Common envelope to explosion delay time of Type Ia supernovae

ABSTRACT I study the rate of Type Ia supernovae (SNe Ia) within about a million years after the assumed common envelope evolution (CEE) that forms the progenitors of these SNe Ia, and find that the population of SNe Ia with short CEE to explosion delay (CEED) time is ≈few × 0.1 of all SNe Ia. I also claim for an expression for the rate of these SNe Ia that occur at short times after the CEE ($t_{\rm CEED} \lesssim 10^6 {~\rm yr}$), which is different from that of the delay time distribution (DTD) billions of years after star formation. This tentatively hints that the physical processes that determine the short CEED time distribution (CEEDTD) are different (at least to some extent) from those that determine the DTD at billions of years. To reach these conclusions I examine SNe Ia that interact with a circumstellar matter (CSM) within months after explosion, so-called SNe Ia-CSM, and the rate of SNe Ia that on a time-scale of tens to hundreds of years interact with a CSM that might have been a planetary nebula, so-called SNe Ia inside a planetary nebula (SNIPs). I assume that the CSM in these populations results from a CEE, and hence this study is relevant mainly to the core-degenerate (CD) scenario, the double-degenerate (DD) scenario, the double-detonation (DDet) scenario with white dwarf companions, and to the CEE-wind channel of the single-degenerate (SD) scenario.

Download Full-text

Double White Dwarf Merger Rates

Proceedings of the International Astronomical Union ◽

10.1017/s1743921312015086 ◽

2011 ◽

Vol 7 (S281) ◽

pp. 223-224

Author(s):

Silvia Toonen ◽

Gijs Nelemans ◽

Simon Portegies Zwart

Keyword(s):

White Dwarf ◽

Delay Time ◽

Time Distribution ◽

White Dwarfs ◽

Type Ia Supernovae ◽

Common Envelope ◽

Cosmological Distance ◽

Type Ia ◽

Ia Supernovae

AbstractType Ia supernovae (SNe Ia) are very successfully used as standard candles on cosmological distance scales, but so far the nature of the progenitor(s) is unclear. A possible scenario for SNe Ia are merging carbon/oxygen white dwarfs with a combined mass exceeding the Chandrasekhar mass. We determine the theoretical rates and delay time distribution of these mergers for two different common envelope prescriptions and metallicities. The shape of the delay time distributions is rather insensitive to the assumptions. The normalization is a factor ~3–13 too low compared to observations.

Download Full-text

The delay time distribution of type Ia supernovae: theory and observation

Proceedings of the International Astronomical Union ◽

10.1017/s1743921310002486 ◽

2009 ◽

Vol 5 (S262) ◽

pp. 31-35

Author(s):

Dany Vanbeveren ◽

Nicki Mennekens ◽

Jean-Pierre De Greve ◽

Erwin De Donder

Keyword(s):

Delay Time ◽

Time Distribution ◽

Theoretical Models ◽

Roche Lobe ◽

Type Ia Supernovae ◽

Population Number ◽

Common Envelope ◽

Type Ia ◽

Red Giant ◽

Ia Supernovae

AbstractUsing a population number synthesis code, the theoretical time distributions of type Ia supernovae in starburst galaxies are calculated, using competing models for the formation of such events: the single degenerate (a white dwarf accreting matter from a late main sequence or red giant companion) and double degenerate (the merger of two white dwarfs) scenario. The code includes the latest results in determining the progenitors for both models. Examples are the mass stripping effect in the case of the single degenerate scenario and the differentiation between the α- (based on the balance of energy) and γ- (based on the balance of angular momentum) description of energy conversion during common envelope evolution of binaries. The shape and extent of the obtained delay time distributions critically depends on which formation scenario is used. Comparing these results to the latest observed distributions allows to draw conclusions about the constraints put on the theoretical models by these observations. We also specifically investigate the influence of the degree of conservatism during Roche lobe overflow on the delay time distribution. We conclude that the single degenerate scenario alone cannot reproduce the observed delay time distributions, and that most double degenerate type Ia supernovae are formed through a quasi-conservative Roche lobe overflow phase followed by spiral-in, as opposed to a double common envelope evolution.

