Revealing progenitors of type Ia supernovae from their light curves and spectra

Kutsuna, Masamichi; Shigeyama, Toshikazu

doi:10.1093/pasj/psv028

Cited by 25 publications

(40 citation statements)

References 27 publications

(46 reference statements)

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“…Radio and X-ray observations reported no detection of the SN in these wavelengths which was interpreted as a support for DD scenario for SN 2014J, and was also used to estimate the progenitor mass-loss rate (Pérez-Torres et al 2014;Margutti et al 2014;Nielsen et al 2014). This estimate is in agreement with the upper limits estimated by Kelly et al (2014) using HST data from near-UV to near-NIR and by Lundqvist et al (2015) using late optical spectra (but see Graham et al 2015 for evidence of multiple components of CSM which would favor the SD scenario, and Kutsuna & Shigeyama (2015) who do not rule it out). Interestingly, Crotts (2015) reported the discovery of light-echoes at ∼80 pc from the SN location revealing the CSM structure.…”

Section: Introductionsupporting

confidence: 84%

SN 2014J at M82 – I. A middle-class Type Ia supernova by all spectroscopic metrics

Galbany

Moreno-Raya

Ruiz‐Lapuente

et al. 2016

Mon. Not. R. Astron. Soc.

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We present the intensive spectroscopic follow up of the type Ia supernova (SN Ia) 2014J in the starburst galaxy M82. Twenty-seven optical spectra have been acquired from January 22 nd to September 1 st 2014 with the Isaac Newton (INT) and William Herschel (WHT) Telescopes. After correcting the observations for the recession velocity of M82 and for Milky Way and host galaxy extinction, we measured expansion velocities from spectral line blueshifts and pseudo-equivalent width of the strongest features in the spectra, which gives an idea on how elements are distributed within the ejecta. We position SN 2014J in the Benetti (2005)

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Section: Introductionsupporting

confidence: 84%

SN 2014J at M82 – I. A middle-class Type Ia supernova by all spectroscopic metrics

Galbany

Moreno-Raya

Ruiz‐Lapuente

et al. 2016

Mon. Not. R. Astron. Soc.

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“…In the CSM-ejecta-interaction scenario, a more extended CSM distribution could generate a brighter flash but with longer diffusion time. Our best-fitting CEI model (Figures 2 & 3) and previous simulations of both two scenarios 8,10,19 all indicate that the particular blue color evolution is inevitable when producing the early flash as bright as that of MUSSES1604D (Extended Data Figure 1), which is incompatible with the red and rapid early color evolution observed for MUSSES1604D.…”

mentioning

confidence: 60%

“…The interaction of SN ejecta with a non-degenerate companion star 8,18,19 ("companionejecta interaction", CEI) or with dense circumstellar material 9,10 ("CSM-ejecta interaction") are popular scenarios to explain the early optical flash. In order to produce a prominent optical flash comparable to that of MUSSES1604D, either a companion with a very extended envelope or a large-scale CSM distribution is required.…”

mentioning

confidence: 99%

“…In order to produce a prominent optical flash comparable to that of MUSSES1604D, either a companion with a very extended envelope or a large-scale CSM distribution is required. In the CEI scenario, a prominent flash generated from the inner, hot region of ejecta can be observed through the hole that is carved out by a red-giant companion 8,19 . In the CSM-ejecta-interaction scenario, a more extended CSM distribution could generate a brighter flash but with longer diffusion time.…”

mentioning

confidence: 99%

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A hybrid type Ia supernova with an early flash triggered by helium-shell detonation

Jiang

Doi

Maeda

et al. 2017

Nature

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127

166

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Type Ia supernovae arise from the thermonuclear explosion of white-dwarf stars that have cores of carbon and oxygen. The uniformity of their light curves makes these supernovae powerful cosmological distance indicators, but there have long been debates about exactly how their explosion is triggered and what kind of companion stars are involved. 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. 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. 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.

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“…As a result, the early supernova light curve can be brightened by the collision of the supernova ejecta with the companion star (Kasen 2010;Moriya et al 2015;Kutsuna & Shigeyama 2015;Liu et al 2015). Also, the companion star may be significantly heated and shocked by the SN impact, causing the envelope of the companion star to be partially removed due to the stripping and ablation mechanism (Wheeler et al 1975;Fryxell & Arnett 1981;Taam & Fryxell 1984).…”

Section: Introductionmentioning

confidence: 99%

The interaction of core-collapse supernova ejecta with a companion star

Liu

Tauris

Röpke

et al. 2015

A&A

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Context. The progenitors of many core-collapse supernovae (CCSNe) are expected to be in binary systems. After the SN explosion in a binary, the companion star may suffer from mass stripping and be shock heated as a result of the impact of the SN ejecta. If the binary system is disrupted by the SN explosion, the companion star is ejected as a runaway star, and in some cases as a hypervelocity star. Aims. By performing a series of three-dimensional (3D) hydrodynamical simulations of the collision of SN ejecta with the companion star, we investigate how CCSN explosions affect their binary companion. Methods. We use the BEC stellar evolution code to construct the detailed companion structure at the moment of SN explosion. The impact of the SN blast wave on the companion star is followed by means of 3D smoothed particle hydrodynamics (SPH) simulations using the Stellar GADGET code. Results. For main-sequence (MS) companion stars, we find that the amount of removed stellar mass, the resulting impact velocity, and the chemical contamination of the companion that results from the impact of the SN ejecta strongly increases with decreasing binary separation and increasing explosion energy. Their relationship can be approximately fitted by power laws, which is consistent with the results obtained from impact simulations of Type Ia SNe. However, we find that the impact velocity is sensitive to the momentum profile of the outer SN ejecta and, in fact, may decrease with increasing ejecta mass, depending on the modeling of the ejecta. Because most companion stars to Type Ib/c CCSNe are in their MS phase at the moment of the explosion, combined with the strongly decaying impact effects with increasing binary separation, we argue that the majority of these SNe lead to inefficient mass stripping and shock heating of the companion star following the impact of the ejecta. Conclusions. Our simulations show that the impact effects of Type Ib/c SN ejecta on the structure of MS companion stars, and thus their long-term post-explosion evolution, is in general not dramatic. We find that at most 10% of their mass is lost and their resulting impact velocities are less than 100 km s −1 .

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Revealing progenitors of type Ia supernovae from their light curves and spectra

Cited by 25 publications

References 27 publications

SN 2014J at M82 – I. A middle-class Type Ia supernova by all spectroscopic metrics

SN 2014J at M82 – I. A middle-class Type Ia supernova by all spectroscopic metrics

A hybrid type Ia supernova with an early flash triggered by helium-shell detonation

The interaction of core-collapse supernova ejecta with a companion star

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