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A hybrid type Ia supernova with an early flash triggered by helium-shell detonation
The detection and simulation of a type Ia supernova with an early, red flash suggests that it formed through detonation of the helium shell of a white dwarf, rather than by collision of the ejecta with a companion star or by merging with another white dwarf. A different kind of supernova Type Ia sup...
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Published in: | Nature (London) 2017-10, Vol.550 (7674), p.80-83 |
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creator | Jiang, Ji-an Doi, Mamoru Maeda, Keiichi Shigeyama, Toshikazu Nomoto, Ken’ichi Yasuda, Naoki Jha, Saurabh W. Tanaka, Masaomi Morokuma, Tomoki Tominaga, Nozomu Ivezić, Željko Ruiz-Lapuente, Pilar Stritzinger, Maximilian D. Mazzali, Paolo A. Ashall, Christopher Mould, Jeremy Baade, Dietrich Suzuki, Nao Connolly, Andrew J. Patat, Ferdinando Wang, Lifan Yoachim, Peter Jones, David Furusawa, Hisanori Miyazaki, Satoshi |
description | The detection and simulation of a type Ia supernova with an early, red flash suggests that it formed through detonation of the helium shell of a white dwarf, rather than by collision of the ejecta with a companion star or by merging with another white dwarf.
A different kind of supernova
Type Ia supernovae have rather uniform and normalizable light curves, making them suitable for cosmology, yet there remains uncertainty over what paths lead to the explosion. Several years ago a claim was made that a flash seen soon after the explosion was evidence of the shock wave hitting a normal companion star, although most other evidence so far suggests that the explosions arise from the merger of two white dwarfs. Ji-an Jiang and collaborators report observations of a red flash half a day after a type Ia explosion. Their observations lead them to the conclusion that the flash came from the detonation of a thin helium shell surrounding the exploding star. The authors conclude that their finding supports the existence of the previously proposed helium-ignition pathway.
Type Ia supernovae arise from the thermonuclear explosion of white-dwarf stars that have cores of carbon and oxygen
1
,
2
. The uniformity of their light curves makes these supernovae powerful cosmological distance indicators
3
,
4
, but there have long been debates about exactly how their explosion is triggered and what kind of companion stars are involved
2
,
5
,
6
. For example, the recent detection of the early ultraviolet pulse of a peculiar, subluminous type Ia supernova has been claimed as evidence for an interaction between a red-giant or a main-sequence companion and ejecta from a white-dwarf explosion
7
,
8
. Here we report observations of a prominent but red optical flash that appears about half a day after the explosion of a type Ia supernova. This supernova shows hybrid features of different supernova subclasses, namely a light curve that is typical of normal-brightness supernovae, but with strong titanium absorption, which is commonly seen in the spectra of subluminous ones. We argue that this early flash does not occur through previously suggested mechanisms such as the companion–ejecta interaction
8
,
9
,
10
. Instead, our simulations show that it could occur through detonation of a thin helium shell either on a near-Chandrasekhar-mass white dwarf, or on a sub-Chandrasekhar-mass white dwarf merging with a less-massive white dwarf. Our finding provides evidence that one branch of previous |
doi_str_mv | 10.1038/nature23908 |
format | article |
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A different kind of supernova
Type Ia supernovae have rather uniform and normalizable light curves, making them suitable for cosmology, yet there remains uncertainty over what paths lead to the explosion. Several years ago a claim was made that a flash seen soon after the explosion was evidence of the shock wave hitting a normal companion star, although most other evidence so far suggests that the explosions arise from the merger of two white dwarfs. Ji-an Jiang and collaborators report observations of a red flash half a day after a type Ia explosion. Their observations lead them to the conclusion that the flash came from the detonation of a thin helium shell surrounding the exploding star. The authors conclude that their finding supports the existence of the previously proposed helium-ignition pathway.
