Internal Conditions of Accreting White Dwarfs

Details Internal Conditions of Accreting White Dwarfs Internal Conditions of Accreting White Dwarfs

2002-09-10

arxiv.org/abs/astro-ph/0209197v1

Astronomy and Astrophysics

Astrophysics

4 pages, 1 figure, uses CRCKAPB.sty (included); to appear in the `NATO Science Series II - Mathematics, Physics and Chemistry'

Scientific paper

We explain the physics of compressional heating of the deep interior of an accreting white dwarf (WD) at accretion rates low enough so that the accumulated hydrogen burns unstably and initiates a classical nova (CN). In this limit, the WD core temperature (T_c) reaches an equilibrium value (T_c,eq) after accreting an amount of mass much less than the WD's mass. Once this equilibrium is reached, the compressional heating from within the envelope exits the surface. This equilibrium yields useful relations between the WD surface temperature, accretion rate and mass that can be employed to measure accretion rates from observed WD effective temperatures, thus testing binary evolution models for cataclysmic variables.

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