Single degenerate supernova type Ia progenitors

Bours, Madelon C. P.; Toonen, Silvia; Nelemans, G.

doi:10.1051/0004-6361/201220692

Cited by 68 publications

(77 citation statements)

References 74 publications

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“…The differences that they find are caused by differences in the inherent assumptions in the codes, such as the initial-final mass relation, helium star evolution, the stability criterion of Roche-lobe overflowing stars and the mass transfer rate. In addition, Bours et al (2013) show that the lack of understanding of the retention efficiency of WDs gives an integrated rate of the SD channel which varies between <10 −7 and 1.5 × 10 −4 M −1 .…”

Section: Other Uncertainties In the Resultsmentioning

confidence: 97%

“…For this and other reasons, the retention efficiency of WDs is uncertain and several models exist which describe this efficiency , and reference therein). Rather than investigating the effect of different retention efficiencies, as was done by Bours et al (2013), we consider an extreme possibility where all mass transferred to the WD by RLOF remains on the WD and is burnt into carbon and oxygen (model F 1 ). We do not consider this unlimited accretion onto a WD as a realistic model, but it represents 1000 10000 Time ( an upper limit to the SD channel.…”

Section: Unlimited Accretion Onto Wdsmentioning

confidence: 99%

“…Finally, binary population synthesis (BPS) studies show that neither channel reproduces the observed SN Ia rate (e.g. Ruiter et al 2009;Mennekens et al 2010;Toonen et al 2012;Bours et al 2013;Chen et al 2012).…”

Section: Introductionmentioning

confidence: 99%

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Theoretical uncertainties of the Type Ia supernova rate

Claeys

Pols

Izzard

et al. 2014

A&A

280

326

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It is thought that Type Ia supernovae (SNe Ia) are explosions of carbon-oxygen white dwarfs (CO WDs). Two main evolutionary channels are proposed for the WD to reach the critical density required for a thermonuclear explosion: the single degenerate (SD) scenario, in which a CO WD accretes from a non-degenerate companion, and the double degenerate (DD) scenario, in which two CO WDs merge. However, it remains difficult to reproduce the observed SN Ia rate with these two scenarios. With a binary population synthesis code we study the main evolutionary channels that lead to SNe Ia and we calculate the SN Ia rates and the associated delay-time distributions. We find that the DD channel is the dominant formation channel for the longest delay times. The SD channel with helium-rich donors is the dominant channel at the shortest delay times. Our standard model rate is a factor of five lower than the observed rate in galaxy clusters. We investigate the influence of ill-constrained aspects of single-and binary-star evolution and uncertain initial binary distributions on the rate of Type Ia SNe. These distributions, as well as uncertainties in both helium star evolution and common envelope evolution, have the greatest influence on our calculated rates. Inefficient common envelope evolution increases the relative number of SD explosions such that for α ce = 0.2 they dominate the SN Ia rate. Our highest rate is a factor of three less than the galaxy-cluster SN Ia rate, but compatible with the rate determined in a field-galaxy dominated sample. If we assume unlimited accretion onto WDs, to maximize the number of SD explosions, our rate is compatible with the observed galaxy-cluster rate.

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Section: Other Uncertainties In the Resultsmentioning

confidence: 97%

Section: Unlimited Accretion Onto Wdsmentioning

confidence: 99%

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Theoretical uncertainties of the Type Ia supernova rate

Claeys

Pols

Izzard

et al. 2014

A&A

280

326

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“…Other observational constraints, such as cluster SN Ia rates, have recently found values closer to 2×10 −3 M −1 (Maoz & Badenes 2010)-still consistent within the large error bars. However, theoretical predictions from binary population synthesis models are frequently lower by factors of 10 or more (Bours et al 2013). This discrepancy between theory and observation remains one of the key concerns in the SN Ia progenitor problem.…”