Type Ia supernovae arise from the thermonuclear explosion of white-dwarf stars that have cores of carbon and oxygen
1
,
2
. The uniformity of their light curves makes these supernovae powerful cosmological distance indicators
3
,
4
, but there have long been debates about exactly how their explosion is triggered and what kind of companion stars are involved
2
,
5
,
6
. For example, the recent detection of the early ultraviolet pulse of a peculiar, subluminous type Ia supernova has been claimed as evidence for an interaction between a red-giant or a main-sequence companion and ejecta from a white-dwarf explosion
7
,
8
. Here we report observations of a prominent but red optical flash that appears about half a day after the explosion of a type Ia supernova. This supernova shows hybrid features of different supernova subclasses, namely a light curve that is typical of normal-brightness supernovae, but with strong titanium absorption, which is commonly seen in the spectra of subluminous ones. We argue that this early flash does not occur through previously suggested mechanisms such as the companion–ejecta interaction
8
,
9
,
10
. Instead, our simulations show that it could occur through detonation of a thin helium shell either on a near-Chandrasekhar-mass white dwarf, or on a sub-Chandrasekhar-mass white dwarf merging with a less-massive white dwarf. Our finding provides evidence that one branch of previously proposed explosion models—the helium-ignition branch—does exist in nature, and that such a model may account for the explosions of white dwarfs in a mass range wider than previously supposed
11
,
12
,
13
,
14
.</description><identifier>ISSN: 0028-0836</identifier><identifier>EISSN: 1476-4687</identifier><identifier>DOI: 10.1038/nature23908</identifier><identifier>PMID: 28980637</identifier><language>eng</language><publisher>London: Nature Publishing Group UK</publisher><subject>639/33/34 ; 639/33/34/864 ; Carbon ; Companion stars ; Computer simulation ; Diffraction ; Dwarf stars ; Ejecta ; Ejection ; Explosions ; Helium ; Humanities and Social Sciences ; letter ; Light ; Light curve ; multidisciplinary ; Observations ; Oxygen ; Science ; Supernova ; Supernovae ; Supernovas ; Thermonuclear explosions ; White dwarf stars ; White dwarfs</subject><ispartof>Nature (London), 2017-10, Vol.550 (7674), p.80-83</ispartof><rights>Macmillan Publishers Limited, part of Springer Nature. All rights reserved. 2017</rights><rights>COPYRIGHT 2017 Nature Publishing Group</rights><rights>Copyright Nature Publishing Group Oct 5, 2017</rights><lds50>peer_reviewed</lds50><woscitedreferencessubscribed>false</woscitedreferencessubscribed><citedby>FETCH-LOGICAL-c556t-4f84cef191c1af93e6322c155a98f9a94e3ae5f8d6ef0301fbf87e3963ed05163</citedby><cites>FETCH-LOGICAL-c556t-4f84cef191c1af93e6322c155a98f9a94e3ae5f8d6ef0301fbf87e3963ed05163</cites></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><link.rule.ids>314,780,784,27924,27925</link.rule.ids><backlink>$$Uhttps://www.ncbi.nlm.nih.gov/pubmed/28980637$$D View this record in MEDLINE/PubMed$$Hfree_for_read</backlink></links><search><creatorcontrib>Jiang, Ji-an</creatorcontrib><creatorcontrib>Doi, Mamoru</creatorcontrib><creatorcontrib>Maeda, Keiichi</creatorcontrib><creatorcontrib>Shigeyama, Toshikazu</creatorcontrib><creatorcontrib>Nomoto, Ken’ichi</creatorcontrib><creatorcontrib>Yasuda, Naoki</creatorcontrib><creatorcontrib>Jha, Saurabh W.</creatorcontrib><creatorcontrib>Tanaka, Masaomi</creatorcontrib><creatorcontrib>Morokuma, Tomoki</creatorcontrib><creatorcontrib>Tominaga, Nozomu</creatorcontrib><creatorcontrib>Ivezić, Željko</creatorcontrib><creatorcontrib>Ruiz-Lapuente, Pilar</creatorcontrib><creatorcontrib>Stritzinger, Maximilian D.</creatorcontrib><creatorcontrib>Mazzali, Paolo A.</creatorcontrib><creatorcontrib>Ashall, Christopher</creatorcontrib><creatorcontrib>Mould, Jeremy</creatorcontrib><creatorcontrib>Baade, Dietrich</creatorcontrib><creatorcontrib>Suzuki, Nao</creatorcontrib><creatorcontrib>Connolly, Andrew J.</creatorcontrib><creatorcontrib>Patat, Ferdinando</creatorcontrib><creatorcontrib>Wang, Lifan</creatorcontrib><creatorcontrib>Yoachim, Peter</creatorcontrib><creatorcontrib>Jones, David</creatorcontrib><creatorcontrib>Furusawa, Hisanori</creatorcontrib><creatorcontrib>Miyazaki, Satoshi</creatorcontrib><title>A hybrid type Ia supernova with an early flash triggered by helium-shell detonation</title><title>Nature (London)</title><addtitle>Nature</addtitle><addtitle>Nature</addtitle><description>The detection and simulation of a type Ia supernova with an early, red flash suggests that it formed through detonation of the helium shell of a white dwarf, rather than by collision of the ejecta with a companion star or by merging with another white dwarf.
