The response of a helium white dwarf to an exploding Type Ia supernova

Papish, Oded; Soker, Noam; Garcı́a–Berro, E.; Aznar–Siguán, Gabriela

doi:10.1093/mnras/stv337

Cited by 28 publications

(34 citation statements)

References 67 publications

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“…The SN ejecta collides with the companion WD, and the interaction of the SN ejecta with the companion WD form the ejecta shadow and companion-origin stream. Papish et al (2015) have also found out such ejecta shadows in their simulations for their D 6 models. The companion WD survives the explosion of the primary WD, and flies away at velocity of ∼ 1700 km s −1 as the surviving WD.…”

Section: Discussionmentioning

confidence: 74%

Three-dimensional Simulation of Double Detonations in the Double-degenerate Model for Type Ia Supernovae and Interaction of Ejecta with a Surviving White Dwarf Companion

Tanikawa

Nomoto

Nakasato

2018

ApJ

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We study the hydrodynamics and nucleosynthesis in the double-detonation model of Type Ia supernovae (SNe Ia) and the interaction between the ejecta and a surviving white dwarf (WD) companion in the double-degenerate scenario. We set up a binary star system with 1.0M and 0.6M carbon-oxygen (CO) WDs, where the primary WD consists of a CO core and helium (He) shell with 0.95 and 0.05M , respectively. We follow the evolution of the binary star system from the initiation of a He detonation, ignition and propagation of a CO detonation, and the interaction of SN ejecta with the companion WD. The companion (or surviving) WD gets a flung-away velocity of ∼ 1700 km s −1 , and captures 56 Ni of ∼ 0.03M , and He of 3 × 10 −4 M . Such He can be detected on the surface of surviving WDs. The SN ejecta contains a "companion-origin stream", and unburned materials stripped from the companion WD (∼ 3 · 10 −3 M ), although the stream compositions would depend on the He shell mass of the companion WD. The ejecta has also a velocity shift of ∼ 1000 km s −1 due to the binary motion of the exploding primary WD. These features would be prominent in nebular-phase spectra of oxygen emission lines from the unburned materials like SN 2010lp and iPTF14atg, and of blue-or red-shifted Fe-group emission lines from the velocity shift like a part of sub-luminous SNe Ia. We expect SN Ia counterparts to the D 6 model would leave these fingerprints for SN Ia observations.

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Section: Discussionmentioning

confidence: 74%

Three-dimensional Simulation of Double Detonations in the Double-degenerate Model for Type Ia Supernovae and Interaction of Ejecta with a Surviving White Dwarf Companion

Tanikawa

Nomoto

Nakasato

2018

ApJ

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“…(1) If the explosion of the two WDs in the DD scenario occurs as they dynamically interact, then the explosion is asymmetrical (e.g., Kashyap et al 2017;Pakmor et al 2012;Tanikawa et al 2015;van Rossum et al 2016), contradicting the structure of most SN Ia remnants (SNRs Ia) that tend to be spherical or axisymmetrical (e.g., Lopez et al 2011). In that respect I note that a surviving WD companion in the DDet scenario also leads to a SNR Ia that possesses non-spherical morphological features (e.g., Papish et al 2015).…”

Section: Merger To Explosion Delay (Med) Timementioning

confidence: 99%

Common envelope to explosion delay time of Type Ia supernovae

Soker

2019

Monthly Notices of the Royal Astronomical Society

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I study the rate of type Ia supernovae (SNe Ia) within about a million years after the assumed common envelope evolution (CEE) that forms the progenitors of these SNe Ia, and find that the population of SNe Ia with short CEE to explosion delay (CEED) time is ≈ few × 0.1 of all SNe Ia. I also claim for an expression for the rate of these SNe Ia that occur at short times after the CEE, t CEED 10 6 yr, that is different from that of the delay time distribution (DTD) billions of years after star formation. This tentatively hints that the physical processes that determine the short CEED times are different (at least to some extend) from those that determine the DTD at billions of years. To reach these conclusions I examine SNe Ia that interact with a circumstellar matter (CSM) within months after explosion, so called SNe Ia-CSM, and the rate of SNe Ia that on a time scale of tens to hundreds of years interact with a CSM that might have been a planetary nebula, so called SNe Ia inside a planetary nebula (SNIPs). I assume that the CSM in these populations results from a CEE, and hence this study is relevant mainly to the core degenerate (CD) scenario, to the double degenerate (DD) scenario, to the double detonation (DDet) scenario with white dwarf companions, and to the CEE-wind channel of the single degenerate (SD) scenario.

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“…Papish et al (2015) list two problems with the SES scenario. When confronting the scenarios with observations, as well as when trying to account for a specific observational property, it is imperative to consider all scenarios.…”

Section: Introductionmentioning

confidence: 99%

Type Ia supernova remnants: shaping by iron bullets

Tsebrenko

Soker

2015

Mon. Not. R. Astron. Soc.

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Using 2D numerical hydrodynamical simulations of type Ia supernova remnants (SNR Ia) we show that iron clumps few times denser than the rest of the SN ejecta might form protrusions in an otherwise spherical SNR. Such protrusions exist in some SNR Ia, e.g., SNR 1885 and Tycho. Iron clumps are expected to form in the deflagration to detonation explosion model. In SNR Ia where there are two opposite protrusions, termed 'ears, such as Kepler's SNR and SNR G1.9+0.3, our scenario implies that the dense clumps, or iron bullets, were formed along an axis. Such a preferred axis can result from a rotating white dwarf progenitor. If our claim holds, this offers an important clue to the SN Ia explosion scenario.

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The response of a helium white dwarf to an exploding Type Ia supernova

Cited by 28 publications

References 67 publications

Three-dimensional Simulation of Double Detonations in the Double-degenerate Model for Type Ia Supernovae and Interaction of Ejecta with a Surviving White Dwarf Companion

Three-dimensional Simulation of Double Detonations in the Double-degenerate Model for Type Ia Supernovae and Interaction of Ejecta with a Surviving White Dwarf Companion

Common envelope to explosion delay time of Type Ia supernovae

Type Ia supernova remnants: shaping by iron bullets

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