The Effect of Metallicity on the Delay-Time Distribution of Type Ia Supernova

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.

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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

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Theoretical Delay Time Distributions

Proceedings of the International Astronomical Union ◽

10.1017/s1743921312015098 ◽

2011 ◽

Vol 7 (S281) ◽

pp. 225-231 ◽

Cited By ~ 2

Author(s):

Gijs Nelemans ◽

Silvia Toonen ◽

Madelon Bours

Keyword(s):

White Dwarf ◽

Delay Time ◽

Population Synthesis ◽

Research Groups ◽

Retention Efficiency ◽

Type Ia Supernova ◽

Type Ia

AbstractWe briefly discuss the method of population synthesis to calculate theoretical delay time distributions of Type Ia supernova progenitors. We also compare the results of different research groups and conclude that, although one of the main differences in the results for single degenerate progenitors is the retention efficiency with which accreted hydrogen is added to the white dwarf core, this alone cannot explain all the differences.

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THE SUPERNOVA DELAY TIME DISTRIBUTION IN GALAXY CLUSTERS AND IMPLICATIONS FOR TYPE-Ia PROGENITORS AND METAL ENRICHMENT

The Astrophysical Journal ◽

10.1088/0004-637x/722/2/1879 ◽

2010 ◽

Vol 722 (2) ◽

pp. 1879-1894 ◽

Cited By ~ 150

Author(s):

Dan Maoz ◽

Keren Sharon ◽

Avishay Gal-Yam

Keyword(s):

Galaxy Clusters ◽

Delay Time ◽

Time Distribution ◽

Metal Enrichment ◽

Type Ia

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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

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Galactic Chemical Evolution in the Context of the Recently Revealed SNe Ia Delay Time Distribution

Proceedings of the International Astronomical Union ◽

10.1017/s1743921312015153 ◽

2011 ◽

Vol 7 (S281) ◽

pp. 251-252

Author(s):

Takuji Tsujimoto

Keyword(s):

Chemical Evolution ◽

Delay Time ◽

Time Distribution ◽

Chemical Properties ◽

Thin Disk ◽

Chemical Enrichment ◽

Precise Knowledge ◽

The Galaxy ◽

Type Ia ◽

Ia Supernovae

AbstractThe Galaxy is composed of four distinct structures, i.e., halo, bulge, and thick and thin disks, that are formed and evolved on different timescales; thus accordingly the speeds of chemical enrichment are different from one another, which is imprinted in individual stellar abundances. To decipher them, precise knowledge of the timing of the release of nucleosynthesis materials from various production sites is critical. The delay time distribution (DTD) of Type Ia supernovae (SNe Ia), recently revealed by the SNe Ia surveys of external galaxies, is incorporated into the models of chemical evolution for each structure. Here we report that the observed chemical properties for the thin and thick disks are compatible with a new SNe Ia DTD, and suggests a close chemical connection between the two in the way that the thin disk is formed from gas left after thick disk formation. This nicely explains the lack of thin disk stars with [Fe/H] ≲ −0.8. In this new context, a top-heavy IMF for the bulge is firmly confirmed. Finally we discuss the possibility of some modification of the DTD that might be considered for the halo case.

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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

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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.

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