Stability and energetics of mass transfer in double white dwarfs

Details Stability and energetics of mass transfer in double white dwarfs Stability and energetics of mass transfer in double white dwarfs

Sep 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999a%26a...349l..17h&link_type=abstract

Astronomy and Astrophysics, v.349, p.L17-L20 (1999)

Astronomy and Astrophysics

Astrophysics

35

Instabilities, Stars: Binaries: Close, Stars: White Dwarfs

Scientific paper

The donor star in an interacting double white dwarf lies deep within the potential well of the accretor, a condition which both alters the minimum mass transfer rate needed to generate an Eddington luminosity, and limits the fraction of matter which can be driven from the binary in a super-Eddington wind. That mass loss itself alters the threshold condition for the onset of dynamical instability of the donor star. We show that, unless the mass of the accreting star is extremely near the Chandrasekhar limit, a significant fraction (exceeding 0.5 for accretors of mass < 1M_sun) must be retained, even when the nominal accretion luminosity far exceeds the Eddington limit. In super-Eddington accretion, the accreted envelope almost certainly extends beyond the orbit of the donor, and will trigger white dwarf merger in a common envelope.

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