Is SN 2006X from a WD + MS system with optically thick wind?

AbstractThe single-degenerate channel is widely accepted as the progenitors of typeIa supernovae (SNe Ia). Following the work of Meng, Chen & Han (2009),we reproduced the birth rate and age of supernovae like SN 2006X by thesingle-degenerate model (WD + MS) with an optically thick wind, whichmay imply that the progenitor of SN 2006X is a WD + MS system.Key words:binaries:close-stars:evolution-supernovae:general-individual (SN 2006X)1.Although type Ia supernovae (SNe Ia) showed their importance in de-termining cosmological parameters, e.g. Ω M and Ω Λ ((Riess et al. 1998;Perlmutter et al. 1999), the progenitor systems of SNe Ia have not beenconfidently identified yet (Hillebrandt & Niemeyer 2000; Leibundgut 2000).Two basic scenarios for the progenitor of SN Ia have been discussed over thelast three decades. One is a single degenerate (SD) model (Whelan & Iben1973; Nomoto, Thielemann & Yokoi 1984), in which a CO WD increases itsmass by accreting hydrogen- or helium-rich matter from its companion, andexplodes when its mass approaches the Chandrasekhar mass limit. The com-panion may be a main-sequence star (WD + MS) or a red-giant star (WD+ RG) (Yungelson et al. 1995; Li & van den Heuvel 1997; Hachisu et al.1999a,b; Nomoto et al. 1999, 2003; Langer et al. 2000; Han & Podsiadlowski2004; Chen & Li 2007, 2009; Han 2008; Meng, Chen & Han 2009; Lu¨ et al.2009, Wang et al. 2009a, b). An alternative is the double degenerate (DD)