Evolution of 3-9 M⊙ stars for Z = 0.001-0.03 and metallicity effects on type Ia supernovae

Recent observations have revealed that Type Ia supernovae (SNe Ia) are not perfect standard candles; they show variations in their absolute magnitudes, light-curve shapes, and spectra. The C/O ratio in the SNe Ia progenitors (C-O white dwarfs) may be related to this variation. In this work, we systematically investigate the effects of stellar mass (M) and metallicity (Z) on the C/O ratio and its distribution in the C-O white dwarfs by calculating stellar evolution from the main sequence through the end of the second dredge-up for M = 3-9 M. and Z = 0.001-0.03. We find that the total carbon mass fraction just before SN Ia explosion varies in the range 0.36-0.5. We also calculate the metallicity dependence of the main-sequence mass range of the SN Ia progenitor white dwarfs. Our results show that the maximum main-sequence mass to form C-O white dwarfs decreases significantly toward lower metallicity, and the number of SN Ia progenitors may be underestimated if metallicity effect is neglected. We discuss the implications of these results on the variation of SNe Ia, determination of cosmological parameters, luminosity function of white dwarfs, and galactic chemical evolution.