White dwarf radii and boundary-layer constraints in three dwarf novae

Details White dwarf radii and boundary-layer constraints in three dwarf novae White dwarf radii and boundary-layer constraints in three dwarf novae

Feb 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990mnras.242..606w&link_type=abstract

Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 242, Feb. 15, 1990, p. 606-615.

Astronomy and Astrophysics

Astronomy

35

Accretion Disks, Boundary Layers, Dwarf Novae, Light Curve, Radii, White Dwarf Stars, Stellar Models, Stellar Structure

Scientific paper

The structure of the boundary layer between the accretion disk and the white dwarf in three quiescent dwarf novae is studied with high S/N eclipse light curves obtained by phase folding 12-20 eclipses. Observations of the eclipses in Z Cha, OY Car, and HT Cas are compared with calculated models of the eclipse shapes of various white dwarf/boundary layer configurations. It is found that the most likely model for each system is an unocculted white dwarf with no boundary layer contributing significantly to the optical flux, or a white dwarf totally covered by an optically thick boundary layer. The implications of the results for the white dwarf radius and physical conditions in the boundary layers are discussed.

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