The Progenitors of Type Ia Supernovae

By Bo Wang, Zhanwen Han. 2012

254 citations recorded by the source corpus.

Using binary population synthesis (BPS), we studied the birthrates of SNe Ia for two progenitor models - the single degenerate model and the double degenerate model. We find that the birthrates from both models are within a factor of a few comparable to those inferred observationally. For each model, we investigate different star-formation histories (single star burst or constant star formation), different metallicities (Z = 0.02, 0.004, 0.001), different parameters for the BPS model (mass transfer efficiency during stable mass transfer, common-envelope ejection parameters) and obtain the evolution of birthrates with time.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/74a19853b1acfa16a06646109ea7292aad5a8b81

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In Astronomy and Astrophysics

Citations in the corpus

Dawes Review 6: The Impact of Companions on Stellar Evolution (2016, background): “The most likely scenario is that type Ia supernovae are exploding carbon–oxygen WD with masses near the Chandrasekhar mass limit of about 1.4 M (Wang & Han, 2012).”
Observational probes of cosmic acceleration (2012, background): “The observed supernova population could have contributions from both channels (see Livio 1999 for a review of Type Ia SN mechanisms).”
The delay-time distribution of Type Ia supernovae from Sloan II (2012, background): “…DTDs have been proposed, whether based on detailed binary population synthesis (e.g. Yungelson & Livio 2000; Nelemans et al. 2001; Han & Podsiadlowski 2004; Mennekens et al. 2010; Meng et al. 2011; Ruiter et al. 2011; see Wang & Han 2012 for a review) or on some simple physical considerations.”
Three-dimensional pure deflagration models with nucleosynthesis and synthetic observables for type ia supernovae (2013, background): “However, it is possible that a CO WD may reach the Chandrasekhar mass by accretion from a helium-burning star (Iben et al. 1987; Ruiter et al. 2011; Wang & Han 2012), in which case one may expect to observe helium lines in the spectra (but, most of the helium will stably be burnt to carbon).”
Mind Your Ps and Qs: The Interrelation between Period (P) and Mass-ratio (Q) Distributions of Binary Stars (2016, background): “…primaries with closely orbiting stellar companions can evolve to produce X-ray binaries (Verbunt 1993), millisecond pulsars (Lorimer 2008), Type Ia (Wang & Han 2012) and possibly Type Ib/c (Yoon et al. 2010) supernovae, Algols (van Rensbergen et al. 2011), short (Nakar 2007) and perhaps long…”
Observational Clues to the Progenitors of Type Ia Supernovae (2013, background): “For each of these cases, different configurations are possible, depending on previous common enevelope and mass transfer phases (e.g., Wang & Han 2012).”