Common Envelope to Explosion Delay time Distribution (CEEDTD) of Type Ia Supernovae

Soker, Noam

doi:10.1088/1674-4527/ac4d25

Cited by 8 publications

(6 citation statements)

References 121 publications

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“…Interestingly, these population properties are very similar to what has been inferred for SNe Iax (Foley et al 2013;Meng & Podsiadlowski 2018;) but also for some high-velocity (e.g., Pan 2020;Zeng et al 2021) and normal SNe Ia (Maoz & Badenes 2010;Soker 2022). SNe Iax in particular, present some properties that make them particularly attractive as potential ONe SN Ia counterparts.…”

Section: Summary and Discussionsupporting

confidence: 81%

“…This mass loss history will likely create a dense metal-rich circumstellar material (CSM) that can subsequently interact with the SN ejecta. This presents some similarities to the "core-denegerate" SN Ia scenario (e.g., Wang et al 2017;Soker 2019Soker , 2022. However, binary interactionsinvolving these stars with the most extended envelopes-may occur leading to a more diverse CSM spectrum.…”

Section: Summary and Discussionmentioning

confidence: 55%

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Thermonuclear and electron-capture supernovae from stripped-envelope stars

Chanlaridis

Antoniadis

Aguilera-Dena

et al. 2022

A&A

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Context. When stripped from their hydrogen-rich envelopes, stars with initial masses between ∼7 and 11 M ⊙ may develop massive degenerate cores and collapse. Depending on the final structure and composition, the outcome can range from a thermonuclear explosion, to the formation of a neutron star in an electron-capture supernova (ECSN). It has recently been demonstrated that stars in this mass range may be more prone to disruption than previously thought: they may initiate explosive oxygen burning when their central densities are still below ρ c ≲ 10 9.6 g cm −3 . At the same time, their envelopes expand significantly, leading to the complete depletion of helium. This combination makes them interesting candidates for type Ia supernovae-which we call (C)ONe SNe Iaand this might have broader implications for the formation of neutron stars via ECSNe. Aims. To constrain the observational counterparts of (C)ONe SNe Ia and the key properties that enable them, it is crucial to constrain the evolution, composition, and precollapse structure of their progenitors, as well as the evolution of these quantities with cosmic time. In turn, this requires a detailed investigation of the final evolutionary stages preceding the collapse, and their sensitivity to input physics. Methods. Here, we modeled the evolution of 252 single, nonrotating helium stars covering the initial mass range 0.8-3.5 M ⊙ , with metallicities between Z = 10 −4 and 0.02, and overshoot efficiency factors from f OV = 0.0 to 0.016 across all convective boundaries. We used these models to constrain several properties of these stars, including their central densities, compositions, envelope masses, and radii at the onset explosive oxygen ignition, as well as the final outcome as a function of initial helium star mass. We further investigate the sensitivity of these properties to mass loss rate assumptions using an additional grid of 110 models with varying wind efficiencies.Results. We find that helium star models with masses between ∼1.8 and 2.7 M ⊙ are able to evolve onto 1.35-1.37 M ⊙ (C)ONe cores that initiate explosive burning at central densities between log 10 (ρ c /g cm −3 ) ∼ 9.3 and 9.6. We constrained the amount of residual carbon retained after core carbon burning as a function of initial conditions, and conclude that it plays a critical role in determining the final outcome: Chandrasekhar-mass degenerate cores that retain more than approximately 0.005 M ⊙ of carbon result in (C)ONe SNe Ia, while those with lower carbon mass become ECSNe. We find that (C)ONe SNe Ia are more likely to occur at high metallicities, whereas at low metallicities ECSNe dominate. However, both SN Ia and ECSN progenitors expand significantly during the final evolutionary stages, so that for the most extended models, a further binary interaction may occur. We constrain the relative ratio between (C)ONe SNe Ia and SNe Ib/c to be 0.17-0.30 at Z = 0.02, and 0.03-0.13 at Z ≤ 10 −3 . Conclusions. We conclude with a discussion on potential observational properties of (C)ONe SNe Ia ...

