Mass Transfer and Evolution of Compact Binaries

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Scientific paper

We present a study of key aspects of the evolution of binary stars with emphasis on binaries consisting of two white dwarf stars obeying the zero temperature mass radius relationship. The evolution of such systems is driven by the loss of angular momentum by gravitational wave radiation. Effects like mass transfer and other modes of angular momentum loss and redistribution influence the evolutionary fate of the binary, and can lead to a merger, the tidal disruption of one of the components or its survival as a long-lived AM Canum Venaticorum (AM CVn) type system. Our study takes into account some of these effects; like mass loss due to super-Eddington accretion, tides, accretion disk formation and direct impact accretion. We find that under some circumstances, the tidal coupling between the spin of the components and the orbit of the binary leads to oscillations in the orbital separation and the mass transfer rate. We also find that as compared to previous studies, a larger fraction of the systems should survive to form AM CVn type systems. Unless the donor star has a finite entropy such that the effective mass-radius relationship deviates significantly from that of a zero temperature white dwarf, we expect our results to be valid. Much of the formalism developed in this work would also apply to other mass-transferring binaries, such as cataclysmic variables and Algol systems.

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