star, that, erupted, continuously, about, days, beginning, september, 2014, before, becoming, remnant, nebula, previously, erupted, 1954, none, theories, proposed, hypotheses, fully, explain, aspects, object, supernova, before, a. iPTF14hls is an unusual supernova star that erupted continuously for about 1 000 days beginning in September 2014 2 before becoming a remnant nebula 3 It had previously erupted in 1954 4 None of the theories nor proposed hypotheses fully explain all the aspects of the object iPTF14hlsSupernova iPTF14hls before and after detection Observation dataEpoch J2000 1 Equinox Constellation Ursa Major Right ascension 09h 20m 34 30s 1 Declination 50 41 46 80 1 Apparent magnitude V 17 716 R 1 AstrometryDistance156 200 000 pc 509 000 000 ly 1 pc Database referencesSIMBADdata Contents 1 Observations 1 1 Ongoing observations 2 Hypotheses 2 1 Antimatter 2 2 Pulsational pair instability supernova 2 3 Magnetar 2 4 Shock interaction 2 5 Common envelope jets 2 6 Fall back accretion 2 7 Variable hyper wind 3 See also 4 References 5 External linksObservations editThe star iPTF14hls was discovered in September 2014 by the Intermediate Palomar Transient Factory 5 and it was first made public in November 2014 by the CRTS survey 6 as CSS141118 092034 504148 7 Based on that information it was confirmed as an exploding star in January 2015 8 4 It was thought then that it was a single supernova event Type II P that would dim in about 100 days but instead it continued its eruption for about 1 000 days 3 while fluctuating in brightness at least five times 1 The brightness varied by as much as 50 4 going through five peaks 5 Also rather than cooling down with time as expected of a Type II P supernova the object maintains a near constant temperature of about 5000 6000 K 1 Checks of photographs from the past found one from 1954 showing an explosion in the same location 4 Since 1954 the star has exploded six times 9 The principal investigator 10 is Iair Arcavi His international team used the Low Resolution Imaging Spectrometer LRIS on the Keck I telescope to obtain the spectrum of the star s host galaxy and the Deep Imaging and Multi Object Spectrograph DEIMOS on Keck II to obtain high resolution spectra of the unusual supernova itself 11 The host galaxy of iPTF14hls is a star forming dwarf galaxy implying low metal content and the weak iron line absorption seen in the supernova spectra are consistent with a low metallicity progenitor 1 The study estimates that the star that exploded was at least 50 times more massive than the Sun 12 The researchers also remark that the debris expansion rate is slower than any other known supernova by a factor of 6 as if exploding in slow motion However if this were due to relativistic time dilation then the spectrum would be red shifted by the same factor of 6 which is inconsistent with their observations 1 In 2017 the expansion speed was constrained to approximately 1 000 km s 13 14 Ongoing observations edit Arcavi s team continue monitoring the object in other bands of the spectrum in collaboration with additional international telescopes and observatories 15 These facilities include the Nordic Optical Telescope and NASA s Swift space telescope the Fermi Gamma ray Space Telescope 16 while the Hubble Space Telescope began to image the location in December 2017 15 17 iPTF14hls was an ongoing event into 2018 when after about 1 000 days its light displayed a dramatic drop but the event remained visible 3 and by November 2018 its spectra had become a remnant nebula 3 A high resolution image of this latest phase was obtained with the Hubble Space Telescope during Cycle 25 October 1 2017 to September 30 2018 3 Hypotheses editCurrent theory predicts that the star would consume all its hydrogen in the first supernova explosion and depending on the initial size of the star the remnants of the core should form a neutron star or a black hole 1 5 4 However these mechanisms are unable to reproduce the observed light curve with its very long bright plateau and multiple brighter peaks 17 18 None of the hypotheses published before early 2018 the first three listed below could explain the continued presence of hydrogen or the energetics observed 19 20 According to Iair Arcavi this discovery requires refinement of existing explosion scenarios or the development of a new scenario that can 1 produce the same spectral signatures as common Type IIP supernovae but with an evolution slowed by a factor of 6 to 10 provide energy to prolong the light curve by a factor of 6 while not introducing narrow line spectral features or strong radio and X ray emission indicative of circumstellar material interaction produce at least five peaks in the light curve