Fundamental Parameters of White Dwarfs in Close Binaries with Late-Type Stars

Details Fundamental Parameters of White Dwarfs in Close Binaries with Late-Type Stars Fundamental Parameters of White Dwarfs in Close Binaries with Late-Type Stars

Jul 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996hst..prop.6615v&link_type=abstract

HST Proposal ID #6615

Computer Science

Hst Proposal Id #6615 Hot Stars

Scientific paper

White dwarfs in close binaries, in a degenerate pair or with a main sequence companion, emerge from a common envelope phase, concomitant with the passage of the most evolved component through the asymptotic giant branch. The properties of the present-day binary are dictated by the efficiency of the momentum transfer leading to orbital shrinkage and mass ejection from the system {PN}. Little is known of this process. Three new close binaries similar to the prototypical system Feige 24 {P=4.2d} consisting of a hot white dwarf star and a late-type companion {dM} have been identified in extreme ultraviolet all-sky surveys {EUVE J0720-317, EUVE J1016-053, EUVE J2013+400}; these objects may represent a dominant phase of white dwarf evolution. We have completed accurate radial velocity studies of the main sequence companion in the three new systems using echelle spectroscopy at Lick Observatory from which we derived accurate orbital ephemerides and mass functions. Extreme Ultraviolet Explorer spectroscopy of the system EUVE J1016-053 also revealed a peculiar abundance pattern in the white dwarf atmosphere, possibly the signature of intense accretion from the close mass-losing companion. We show that GHRS observations will solve the question of the peculiar surface abundance of the accreting white dwarf and also accurately solve the mass function of the system and constrain models of close binary evolution.

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