Merging of Components in Close Binaries: Type Ia Supernovae, Massive White Dwarfs, and Ap stars

Details Merging of Components in Close Binaries: Type Ia Supernovae, Massive White Dwarfs, and Ap stars Merging of Components in Close Binaries: Type Ia Supernovae, Massive White Dwarfs, and Ap stars

2009-01-30

arxiv.org/abs/0901.4899v1

Astron.Rep.53:214-222,2009

Astronomy and Astrophysics

Astrophysics

Solar and Stellar Astrophysics

15 pages, 4 figures

Scientific paper

10.1134/S1063772909030032

The "Scenario Machine" (a computer code designed for studies of the evolution of close binaries) was used to carry out a population synthesis for a wide range of merging astrophysical objects: main-sequence stars with main-sequence stars; white dwarfs with white dwarfs, neutron stars, and black holes; neutron stars with neutron stars and black holes; and black holes with black holes.We calculate the rates of such events, and plot the mass distributions for merging white dwarfs and main-sequence stars. It is shown that Type Ia supernovae can be used as standard candles only after approximately one billion years of evolution of galaxies. In the course of this evolution, the average energy of Type Ia supernovae should decrease by roughly 10%; the maximum and minimum energies of Type Ia supernovae may differ by no less than by a factor of 1.5. This circumstance should be taken into account in estimations of parameters of acceleration of the Universe. According to theoretical estimates, the most massive - as a rule, magnetic - white dwarfs probably originate from mergers of white dwarfs of lower mass. At least some magnetic Ap and Bp stars may form in mergers of low-mass main sequence stars (<1.5 mass of the Sun) with convective envelopes.

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