Twelve years of IUE spectra of the interacting binary VV Cephei

Details Twelve years of IUE spectra of the interacting binary VV Cephei Twelve years of IUE spectra of the interacting binary VV Cephei

Oct 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991a%26as...90..175b&link_type=abstract

Astronomy and Astrophysics Supplement Series (ISSN 0365-0138), vol. 90, no. 1, Oct. 1991, p. 175-190.

Astronomy and Astrophysics

Astrophysics

9

Absorption Spectra, Eclipsing Binary Stars, Emission Spectra, Iue, Stellar Spectra, Ultraviolet Spectra, Accretion Disks, B Stars, Chromosphere, Companion Stars, High Temperature Gases, Hot Stars, Line Spectra, M Stars, Mass Transfer, Red Shift

Scientific paper

All well-exposed high-resolution IUE spectra obtained of the eclipsing binary system VV Cephei (M2Iabep + B) are examined. High-temperature absorption features attributable to the hot companion were detected, indicating that the companion (or the inner regions of its accretion disk) are not as hot as a B1-B2 star. Doubling of Fe II (UV 1) lines, with an additional narrow component redshifted by about 60 km/sec, occurs only when the B star is behind the plane of the sky containing the M supergiant, suggesting the existence of mass transfer from the red to the blue star. Absorption features from neutral elements weaken dramatically during egress, while those from ionized elements remain at nearly constant strength. During egress from primary eclipse, the Mg II resonance doublet shows asymmetric double-peaked emission indicative of formation in an expanding chromosphere. It is concluded that the outer atmosphere of the M supergiant is highly clumped.

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