Delay times and rates for Type Ia supernovae and thermonuclear explosions from double-detonation sub-Chandrasekhar mass models

Ruiter, Ashley J.; Belczyński, K.; Sim, Stuart; Hillebrandt, W.; Fryer, Christopher L.; Fink, Michael; Kromer, M.

doi:10.1111/j.1365-2966.2011.19276.x

Cited by 151 publications

(215 citation statements)

References 96 publications

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“…Maoz et al (2011) study the hosts of the local SNe found in the LOSS and find a prompt channel (with τ < 420 Myr) with 99% significance. Models of Ia explosions also show the possibility of such a channel (Nomoto et al 2009;Ruiter et al 2011). The Ia rates are then modelled with one prompt component, directly proportional to the SFH, and one delayed component.…”

Section: Delay Time Distributions For Ia Supernovaementioning

confidence: 99%

The rate of supernovae at redshift 0.1–1.0

Melinder

Dahlén

Trinchant

et al. 2012

A&A

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We present supernova rate measurements at redshift 0.1-1.0 from the Stockholm VIMOS Supernova Survey (SVISS). The sample contains 16 supernovae in total. The discovered supernovae have been classified as core collapse or type Ia supernovae (9 and 7, respectively) based on their light curves, colour evolution and host galaxy photometric redshift. at z = 0.62. All of these rate estimates have been corrected for host galaxy extinction, using a method that includes supernovae missed in infrared bright galaxies at high redshift. We use Monte Carlo simulations to make a thorough study of the systematic effects from assumptions made when calculating the rates and find that the most important errors come from misclassification, the assumed mix of faint and bright supernova types and uncertainties in the extinction correction. We compare our rates to other observations and to the predicted rates for core collapse and type Ia supernovae based on the star formation history and different models of the delay time distribution. Overall, our measurements, when taking the effects of extinction into account, agree quite well with the predictions and earlier results. Our results highlight the importance of understanding the role of systematic effects, and dust extinction in particular, when trying to estimate the rates of supernovae at moderate to high redshift.

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Section: Delay Time Distributions For Ia Supernovaementioning

confidence: 99%

The rate of supernovae at redshift 0.1–1.0

Melinder

Dahlén

Trinchant

et al. 2012

A&A

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“…Most of these discussions above focused on the Chandrasekhar mass model, in which the WDs explode as SNe Ia when their masses are close to the Chandrasekhar mass limit. However, the sub-Chandrasekhar mass model may still be able to explain SNe Ia such as 1991bg, as well as normal SNe Ia (Sim et al 2010;Ruiter et al 2011). In addition, observations of several very bright SNe Ia implied that their progenitor WDs might have a super-Chandrasekhar mass (Astier et al 2006;Howell et al 2006;Hicken et al 2007;Scalzo et al 2010;Yuan et al 2010;Tanaka et al 2010;Yamanaka et al 2010).…”

Section: Introductionmentioning

confidence: 99%

The birth rate of supernovae from double-degenerate and core-degenerate systems

Meng

Yang

2012

A&A

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Context. Some recent observations of the delay-time distribution (DTD) of Type Ia supernovae (SNe Ia) seem to uphold the doubledegenerate (DD) scenario as the progenitor model of SNe Ia, but the core-degenerate (CD) scenario remains a strong competitor to the DD one. Aims. We investigate the effects of metallicity and the different treatments of common envelope (CE) on the DTD of SNe Ia by considering the DD and CD scenarios, and check the suggestion that the total mass of DD system is the main dependent variable of Phillips relation. Methods. We perform a series of Monte Carlo simulations based on a rapid binary evolution code and consider two treatments of CE evolution, i.e. α-formalism and γ-algorithm. Results. We find that only when the α-formalism is considered with a high CE ejection efficiency, may the shape of the DTD for DD systems be consistent with that derived observationally, i.e. a power law of ∼t −1 , while the value of the birth rate of SNe Ia marginally matches observations. For the α-formalism with a low CE ejection efficiency and the γ-algorithm, neither the shape of the DTD nor the value of the birth rate can be compared with those of the observations. Metallicity may not have a significant influence on the shape of DTD, but a lower metallicity may lead to a slightly higher birth rate of SNe Ia by a factor of 2, especially for SNe Ia with long delay times. If the results for the single-degenerate (SD) channel are incorporated into those for the DTD, both the shape of DTD and its value may be closely consistent with observations for SNe Ia younger than 2.5 Gyr, and SD and DD channels provide comparable contributions to the total SNe Ia, while for SNe Ia with delay times longer than 2.5 Gyr, DD is the dominant channel and the birth rate is lower than that derived from observations by a factor up to about four. In addition, we calculate the evolutions of various integral parameters of DD systems, and do not find any one suitable to explain the correlation between the brightness of SNe Ia and its delay time. Moreover, there are three channels producing CD systems that may contribute a few SNe Ia, but the contribution of CD systems to the total SNe Ia is no more than 1%. Conclusions. There may be other channels or mechanisms contributing to SNe Ia with long delay times.

