Common envelope to explosion delay time of Type Ia supernovae

Soker, Noam

doi:10.1093/mnras/stz2817

Cited by 14 publications

(13 citation statements)

References 148 publications

(239 reference statements)

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“…Meng & Podsiadlowski (2017) proposed that a common envelope could be formed during such a RLOF phase. Moreover, the explosion of hybrid CONe WDs with a nondegenerate companion and within such a massive H-rich common envelope may explain most of the observational features as well as the rates of SNe Ia-CSM (Meng & Podsiadlowski 2018;Soker 2019).…”

Section: Implications Of Various Pre-explosion Mass-loss Modelsmentioning

confidence: 99%

The Interaction of Supernova 2018evt with a Substantial Amount of Circumstellar Matter -- An SN1997cy-like Event

Yang¹,

Baade²,

Hoêflich³

et al. 2022

Preprint

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A rare class of supernovae (SNe) is characterized by strong interaction between the ejecta and several solar masses of circumstellar matter (CSM) as evidenced by strong Balmer-line emission. Within the first few weeks after the explosion, they may display spectral features similar to overluminous Type Ia SNe, while at later phase their observation properties exhibit remarkable similarities with some extreme case of Type IIn SNe that show strong Balmer lines years after the explosion. We present polarimetric observations of SN 2018evt obtained by the ESO Very Large Telescope from 172 to 219 days after the estimated time of peak luminosity to study the geometry of the CSM. The nonzero continuum polarization decreases over time, suggesting that the mass loss of the progenitor star is aspherical. The prominent H emission can be decomposed into a broad, time-evolving component and an intermediate-width, static component. The former shows polarized signals, and it is likely to arise from a cold dense shell (CDS) within the region between the forward and reverse shocks. The latter is significantly unpolarized, and it is likely to arise from shocked, fragmented gas clouds in the H-rich CSM. We infer that SN 2018evt exploded inside a massive and aspherical circumstellar cloud. The symmetry axes of the CSM and the SN appear to be similar. SN 2018evt shows observational properties common to events that display strong interaction between the ejecta and CSM, implying that they share similar circumstellar configurations. Our preliminary estimate also suggests that the circumstellar environment of SN 2018evt has been significantly enriched at a rate of ∼ 0.1 M ⊙ yr −1 over a period of > 100 yr.

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Section: Implications Of Various Pre-explosion Mass-loss Modelsmentioning

confidence: 99%

The Interaction of Supernova 2018evt with a Substantial Amount of Circumstellar Matter -- An SN1997cy-like Event

Yang¹,

Baade²,

Hoêflich³

et al. 2022

Preprint

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“…Dallaporta 1973; Della Valle & Livio 1994;Howell 2001;Mannucci et al 2006) requiring two or more progenitor models, is being increasingly considered (e.g. Wang & Han 2012;Wang et al 2013;Livio & Mazzali 2018;Stritzinger et al 2018;Bear & Soker 2018;Soker 2019). The SINGG radial analysis favours long-lived, low mass binaries for at least the majority of Type Ia progenitor systems in star-forming galaxies.…”

Section: Low Masses For Type Ia Sne Binariesmentioning

confidence: 99%

The radial distribution of supernovae compared to star formation tracers

Audcent-Ross

Meurer

Audcent

et al. 2019

Monthly Notices of the Royal Astronomical Society

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Given the limited availability of direct evidence (pre-explosion observations) for supernova (SN) progenitors, the location of supernovae (SNe) within their host galaxies can be used to set limits on one of their most fundamental characteristics, their initial progenitor mass. We present our constraints on SN progenitors derived by comparing the radial distributions of 80 SNe in the SINGG and SUNGG surveys to the R-band, Hα, and UV light distributions of the 55 host galaxies. The strong correlation of Type Ia SNe with R-band light is consistent with models containing only low mass progenitors, reflecting earlier findings. When we limit the analysis of Type II SNe to apertures containing 90 per cent of the total flux, the radial distribution of these SNe best traces far ultraviolet (FUV) emission, consistent with recent direct detections indicating Type II SNe have moderately massive red supergiant progenitors. Stripped Envelope (SE) SNe have the strongest correlation with Hα fluxes, indicative of very massive progenitors (M * 20 M ). This result contradicts a small, but growing, number of direct detections of SE SN progenitors indicating they are moderately massive binary systems. Our result is consistent, however, with a recent population analysis suggesting binary SE SN progenitor masses are regularly underestimated. SE SNe are centralised with respect to Type II SNe and there are no SE SNe recorded beyond half the maximum disc radius in the optical and one third the disc radius in the ultraviolet. The absence of SE SNe beyond these distances is consistent with reduced massive star formation efficiencies in the outskirts of the host galaxies.

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“…The rotating super-Chandrasekhar WDs will experience a spin-down phase before they explode as SNe Ia (Justham 2011;Di Stefano & Kilic 2012;Hachisu et al 2012). The spin-down phase is also required by the observations of some SNe Ia (Soker 2018(Soker , 2019. However, at present, there are still many uncertainties on the spin-up/spin-down model, e.g.…”

Section: Methodsmentioning

confidence: 99%

“…However, at present, there are still many uncertainties on the spin-up/spin-down model, e.g. the spin-down timescale although a few 10 6 yr is favoured (Meng & Podsiadlowski 2018;Soker 2019), the exact time of the onset of the spindown phase (Meng & Podsiadlowski 2013) and WD growth pattern after M WD = 1.378 M ⊙ . So, following Meng & Li (2019), we define a pseudo spin-down timescale, τ sp , that is the time interval from when M WD = 1.378 M ⊙ to the time of supernova explosion.…”

Section: Methodsmentioning

confidence: 99%

Hot subdwarfs from the surviving companions of the white dwarf + main-sequence channel of Type Ia supernovae

Meng,

Luo

2021

Preprint

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Some surviving companions of type Ia supernovae (SNe Ia) from the white-dwarf + main-sequence (WD + MS) channel may evolve to hot subdwarfs. In this paper, we preformed stellar evolution calculations for surviving companions of close WD + MS systems in the spin-up/spin-down model and the canonical non-rotating model to map out the initial parameter spaces in the orbital period -secondary mass plane in which the surviving companions can evolve to hot subdwarfs. Based on these results, we carried out a series of binary population synthesis calculation to obtain the Galactic birth rate of the hot subdwarfs from the WD + MS channel, which is 2.3 − 6 × 10 −4 yr −1 for the spin-up/spin-down model and 0.7 − 3 × 10 −4 yr −1 for the canonical non-rotating model. We also show the distributions of some integral properties of the hot subdwarfs, e.g. the mass and the space velocity, for different models. In addition, comparing our results with the observations of the intermediate helium-rich (iHe-rich) hot subdwarfs, the hot subdwarfs from the WD + MS channel may explain some observational features of the iHe-rich hot subdwarfs, especially for those from the spin-up/spin-down model. Although we expect that the SN Ia channel can only contribute a small fraction of the iHe-rich hot subdwarf population, some of these may help to explain cases with unusual kinematics.

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Common envelope to explosion delay time of Type Ia supernovae

Cited by 14 publications

References 148 publications

The Interaction of Supernova 2018evt with a Substantial Amount of Circumstellar Matter -- An SN1997cy-like Event

The Interaction of Supernova 2018evt with a Substantial Amount of Circumstellar Matter -- An SN1997cy-like Event

The radial distribution of supernovae compared to star formation tracers

Hot subdwarfs from the surviving companions of the white dwarf + main-sequence channel of Type Ia supernovae

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