decouple the deduced line forming photosphere from the continuum photosphere maintain a photospheric phase with a constant line velocity gradient for over 600 days Antimatter edit One hypothesis involves burning antimatter in a stellar core 5 this hypothesis holds that massive stars become so hot in their cores that energy is converted into matter and antimatter causing the star to become extremely unstable and undergo repeated bright eruptions over periods of years 21 Antimatter in contact with matter would cause an explosion that blows off the outer layers of the star and leaves the core intact this process can repeat over decades before the large final explosion and collapse to a black hole 12 Pulsational pair instability supernova edit Another hypothesis is the pulsational pair instability supernova a massive star that may lose about half its mass before a series of violent pulses begins 1 19 On every pulse material rushing away from the star can catch up with earlier ejected material producing bright flashes of light as it collides simulating an additional explosion see supernova impostor However the energy released by the iPTF14hls supernova is more than the theory predicts 12 Magnetar edit Magnetar models can also explain many of the observed features but give a smooth light curve and may require an evolving magnetic field strength 20 22 Shock interaction edit Jennifer E Andrews and Nathan Smith hypothesised that the observed light spectrum is a clear signature of shock interaction of ejected material with dense circumstellar material CSM They proposed that a typical explosion energy with enveloped or swallowed CSM interaction as seen in some recent supernovae including SN 1998S SN 2009ip and SN 1993J could explain the peculiar evolution of iPTF14hls 23 In December 2017 a team using the Fermi Gamma ray Space Telescope reported that they may have detected in iPTF14hls for the first time high energy gamma ray emission from a supernova 16 The gamma ray source appears 300 days after the explosion of iPTF14hls and is still observable but more observations are needed to verify that iPTF14hls is the exact source of the observed gamma ray emission 16 If the association between the gamma ray source and iPTF14hls is real there are difficulties to model its gamma ray emission in the framework of particle acceleration in supernova ejecta produced shock The energy conversion efficiency needs to be very high so it is suggested that a jet anisotropic emission from a close companion may be necessary to explain some of the observed data 16 No X ray emissions have been detected which makes the interpretation of the gamma ray emission a difficult task 24 Common envelope jets edit This hypothesis suggests common envelope jets supernova CEJSN impostors resulting from a neutron star companion It proposes a new type of repeating transient outburst initiated by a neutron star entering the envelope of an evolved massive star accreting envelope material and subsequently launching jets which interact with their surroundings 25 26 The ejecta could reach velocities of 10 000 km s despite not being a supernova 25 Fall back accretion edit One team suggests the possibility that the observed slow expansion may be an effect of fall back accretion and presented a model 3 27 Variable hyper wind edit A long term outflow similar to stellar winds with variable mass loss rates rather than a sudden outburst like supernovae could fit the data of the light curve not only of iPTF14hls but also of Eta Carinae The observations could be a result of extreme wind from very massive stars 28 See also edit nbsp Astronomy portal Eta Carinae a massive star undergoing similar eruptionsReferences edit a b c d e f g h i j k l Arcavi Iair et al 2017 Energetic eruptions leading to a peculiar hydrogen rich explosion of a massive star PDF Nature 551 7679 210 213 arXiv 1711 02671 Bibcode 2017Natur 551 210A doi 10 1038 nature24030 PMID 29120417 S2CID 205260551 Tasoff H 9 November 2017 Bizarre Supernova Defies Understanding Scientific American Retrieved 2010 08 20 a b c d e f Sollerman J Taddia F Arcavi I Fremling C Fransson C Burke J Cenko S B Andersen O Andreoni I Barbarino C Blagorodova N Brink T G Filippenko A V Gal Yam A Hiramatsu D Hosseinzadeh G Howell D A De Jaeger T Lunnan R McCully C Perley D A Tartaglia L Terreran G Valenti S Wang X 2019 Late time observations of the extraordinary Type II supernova iPTF14hls Astronomy and Astrophysics 621 A30 arXiv 1806 10001 Bibcode 2019A amp A 621A 30S doi 10 1051 0004 6361 201833689 S2CID 119218055 a b c d e Paul Rincon 8 November 2017 Zombie star survived going supernova BBC News Retrieved 2019 11 11 a b c d Lisa Grossman 2017 11 07 This star cheated death exploding