Section: Dtd Model Fitting Resultsmentioning

confidence: 99%

TYPE Ia SUPERNOVA RATE MEASUREMENTS TO REDSHIFT 2.5 FROM CANDELS: SEARCHING FOR PROMPT EXPLOSIONS IN THE EARLY UNIVERSE

et al. 2014

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The Cosmic Assembly Near-infrared Deep Extragalactic Legacy Survey (CANDELS) was a multi-cycle treasury program on the Hubble Space Telescope (HST) that surveyed a total area of ∼0.25 deg 2 with ∼900 HST orbits spread across five fields over three years. Within these survey images we discovered 65 supernovae (SNe) of all types, out to z ∼ 2.5. We classify ∼24 of these as Type Ia SNe (SNe Ia) based on host galaxy redshifts and SN photometry (supplemented by grism spectroscopy of six SNe). Here we present a measurement of the volumetric SN Ia rate as a function of redshift, reaching for the first time beyond z = 2 and putting new constraints on SN Ia progenitor models. Our highest redshift bin includes detections of SNe that exploded when the universe was only ∼3 Gyr old and near the peak of the cosmic star formation history. This gives the CANDELS high redshift sample unique leverage for evaluating the fraction of SNe Ia that explode promptly after formation (<500 Myr). Combining the CANDELS rates with all available SN Ia rate measurements in the literature we find that this prompt SN Ia fraction is f P = 0.53 ±0.09 stat0.10 ±0.10 sys0.26 , consistent with a delay time distribution that follows a simple t −1 power law for all times t > 40 Myr. However, mild tension is apparent between ground-based low-z surveys and space-based high-z surveys. In both CANDELS and the sister HST program CLASH (Cluster Lensing And Supernova Survey with Hubble), we find a low rate of SNe Ia at z > 1. This could be a hint that prompt progenitors are in fact relatively rare, accounting for only 20% of all SN Ia explosions-though further analysis and larger samples will be needed to examine that suggestion.

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“…We find this scenario questionable, both with respect to its realization and its stability, although attractive if the main goal is to match the observed SN Ia rates with theoretical modelling based solely on the single-degenerate scenario. In a recent paper Bours et al (2013) demonstrated the strong dependence on the predicted SN Ia rates on the wind-stripping effect and on the mass accumulation (retention) efficiency of the accreting WD. and Liu et al (2010) studied the helium star donor channel for SNe Ia.…”

Section: Comparison To Previous Workmentioning

confidence: 98%

Evolution towards and beyond accretion-induced collapse of massive white dwarfs and formation of millisecond pulsars

Tauris

Sanyal

Yoon

et al. 2013

A&A

147

181

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Context. Millisecond pulsars (MSPs) are generally believed to be old neutron stars (NSs), formed via type Ib/c core-collapse supernovae (SNe), which have been spun up to high rotation rates via accretion from a companion star in a low-mass X-ray binary (LMXB). In an alternative formation channel, NSs are produced via the accretion-induced collapse (AIC) of a massive white dwarf (WD) in a close binary. Aims. Here we investigate binary evolution leading to AIC and examine if NSs formed in this way can subsequently be recycled to form MSPs and, if so, how they can observationally be distinguished from pulsars formed via the standard core-collapse SN channel in terms of their masses, spins, orbital periods and space velocities. Methods. Numerical calculations with a detailed stellar evolution code were used for the first time to study the combined pre-and post-AIC evolution of close binaries. We investigated the mass transfer onto a massive WD (treated as a point mass) in 240 systems with three different types of non-degenerate donor stars: main-sequence stars, red giants, and helium stars. When the WD is able to accrete sufficient mass (depending on the mass-transfer rate and the duration of the accretion phase) we assumed it collapses to form a NS and we studied the dynamical effects of this implosion on the binary orbit. Subsequently, we followed the mass-transfer epoch which resumes once the donor star refills its Roche lobe and calculated the continued LMXB evolution until the end. Results. We show that recycled pulsars may form via AIC from all three types of progenitor systems investigated and find that the final properties of the resulting MSPs are, in general, remarkably similar to those of MSPs formed via the standard core-collapse SN channel. However, as a consequence of the fine-tuned mass-transfer rate necessary to make the WD grow in mass, the resultant MSPs created via the AIC channel preferentially form in certain orbital period intervals. In addition, their predicted small space velocities can also be used to identify them observationally. The production time of NSs formed via AIC can exceed 10 Gyr which can therefore explain the existence of relatively young NSs in globular clusters. Our calculations are also applicable to progenitor binaries of SNe Ia under certain conditions.

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Single degenerate supernova type Ia progenitors

Cited by 68 publications

References 74 publications

Theoretical uncertainties of the Type Ia supernova rate

Theoretical uncertainties of the Type Ia supernova rate

TYPE Ia SUPERNOVA RATE MEASUREMENTS TO REDSHIFT 2.5 FROM CANDELS: SEARCHING FOR PROMPT EXPLOSIONS IN THE EARLY UNIVERSE

Evolution towards and beyond accretion-induced collapse of massive white dwarfs and formation of millisecond pulsars

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