Download Full-text

Delay Time Distribution Measurement of Type Ia Supernovae by the Subaru/XMM-Newton Deep Survey and Implications for the Progenitor

Publications of the Astronomical Society of Japan ◽

10.1093/pasj/60.6.1327 ◽

2008 ◽

Vol 60 (6) ◽

pp. 1327-1346 ◽

Cited By ~ 164

Author(s):

Tomonori Totani ◽

Tomoki Morokuma ◽

Takeshi Oda ◽

Mamoru Doi ◽

Naoki Yasuda

Keyword(s):

Delay Time ◽

Time Distribution ◽

Type Ia Supernovae ◽

Distribution Measurement ◽

Type Ia ◽

Deep Survey ◽

Ia Supernovae

Download Full-text

Delay-Time Distribution of Type-Ia Supernovae: Theory versus Observation

10.1063/1.3536376 ◽

2010 ◽

Author(s):

Nicki Mennekens ◽

Dany Vanbeveren ◽

Jean-Pierre De Greve ◽

Erwin De Donder ◽

Vicky Kologera ◽

...

Keyword(s):

Delay Time ◽

Time Distribution ◽

Type Ia Supernovae ◽

Type Ia ◽

Theory Versus ◽

Ia Supernovae

Download Full-text

The delay-time distribution of Type Ia supernovae: a comparison between theory and observation

Astronomy and Astrophysics ◽

10.1051/0004-6361/201014115 ◽

2010 ◽

Vol 515 ◽

pp. A89 ◽

Cited By ~ 83

Author(s):

N. Mennekens ◽

D. Vanbeveren ◽

J. P. De Greve ◽

E. De Donder

Keyword(s):

Delay Time ◽

Time Distribution ◽

Type Ia Supernovae ◽

Type Ia ◽

Ia Supernovae

Download Full-text

The demographics of neutron star – white dwarf mergers

Astronomy and Astrophysics ◽

10.1051/0004-6361/201833164 ◽

2018 ◽

Vol 619 ◽

pp. A53 ◽

Cited By ~ 19

Author(s):

S. Toonen ◽

H. B. Perets ◽

A. P. Igoshev ◽

E. Michaely ◽

Y. Zenati

Keyword(s):

Delay Time ◽

Time Distribution ◽

Initial Conditions ◽

Population Synthesis ◽

Physical Processes ◽

Common Envelope ◽

Tail Distribution ◽

Wide Range ◽

Type Ia ◽

Ia Supernovae

Context. The mergers of neutron stars (NSs) and white dwarfs (WDs) could give rise to explosive transients, potentially observable with current and future transient surveys. However, the expected properties and distribution of such events is not well understood. Aims. Here we characterise the rates of such events, their delay-time distributions, their progenitors, and the distribution of their properties. Methods. We use binary population synthesis models and consider a wide range of initial conditions and physical processes. In particular we consider different common-envelope evolution models and different NS natal kick distributions. We provide detailed predictions arising from each of the models considered. Results. We find that the majority of NS–WD mergers are born in systems in which mass-transfer played an important role, and the WD formed before the NS. For the majority of the mergers the WDs have a carbon-oxygen composition (60−80%) and most of the rest are with oxygen-neon WDs. The time-integrated rates of NS–WD mergers are in the range of 3−15% of the type Ia supernovae (SNe) rate. Their delay-time distribution is very similar to that of type Ia SNe, but is slightly biased towards earlier times. They typically explode in young 100 Myr < τ < 1 Gyr environments, but have a tail distribution extending to long, gigayear-timescales. Models including significant kicks give rise to relatively wide offset distribution extending to hundreds of kiloparsecs. Conclusions. The demographic and physical properties of NS–WD mergers suggest they are likely to be peculiar type Ic-like SNe, mostly exploding in late-type galaxies. Their overall properties could be related to a class of recently observed rapidly evolving SNe, while they are less likely to be related to the class of Ca-rich SNe.

Download Full-text