MONTE CARLO POPULATION SYNTHESIS OF POST-COMMON-ENVELOPE WHITE DWARF BINARIES AND TYPE Ia SUPERNOVA RATE

Binary population synthesis (BPS) studies provide a comprehensive way to understand the evolution of binaries and their end products. Close white dwarf (WD) binaries have crucial characteristics for examining the influence of unresolved physical parameters on binary evolution. In this paper, we perform Monte Carlo BPS simulations, investigating the population of WD/main-sequence (WD/MS) binaries and double WD binaries using a publicly available binary star evolution code under 37 different assumptions for key physical processes and binary initial conditions. We considered different combinations of the binding energy parameter (lambda(g): considering gravitational energy only; lambda(b): considering both gravitational energy and internal energy; and lambda(e): considering gravitational energy, internal energy, and entropy of the envelope, with values derived from the MESA code), CE efficiency, critical mass ratio, initial primary mass function, and metallicity. We find that a larger number of post-CE WD/MS binaries in tight orbits are formed when the binding energy parameters are set by lambda(e) than in those cases where other prescriptions are adopted. We also determine the effects of the other input parameters on the orbital periods and mass distributions of post-CE WD/MS binaries. As they contain at least one CO WD, double WD systems that evolved from WD/MS binaries may explode as type Ia supernovae (SNe Ia) via merging. In this work, we also investigate the frequency of two WD mergers and compare it to the SNe Ia rate. The calculated Galactic SNe Ia rate with lambda = lambda(e) is comparable to the observed SNe Ia rate, similar to 8.2 x 10(-5) yr(-1) - similar to 4 x 10(-3) yr(-1) depending on the other BPS parameters, if a DD system does not require a mass ratio higher than similar to 0.8 to become an SNe Ia. On the other hand, a violent merger scenario, which requires the combined mass of two CO WDs >= 1.6M(circle dot) and a mass ratio >0.8, results in a much lower SNe Ia rate than is observed.