PG 0308 + 096 and PG 1026 + 002 - Two new short period binary stars resulting from common-envelope evolution

Details PG 0308 + 096 and PG 1026 + 002 - Two new short period binary stars resulting from common-envelope evolution PG 0308 + 096 and PG 1026 + 002 - Two new short period binary stars resulting from common-envelope evolution

May 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993aj....105.1945s&link_type=abstract

Astronomical Journal (ISSN 0004-6256), vol. 105, no. 5, p. 1945-1955.

Astronomy and Astrophysics

Astronomy

45

Binary Stars, H Alpha Line, Main Sequence Stars, Stellar Spectrophotometry, Ultraviolet Spectroscopy, White Dwarf Stars, Orbital Velocity, Radial Velocity, Spectral Line Width, Stellar Mass

Scientific paper

Ultraviolet spectroscopy, optical spectroscopy, and spectrophotometry have been used to study the excess UV stars PG 0308 + 096 and PG 1026 + 002. Both objects are short-period binary systems, each containing a DA white dwarf star and a dM star. Orbital periods of approximately 0.284 day for PG 0308 + 096, and aproximately 0.597 day for PG 1026, have been found by spectroscopic analysis of the H-alpha emission line. Ly-alpha and Balmer line profile fitting were used to estimate the mass of white dwarf stars; mass estimates for the dM stars are based on their spectral types. The orbital inclinations are derived from these masses, the periods, and amplitudes of the H-alpha radial velocity curves. The equivalent width of the H-alpha emission line, in each binary system, varies with the orbital phase in such a manner as to imply that it arises, in large part at least, from the hemisphere of the M star that faces the white dwarf star.

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