The core-degenerate scenario for the progenitors of Type Ia supernovae

Wang, Bo; Zhou, Wenchen; Zuo, Zhao-Yu; Li, Yin-Bi; Luo, Xia; Zhang, Jujia; Liu, Dongdong; Wu, Chenjie

doi:10.1093/mnras/stw2646

Cited by 18 publications

(14 citation statements)

References 76 publications

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“…This presents some similarities to the "core-denegerate" SN Ia scenario (e.g. Wang et al 2017;Soker 2019Soker , 2021. However, binary interactions-which are practically guaranteed, given how large these stars become (Figure 10)-may lead to a more diverse CSM spectrum.…”

Section: Shell Burning and Envelope Ejection Prior To Collapse Near-supporting

confidence: 53%

Thermonuclear and Electron-Capture Supernovae from Stripped-Envelope Stars

Chanlaridis¹,

Antoniadis²,

Aguilera-Dena³

et al. 2022

Preprint

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Context. When stripped from their hydrogen-rich envelopes, stars with initial masses between ∼7 and 11 M 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 been recently 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 Ia-and 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 pre-collapse 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 model the evolution of 252 single, non-rotating helium-stars covering the initial mass range 0.8-3.5 M , 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 use these models to constrain several properties of these stars, including their central densities, compositions and envelope masses at the time of explosive oxygen ignition, and 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 constrain 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 cores with residual carbon mass fractions of X min ( 12 C) 0.004 result in (C)ONe SNe Ia, while those with lower carbon mass fractions become ECSNe. We find that (C)ONe SNe Ia are more likely to occur at high metallicities, whereas at low metallicities ECSNe dominate. 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 and their progenitors. In the few thousand years leading to the explosion, at least some progenitors should be identifiable as luminous metal-rich supergiants, embedded in hydrogen-free circumstellar nebulae.

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Section: Shell Burning and Envelope Ejection Prior To Collapse Near-supporting

confidence: 53%

Thermonuclear and Electron-Capture Supernovae from Stripped-Envelope Stars

Chanlaridis¹,

Antoniadis²,

Aguilera-Dena³

et al. 2022

Preprint

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“…I here argue that at least those that occurs within a million years after the CEE come from the CD scenario. I do note thought that there are claims that the CD scenario contributes less than my estimate in the Table 1 (e.g., Wang et al 2017). ⋆ Summary of section 5.…”

Section: Delay Times and Their Implicationsmentioning

confidence: 84%

Supernovae Ia in 2019 (review): a rising demand for spherical explosions

Soker

2019

Preprint

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I review new studies of type Ia supernovae (SNe Ia) from 2019, and use these to improve the comparison between the five binary SN Ia scenarios. New low polarisation measurements solidify the claim that most SN Ia explosions are globally spherically symmetric (clumps are possible). Explosions by dynamical processes, like explosions that take place during a merger process of two white dwarfs (WDs) in the double degenerate (DD) scenario, or during an accretion process in the double detonation (DDet) scenario and in the single degenerate (SD) scenario, lead to non-spherical explosions, in contradiction with observations of normal SNe Ia. I argue that these (DD, DDet, SD) scenarios account mainly for peculiar SNe Ia. The explosion of a Chandrasekhar mass (M CH ) WD (deflagration to detonation process) has a global spherical structure that is compatible with observations. To reach spherical explosions, SN Ia scenarios should allow for a time delay between the formation of an M Ch -WD and its explosion. As such, I split the DD scenario to a channel without merger to explosion delay (MED) time (that forms mainly peculiar SNe Ia), and a channel with a MED, the DD-MED channel (scenario). I speculate that the main contributors to normal SNe Ia are the core degenerate (CD) scenario, the DD-MED scenario, both have M CH spherical explosions, and the DD scenario that has sub-C CH non-spherical explosions.

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“…However, it is completely unclear why young merger tends to have a strong magnetic field, and then lead to a short spin-down timescale (Ilkov & Soker 2012). In addition, the CD model is less possible to contribute to the majority of SNe Ia (Meng & Yang 2012;Wang et al 2017), although the argument on the contribution exists (Ilkov & Soker 2013).…”

Section: Dd Modelmentioning

confidence: 97%

High-velocity Feature as the Indicator of the Stellar Population of Type Ia Supernovae

Meng

2019

ApJ

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Although type Ia supernovae (SNe Ia) are very useful in many astrophysical fields, their exact nature is still unclear, e.g. the progenitor and explosion models. The high-velocity features (HVFs) in optical spectra of SNe Ia could provide some meaningful information to constrain the nature of SNe Ia. Here, I show strong evidence that the SNe Ia with strong CaII infrared triple (CaII IR3) HVF around maximum brightness associate with relatively younger population than those with weak CaII IR3 HVF, e.g. the SNe Ia with strong CaII IR3 HVF tend to occur in late-type galaxy, or early-type galaxy with significant star formation. In addition, using pixel statistics I find that the SNe Ia with strong maximum-light CaII IR3 HVF show a higher degree of association with star formation index, e.g. Hα or near-UV emission, than those with weak CaII IR3 HVF. Moreover, I find that the strength of the CaII IR3 HVF is linearly dependent on the difference of the absorption-weighted velocities between CaII IR3 and SiII 635.5 nm absorption lines, which then is a good index to diagnose whether or not there is a high-velocity component in the CaII IR3 absorption feature in the spectra of SNe Ia. I finally discussed the origin of the HVFs and the constraints from our discoveries on the progenitor model of SNe Ia.

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The core-degenerate scenario for the progenitors of Type Ia supernovae

Cited by 18 publications

References 76 publications

Thermonuclear and Electron-Capture Supernovae from Stripped-Envelope Stars

Thermonuclear and Electron-Capture Supernovae from Stripped-Envelope Stars

Supernovae Ia in 2019 (review): a rising demand for spherical explosions

High-velocity Feature as the Indicator of the Stellar Population of Type Ia Supernovae

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