scholarly journals Type-Ia Supernovae: New Clues to their Progenitors from the Delay Time Distribution

2010 ◽  
Author(s):  
Dan Maoz ◽  
Vicky Kologera ◽  
Marc van der Sluys
Keyword(s):  
Delay Time ◽  
Time Distribution ◽  
Type Ia Supernovae ◽  
Type Ia ◽  
Ia Supernovae

scholarly journals Common envelope to explosion delay time of Type Ia supernovae

2019 ◽  
Vol 490 (2) ◽  
pp. 2430-2435 ◽  
Author(s):  
Noam Soker
Keyword(s):  
Delay Time ◽  
Planetary Nebula ◽  
Time Distribution ◽  
Circumstellar Matter ◽  
Type Ia Supernovae ◽  
Common Envelope ◽  
Type Ia ◽  
Explosion Delay ◽  
Ia Supernovae ◽  
Short Times

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.

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

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

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

2010 ◽  
Vol 515 ◽  
pp. A89 ◽  
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

scholarly journals Supernovae in the Subaru Deep Field: the rate and delay-time distribution of Type Ia supernovae out to redshift 2

2011 ◽  
Vol 417 (2) ◽  
pp. 916-940 ◽  
Author(s):  
O. Graur ◽  
D. Poznanski ◽  
D. Maoz ◽  
N. Yasuda ◽  
T. Totani ◽  
...  
Keyword(s):  
Delay Time ◽  
Time Distribution ◽  
Type Ia Supernovae ◽  
Type Ia ◽  
Ia Supernovae

scholarly journals The delay-time distribution of Type Ia supernovae from Sloan II

2012 ◽  
Vol 426 (4) ◽  
pp. 3282-3294 ◽  
Author(s):  
Dan Maoz ◽  
Filippo Mannucci ◽  
Timothy D. Brandt
Keyword(s):  
Delay Time ◽  
Time Distribution ◽  
Type Ia Supernovae ◽  
Type Ia ◽  
Ia Supernovae

scholarly journals Double White Dwarf Merger Rates

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.

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

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.

scholarly journals The delay time distribution of Type-Ia supernovae in galaxy clusters: the impact of extended star-formation histories

2021 ◽  
Vol 502 (4) ◽  
pp. 5882-5895
Author(s):  
Jonathan Freundlich ◽  
Dan Maoz
Keyword(s):  
Star Formation ◽  
Galaxy Clusters ◽  
Power Law ◽  
Delay Time ◽  
Time Distribution ◽  
Type Ia Supernovae ◽  
Type Ia ◽  
Ia Supernovae ◽  
Star Formation Histories ◽  
Field Galaxy

ABSTRACT The delay time distribution (DTD) of Type-Ia supernovae (SNe Ia) is important for understanding chemical evolution, SN Ia progenitors, and SN Ia physics. Past estimates of the DTD in galaxy clusters have been deduced from SN Ia rates measured in cluster samples observed at various redshifts, corresponding to different time intervals after a presumed initial brief burst of star formation. A recent analysis of a cluster sample at z = 1.13–1.75 confirmed indications from previous studies of lower redshift clusters, that the DTD has a power-law form, DTD(t) = R1(t/Gyr)α, with amplitude R1, at delay $t=1\,\rm Gyr$, several times higher than measured in field-galaxy environments. This implied that SNe Ia are somehow produced in larger numbers by the stellar populations in clusters. This conclusion, however, could have been affected by the implicit assumption that the stars were formed in a single brief starburst at high z. Here, we re-derive the DTD from the cluster SN Ia data, but relax the single-burst assumption. Instead, we allow for a range of star-formation histories and dust extinctions for each cluster. Via MCMC modelling, we simultaneously fit, using stellar population synthesis models and DTD models, the integrated galaxy-light photometry in several bands, and the SN Ia numbers discovered in each cluster. With these more-realistic assumptions, we find a best-fitting DTD with power-law index $\alpha =-1.09_{-0.12}^{+0.15}$, and amplitude $R_1=0.41_{-0.10}^{+0.12}\times 10^{-12}\,{\rm yr}^{-1}\, {\rm M}_\odot ^{-1}$. We confirm a cluster-environment DTD with a larger amplitude than the field-galaxy DTD, by a factor ∼2–3 (at 3.8σ). Cluster and field DTDs have consistent slopes of α ≈ −1.1.

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