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Section: Summary and Discussionsupporting

confidence: 81%

Section: Summary and Discussionmentioning

confidence: 55%

Thermonuclear and electron-capture supernovae from stripped-envelope stars

Chanlaridis

Antoniadis

Aguilera-Dena

et al. 2022

A&A

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“…Condition 2 (equation 2) does not impose a strong limit on pre-explosion LTP/VLTP if we consider that, crudely, ≈ 50% of SNe Ia might obey this condition (Soker 2022). It is Condition 1 (equation 1) that strongly constrains the number of pre-explosion LTP/VLTP.…”

Section: A Merger To Explosion Delay (Med) Timementioning

confidence: 99%

“…The explosion of a SN inside a planetary nebula is termed SNIP. In (Soker 2022) I crudely deduced by analysing observations that SNIPs account for ≈ 50% of all normal SNe Ia (i.e., not including peculiar SNe Ia).…”

Section: Relevant Timescalesmentioning

confidence: 99%

Pre-explosion helium shell flash in type Ia supernovae

Soker

2022

Preprint

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I study the possibility that within the frame of the core degenerate (CD) scenario for type Ia supernovae (SNe Ia) the merger process of the core of the asymptotic giant branch (AGB) star and the white dwarf (WD) maintains an envelope mass of ≈ 0.03M ⊙ that causes a later helium shell flash. I estimate the number of pre-explosion helium shell flash events to be less than few per cents of all CD scenario SNe Ia. A helium shell flash while the star moves to the left on the HR diagram as a post-AGB star (late thermal pulse-LTP) or along the WD cooling track (very-LTP) causes the star to expand and become a 'born again' AGB star. Merger remnants exploding while still on the AGB form peculiar SNe Ia or peculiar SNe II (if hydrogen is detected), while an explosion inside an inflated born-again star results in an early flux excess in the light curve of the SN Ia. The fraction of systems that might show an early flux excess due to LTP/VLTP is < few × 10 −4 of all SNe Ia, much below the observed fraction. In the frame of the CD scenario SNe Ia with early flux excess result from SN ejecta collision with planetary nebula fallback gas, or from mixing of 56 Ni to the outer regions of the SN ejecta. Ongoing sky surveys might find about one case per year where LTP/VLTP influences the SN light curve.

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“…Condition 2 (Equation ( 2)) does not impose a strong limit on pre-explosion LTP/VLTP if we consider that, crudely, ≈50% of SNe Ia might obey this condition (Soker 2022). It is Condition 1 (Equation ( 1)) that strongly constrains the number of pre-explosion LTP/VLTPs.…”

Section: A Merger To Explosion Delay (Med) Timementioning

confidence: 99%

Pre-explosion Helium Shell Flash in Type Ia Supernovae

Soker¹

2022

Res. Astron. Astrophys.

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I study the possibility that within the frame of the core degenerate (CD) scenario for type Ia supernovae (SNe Ia) the merger process of the core of the asymptotic giant branch (AGB) star and the white dwarf (WD) maintains an envelope mass of $\approx 0.03 M_\odot$ that causes a later helium shell flash. I estimate the number of pre-explosion helium shell flash events to be less than few per cents of all CD scenario SNe Ia. A helium shell flash while the star moves to the left on the HR diagram as a post-AGB star (late thermal pulse---LTP) or along the WD cooling track (very-LTP) causes the star to expand and become a `born again’ AGB star. Merger remnants exploding while still on the AGB form \add{hydrogen-polluted} peculiar SNe Ia, while an explosion inside an inflated born-again star results in an early flux excess in the light curve of the SN Ia. The fraction of systems that might show an early flux excess due to LTP/VLTP is $< {\rm few} \times 10^{-4}$ of all SNe Ia, much below the observed fraction. In the frame of the CD scenario SNe Ia with early flux excess result from SN ejecta collision with planetary nebula fallback gas, or from mixing of $^{56}$Ni to the outer regions of the SN ejecta. Ongoing sky surveys might find about one case per year where LTP/VLTP influences the SN light curve.

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Common Envelope to Explosion Delay time Distribution (CEEDTD) of Type Ia Supernovae

Cited by 8 publications

References 121 publications

Thermonuclear and electron-capture supernovae from stripped-envelope stars

Thermonuclear and electron-capture supernovae from stripped-envelope stars

Pre-explosion helium shell flash in type Ia supernovae

Pre-explosion Helium Shell Flash in Type Ia Supernovae

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