A different kind of supernova
Type Ia supernovae have rather uniform and normalizable light curves, making them suitable for cosmology, yet there remains uncertainty over what paths lead to the explosion. Several years ago a claim was made that a flash seen soon after the explosion was evidence of the shock wave hitting a normal companion star, although most other evidence so far suggests that the explosions arise from the merger of two white dwarfs. Ji-an Jiang and collaborators report observations of a red flash half a day after a type Ia explosion. Their observations lead them to the conclusion that the flash came from the detonation of a thin helium shell surrounding the exploding star. The authors conclude that their finding supports the existence of the previously proposed helium-ignition pathway.
Type Ia supernovae arise from the thermonuclear explosion of white-dwarf stars that have cores of carbon and oxygen
1
,
2
. The uniformity of their light curves makes these supernovae powerful cosmological distance indicators
3
,
4
, but there have long been debates about exactly how their explosion is triggered and what kind of companion stars are involved
2
,
5
,
6
. For example, the recent detection of the early ultraviolet pulse of a peculiar, subluminous type Ia supernova has been claimed as evidence for an interaction between a red-giant or a main-sequence companion and ejecta from a white-dwarf explosion
7
,
8
. Here we report observations of a prominent but red optical flash that appears about half a day after the explosion of a type Ia supernova. This supernova shows hybrid features of different supernova subclasses, namely a light curve that is typical of normal-brightness supernovae, but with strong titanium absorption, which is commonly seen in the spectra of subluminous ones. We argue that this early flash does not occur through previously suggested mechanisms such as the companion–ejecta interaction
8
,
9
,
10
. Instead, our simulations show that it could occur through detonation of a thin helium shell either on a near-Chandrasekhar-mass white dwarf, or on a sub-Chandrasekhar-mass white dwarf merging with a less-massive white dwarf. Our finding provides evidence that one branch of previously proposed explosion models—the helium-ignition branch—does exist in nature, and that such a model may account for the explosions of white dwarfs in a mass range wider than previously supposed
11
,
12
,
13
,
14
.</description><subject>639/33/34</subject><subject>639/33/34/864</subject><subject>Carbon</subject><subject>Companion stars</subject><subject>Computer simulation</subject><subject>Diffraction</subject><subject>Dwarf stars</subject><subject>Ejecta</subject><subject>Ejection</subject><subject>Explosions</subject><subject>Helium</subject><subject>Humanities and Social Sciences</subject><subject>letter</subject><subject>Light</subject><subject>Light curve</subject><subject>multidisciplinary</subject><subject>Observations</subject><subject>Oxygen</subject><subject>Science</subject><subject>Supernova</subject><subject>Supernovae</subject><subject>Supernovas</subject><subject>Thermonuclear explosions</subject><subject>White dwarf stars</subject><subject>White 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Basic</collection><collection>University of Michigan</collection><collection>Genetics Abstracts</collection><collection>SIRS Editorial</collection><collection>Environment Abstracts</collection><collection>MEDLINE - Academic</collection><jtitle>Nature (London)</jtitle></facets><delivery><delcategory>Remote Search Resource</delcategory><fulltext>fulltext</fulltext></delivery><addata><au>Jiang, Ji-an</au><au>Doi, Mamoru</au><au>Maeda, Keiichi</au><au>Shigeyama, Toshikazu</au><au>Nomoto, Ken’ichi</au><au>Yasuda, Naoki</au><au>Jha, Saurabh W.</au><au>Tanaka, Masaomi</au><au>Morokuma, Tomoki</au><au>Tominaga, Nozomu</au><au>Ivezić, Željko</au><au>Ruiz-Lapuente, Pilar</au><au>Stritzinger, Maximilian D.</au><au>Mazzali, Paolo A.</au><au>Ashall, Christopher</au><au>Mould, Jeremy</au><au>Baade, Dietrich</au><au>Suzuki, Nao</au><au>Connolly, Andrew J.</au><au>Patat, Ferdinando</au><au>Wang, Lifan</au><au>Yoachim, Peter</au><au>Jones, David</au><au>Furusawa, Hisanori</au><au>Miyazaki, Satoshi</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>A hybrid type Ia supernova with an early flash triggered by helium-shell detonation</atitle><jtitle>Nature (London)</jtitle><stitle>Nature</stitle><addtitle>Nature</addtitle><date>2017-10-05</date><risdate>2017</risdate><volume>550</volume><issue>7674</issue><spage>80</spage><epage>83</epage><pages>80-83</pages><issn>0028-0836</issn><eissn>1476-4687</eissn><abstract>The detection and simulation of a type Ia supernova with an early, red flash suggests that it formed through detonation of the helium shell of a white dwarf, rather than by collision of the ejecta with a companion star or by merging with another white dwarf.
