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Single Degenerate model is the most widely accepted progenitor model of typeIa supernovae (SNe Ia), in which a carbon-oxygen white dwarf (CO WD) accreteshydrogen-rich material from a main sequence or a slightly evolved star (WD +MS)to increase its mass, and explodes when its mass approaches the Chandrasekharmass limit. During the mass transfer phase between the two components, anoptically thick wind may occur and the material lost as the wind may exist ascircumstellar material (CSM). Searching the CSM around progenitor star ishelpful to discriminate different progenitor models of SNe Ia. Meanwhile, theCSM is a source of color excess.The purpose of this paper is to study the colorexcess produced from the single-degenerate progenitor model with opticallythick wind, and reproduce the distribution of color excesses of SNe Ia. Meng etal. (2009) systemically carried out binary evolution calculation of the WD +MSsystems for various metallicities and showed the parameters of the systemsbefore Roche lobe overflow and at the moment of supernova explosion in Meng &Yang (2009). With the results of Meng et al. (2009), we calculate the colorexcesses of SNe Ia at maximum light via a simple analytic method.We reproducesthe distribution of color excesses of SNe Ia by our binary population synthesisapproach if the velocity of the optically thick wind is taken to be of order ofmagnitude of 10 km s$^{\rm -1}$. However, if the wind velocity is larger than100 km s$^{\rm -1}$, the reproduction is bad.

Color excesses of type Ia supernovae from the single-degenerate channel model