again and again Science News Retrieved 2019 11 11 The CRTS Survey crts caltech edu Retrieved 2017 11 15 Detection of CSS141118 092034 504148 Retrieved 2019 11 11 Li Wenxiong Wang Xiaofeng Zhang Tianmeng 2015 01 01 Spectroscopic Classification of CSS141118 092034 504148 as a Type II P Supernova The Astronomer s Telegram 6898 1 Bibcode 2015ATel 6898 1L Joel Hruska 2017 11 10 Astronomers Find Star That Has Exploded Six Times Extremetech Retrieved 2017 11 26 Arcavi I et al 2017 Supplementary Information to Arcavi Iair et al 2017 PDF Nature 551 7679 210 213 arXiv 1711 02671 Bibcode 2017Natur 551 210A doi 10 1038 nature24030 PMID 29120417 S2CID 205260551 Astronomers Discover A Star That Would Not Die W M Keck Observatory 2017 11 08 Retrieved 2019 11 11 a b c Astronomers discover a star that would not die Astronomy Now 2017 11 07 Retrieved 2019 11 11 Milisavljevic Dan Margutti Raffaella 2018 Peculiar Supernovae Space Science Reviews 214 4 68 arXiv 1805 03655 Bibcode 2018SSRv 214 68M doi 10 1007 s11214 018 0500 y S2CID 118946200 Andrews Jennifer E Smith Nathan 2018 Strong late time circumstellar interaction in the peculiar supernova iPTF14hls Monthly Notices of the Royal Astronomical Society 477 1 74 arXiv 1712 00514 Bibcode 2018MNRAS 477 74A doi 10 1093 mnras sty584 S2CID 119254457 a b Harrison Tasoff 2017 11 08 Bizarre 3 Year Long Supernova Defies Our Understanding of How Stars Die Space Retrieved 2019 11 11 a b c d Yuan Qiang Liao Neng Hui Xin Yu Liang Li Ye Fan Yi Zhong Zhang Bing Hu Hong Bo Bi Xiao Jun 2018 Fermi Large Area Telescope Detection of Gamma Ray Emission from the Direction of Supernova iPTF14hls The Astrophysical Journal 854 2 L18 arXiv 1712 01043 Bibcode 2018ApJ 854L 18Y doi 10 3847 2041 8213 aaacc9 S2CID 59932302 a b Arcavi Iair 2017 What Type of Star Made the One of a kind Supernova iPTF14hls HST Proposal 15222 Bibcode 2017hst prop15222A John Timmer 2017 11 08 Scientists on new supernova WTF have we been looking at Ars Technica Retrieved 2019 11 11 a b Ian Sample 2017 11 08 Zombie star amazes astronomers by surviving multiple supernovae The Guardian Retrieved 2019 11 11 a b Woosley S E 2018 Models for the Unusual Supernova iPTF14hls The Astrophysical Journal 863 1 105 arXiv 1801 08666 Bibcode 2018ApJ 863 105W doi 10 3847 1538 4357 aad044 S2CID 119412234 Jake Parks 2017 11 09 This Star Went Supernova And Then Went Supernova Again Discovery Magazine Archived from the original on 2018 05 31 Retrieved 2019 11 11 Dessart Luc 2018 A magnetar model for the hydrogen rich super luminous supernova iPTF14hls Astronomy amp Astrophysics 610 L10 arXiv 1801 05340 Bibcode 2018A amp A 610L 10D doi 10 1051 0004 6361 201732402 S2CID 119073998 Andrews Jennifer E Smith Nathan 2018 Strong late time circumstellar interaction in the peculiar supernova iPTF14hls Monthly Notices of the Royal Astronomical Society 477 1 74 79 arXiv 1712 00514 Bibcode 2018MNRAS 477 74A doi 10 1093 mnras sty584 S2CID 119254457 Yuan Qiang Liao Neng Hui Xin Yu Liang Li Ye Fan Yi Zhong Zhang Bing Hu Hong Bo Bi Xiao Jun 2018 Fermi Large Area Telescope Detection of Gamma Ray Emission from the Direction of Supernova iPTF14hls The Astrophysical Journal 854 2 L18 arXiv 1712 01043 Bibcode 2018ApJ 854L 18Y doi 10 3847 2041 8213 aaacc9 S2CID 59932302 a b Gilkis Avishai Soker Noam Kashi Amit 2019 Common envelope jets supernova CEJSN impostors resulting from a neutron star companion Monthly Notices of the Royal Astronomical Society 482 3 4233 arXiv 1802 08669 Bibcode 2019MNRAS 482 4233G doi 10 1093 mnras sty3008 S2CID 119400775 Soker Noam Gilkis Avishai 2018 Explaining iPTF14hls as a common envelope jets supernova Monthly Notices of the Royal Astronomical Society 475 1 1198 arXiv 1711 05180 Bibcode 2018MNRAS 475 1198S doi 10 1093 mnras stx3287 S2CID 59330952 Wang L J Wang X F Wang S Q Dai Z G Liu L D Song L M Rui L M Cano Z Li B 2018 A Fallback Accretion Model for the Unusual Type II P Supernova iPTF14hls The Astrophysical Journal 865 2 95 arXiv 1802 03982 Bibcode 2018ApJ 865 95W doi 10 3847 1538 4357 aadba4 S2CID 118940781 Moriya Takashi J Mazzali Paolo A Pian Elena 2020 iPTF14hls as a variable hyper wind from a very massive star Monthly Notices of the Royal Astronomical Society 491 1 arXiv 1911 01740 doi 10 1093 mnras stz3122 External links editLight curves and spectra Archived 2017 11 14 at the Wayback Machine on the Open Supernova Catalog Archived 2016 03 03 at the Wayback Machine This star refuses to die even after it explodes engadget The star that blew up a little Then blew up a lot SyFyWire Portal nbsp Astronomy Retrieved from https en wikipedia org w index php title IPTF14hls amp oldid 1220685718, wikipedia, wiki, book, books, library,

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