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“…Despite significant advances in the observational instruments and methods, the properties of low-mass companions (q0.3) around earlytype stars at intermediate orbital periods (P≈50-10 4 days) remain elusive. This region is especially interesting because low-mass X-ray binaries and millisecond pulsars that form in the galactic field (Kalogera & Webbink 1998;Kiel & Hurley 2006), as well as certain channels of Type Ia supernovae (Whelan & Iben 1973;Ruiter et al 2011), may evolve from extreme mass-ratio binaries at initially intermediate orbital periods (Figure 1). Although we investigate all portions of the binary parameter space, we are especially concerned with determining accurate companion statistics at intermediate orbital periods.…”

Section: Introductionmentioning

confidence: 99%

Mind Your Ps and Qs: The Interrelation between Period (P) and Mass-ratio (Q) Distributions of Binary Stars

Moe

Stefano

2017

ApJS

1,094

1,200

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We compile observations of early-type binaries identified via spectroscopy, eclipses, long-baseline interferometry, adaptive optics, common proper motion, etc. Each observational technique is sensitive to companions across a narrow parameter space of orbital periods P and mass ratios q=M comp /M 1 . After combining the samples from the various surveys and correcting for their respective selection effects, we find that the properties of companions to O-type and B-type main-sequence (MS) stars differ among three regimes. First, at short orbital periods P20days (separations a0.4 au), the binaries have small eccentricities e0.4, favor modest mass ratios á ñ » q 0.5, and exhibit a small excess of twins q>0.95. Second, the companion frequency peaks at intermediate periods log P (days)≈3.5 (a ≈ 10 au), where the binaries have mass ratios weighted toward small values q≈0.2-0.3 and follow a Maxwellian "thermal" eccentricity distribution. Finally, companions with long orbital periods log P (days)≈5.5-7.5 (a ≈ 200-5000 au) are outer tertiary components in hierarchical triples and have a mass ratio distribution across q≈0.1-1.0 that is nearly consistent with random pairings drawn from the initial mass function. We discuss these companion distributions and properties in the context of binary-star formation and evolution. We also reanalyze the binary statistics of solar-type MS primaries, taking into account that 30% ±10% of single-lined spectroscopic binaries likely contain white dwarf companions instead of low-mass stellar secondaries. The mean frequency of stellar companions with q>0.1 and log P (days)<8.0 per primary increases from 0.50±0.04 for solar-type MS primaries to 2.1±0.3 for O-type MS primaries. We fit joint probability density functions ¹ ( ) ( ) ( ) ( ) ( ) f M q P e f M f q f P f e , , , 1 1 to the corrected distributions, which can be incorporated into binary population synthesis studies.

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Delay times and rates for Type Ia supernovae and thermonuclear explosions from double-detonation sub-Chandrasekhar mass models

Cited by 151 publications

References 96 publications

The rate of supernovae at redshift 0.1–1.0

The rate of supernovae at redshift 0.1–1.0

The birth rate of supernovae from double-degenerate and core-degenerate systems

Mind Your Ps and Qs: The Interrelation between Period (P) and Mass-ratio (Q) Distributions of Binary Stars

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