Optical spectroscopy of CH Cygni in 1985/86

Details Optical spectroscopy of CH Cygni in 1985/86 Optical spectroscopy of CH Cygni in 1985/86

Mar 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987ap%26ss.131..733m&link_type=abstract

(IAU, Colloquium on Cataclysmic Variables. Recent Multi-Frequency Observations and Theoretical Developments, 93rd, Bamberg, West

Astronomy and Astrophysics

Astrophysics

39

Eclipsing Binary Stars, M Stars, Stellar Mass Accretion, Stellar Spectrophotometry, Visible Spectrum, White Dwarf Stars, H Beta Line, H Gamma Line, Light Curve, Radial Velocity, Stellar Models

Scientific paper

Recent spectroscopic and photometric observations of CH Cyg are explained in terms of an eclipsing binary (with P = 5700 days) consisting of an M6 III star and an accreting white dwarf. The Roch lobe size is shown to be about two times larger than the radius of the cool giant, even at periastron, and accretion from the stellar wind is expected. The Balmer line profile variations noted during the 1985 minimum can be interpreted as the eclipse of a rotating disk or ring. Data suggest that sufficient mass can be accumulated in the disk during 10-12 yr to support the luminosity observed during the active phase. Aspects of the peculiar behavior of CH Cyg can be accounted for by the presence of an accretion cone with a disk inside and an ionization shock front outside.

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