A different kind of supernova
Type Ia supernovae have rather uniform and normalizable light curves, making them suitable for cosmology, yet there remains uncertainty over what paths lead to the explosion. Several years ago a claim was made that a flash seen soon after the explosion was evidence of the shock wave hitting a normal companion star, although most other evidence so far suggests that the explosions arise from the merger of two white dwarfs. Ji-an Jiang and collaborators report observations of a red flash half a day after a type Ia explosion. Their observations lead them to the conclusion that the flash came from the detonation of a thin helium shell surrounding the exploding star. The authors conclude that their finding supports the existence of the previously proposed helium-ignition pathway.
Type Ia supernovae arise from the thermonuclear explosion of white-dwarf stars that have cores of carbon and oxygen
1
,
2
. The uniformity of their light curves makes these supernovae powerful cosmological distance indicators
3
,
4
, but there have long been debates about exactly how their explosion is triggered and what kind of companion stars are involved
2
,
5
,
6
. For example, the recent detection of the early ultraviolet pulse of a peculiar, subluminous type Ia supernova has been claimed as evidence for an interaction between a red-giant or a main-sequence companion and ejecta from a white-dwarf explosion
7
,
8
. Here we report observations of a prominent but red optical flash that appears about half a day after the explosion of a type Ia supernova. This supernova shows hybrid features of different supernova subclasses, namely a light curve that is typical of normal-brightness supernovae, but with strong titanium absorption, which is commonly seen in the spectra of subluminous ones. We argue that this early flash does not occur through previously suggested mechanisms such as the companion–ejecta interaction
8
,
9
,
10
. Instead, our simulations show that it could occur through detonation of a thin helium shell either on a near-Chandrasekhar-mass white dwarf, or on a sub-Chandrasekhar-mass white dwarf merging with a less-massive white dwarf. Our finding provides evidence that one branch of previously proposed explosion models—the helium-ignition branch—does exist in nature, and that such a model may account for the explosions of white dwarfs in a mass range wider than previously supposed
11
,
12
,
13
,
14
.</abstract><cop>London</cop><pub>Nature Publishing Group UK</pub><pmid>28980637</pmid><doi>10.1038/nature23908</doi><tpages>4</tpages></addata></record> |
fulltext | fulltext |
identifier | ISSN: 0028-0836 |
ispartof | Nature (London), 2017-10, Vol.550 (7674), p.80-83 |
issn | 0028-0836 1476-4687 |
language | eng |
recordid | cdi_proquest_miscellaneous_1947619477 |
source | Nature |
subjects | 639/33/34 639/33/34/864 Carbon Companion stars Computer simulation Diffraction Dwarf stars Ejecta Ejection Explosions Helium Humanities and Social Sciences letter Light Light curve multidisciplinary Observations Oxygen Science Supernova Supernovae Supernovas Thermonuclear explosions White dwarf stars White dwarfs |
title | A hybrid type Ia supernova with an early flash triggered by helium-shell detonation |
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