Compressional Heating of Accreting White Dwarfs and Classical Novae Ignition

Details Compressional Heating of Accreting White Dwarfs and Classical Novae Ignition Compressional Heating of Accreting White Dwarfs and Classical Novae Ignition

Jul 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002hst..prop.9517b&link_type=abstract

HST Proposal ID #9517

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Hst Proposal Id #9517 Hot Stars

Scientific paper

We are proposing a broad theoretical study of the compressional {and nuclear} heating of white dwarfs {WDs} accreting at rates relevant to cataclysmic variables {CVs}, where the fresh fuel is burned unstably in classical novae. Our work will yield the internal WD luminosity as a function of the time averaged accretion rate, < ngledot M angle, WD mass and metallicity. We also include the recurrent heating and cooling of the WD throughout the classical novae limit cycle in order to find the WD core temperature and accumulated mass at ignition. Comparing these theoretical masses to the observed ejected masses will tell us whether the WD mass in CVs is secularly increasing or decreasing and whether CVs can actually be Type Ia progenitors. Several Dwarf novae systems have been observed in quiescence with HST/STIS, when the accretion rate is low and the WD photosphere can be directly detected. Initial comparisons of our theoretical work to these observations is encouraging and supports Sion's suggestion that gravitational energy release within the WD rejuvenates an otherwise cold WD into a much hotter state. Our work has immediate relevance to: {1} the STIS observations noted above and {2} HST searches for quiescent, low < ngledot M angle CVs in globular clusters {where the optical and UV magnitudes are affected by the hot WD}.

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