COLLISIONS OF WHITE DWARFS AS A NEW PROGENITOR CHANNEL FOR TYPE Ia SUPERNOVAE

Rosswog, Stephan; Kasen, Daniel; Guillochon, James; Ramírez-Ruiz, E.

doi:10.1088/0004-637x/705/2/l128

Cited by 218 publications

(309 citation statements)

References 29 publications

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“…Finally, we do not consider triple star evolution, which produces double WD mergers in eccentric orbits (Hamers et al 2013) and, according to Rosswog et al (2009), is an alternative scenario to produce SNe Ia. Even though we do not investigate the rate of these channels, it is expected that similar uncertainties to those discussed in this work influence the rate.…”

Section: Other Uncertainties In the Resultsmentioning

confidence: 93%

Theoretical uncertainties of the Type Ia supernova rate

Claeys

Pols

Izzard

et al. 2014

A&A

281

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: 93%

Theoretical uncertainties of the Type Ia supernova rate

Claeys

Pols

Izzard

et al. 2014

A&A

281

326

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show abstract

“…The 847 keV emission also peaks at a later stage. Recently, several authors have explored the collision of two WDs in dense stellar systems as an alternate pathway to SN Ia within the family of DD scenarios (Rosswog et al 2009;Raskin et al 2009b). Shock-triggered thermonuclear explosions in such events are predicted to yield 56 Ni masses that are sufficient to power subluminous SNe Ia.…”

Section: Discussionmentioning

confidence: 99%

REVEALING TYPE Ia SUPERNOVA PHYSICS WITH COSMIC RATES AND NUCLEAR GAMMA RAYS

Horiuchi¹,

Beacom²

2010

ApJ

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Type Ia supernovae (SNe Ia) remain mysterious despite their central importance in cosmology and their rapidly increasing discovery rate. The progenitors of SNe Ia can be probed by the delay time between progenitor birth and explosion as SNe Ia. The explosions and progenitors of SNe Ia can be probed by MeV nuclear gamma rays emitted in the decays of radioactive nickel and cobalt into iron. We compare the cosmic star formation and SN Ia rates, finding that their different redshift evolution requires a large fraction of SNe Ia to have large delay times. A delay-time distribution of the form t −α with α = 1.0 ± 0.3 provides a good fit, implying that 50% of SNe Ia explode more than ∼1 Gyr after progenitor birth. The extrapolation of the cosmic SN Ia rate to z = 0 agrees with the rate we deduce from catalogs of local SNe Ia. We investigate prospects for gamma-ray telescopes to exploit the facts that escaping gamma rays directly reveal the power source of SNe Ia and uniquely provide tomography of the expanding ejecta. We find large improvements relative to earlier studies by Gehrels et al. in 1987 andWoosley in 1997 due to larger and more certain SN Ia rates and advances in gamma-ray detectors. The proposed Advanced Compton Telescope, with a narrow-line sensitivity ∼60 times better than that of current satellites, would, on an annual basis, detect up to ∼100 SNe Ia (3σ ) and provide revolutionary model discrimination for SNe Ia within 20 Mpc, with gamma-ray light curves measured with ∼10σ significance daily for ∼100 days. Even more modest improvements in detector sensitivity would open a new and invaluable astronomy with frequent SN Ia gamma-ray detections.

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“…The diversity of SNe Ia may reflect the diversities of the explosion mechanisms (e.g., Jordan et al 2008;Kasen et al 2009;Bildsten et al 2007) and the progenitors. Some recent works for the latter differences include the companion's mass and metallicity in the single-degenerate scenario (e.g., Hachisu et al 2008) and the case of collision in the double-degenerate scenario (e.g., Rosswog et al 2009;Raskin et al 2009). …”

Section: Introductionmentioning

confidence: 99%