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Ultraviolet and optical observations of the mass-losing contact binary SV Centauri

Published online by Cambridge University Press:  12 April 2016

H. Drechsel ,
H.D. Radecke ,
J. Rahe ,
G. Rupprecht ,
W. Wargau  and
B. Wolf
H. Drechsel
Affiliation:
Remeis-Sternwarte Bamberg, Astronomisches Institut der Universität Erlangen-Nürnberg
H.D. Radecke
Affiliation:
Remeis-Sternwarte Bamberg, Astronomisches Institut der Universität Erlangen-Nürnberg
J. Rahe
Affiliation:
Remeis-Sternwarte Bamberg, Astronomisches Institut der Universität Erlangen-Nürnberg
G. Rupprecht
Affiliation:
Remeis-Sternwarte Bamberg, Astronomisches Institut der Universität Erlangen-Nürnberg
W. Wargau
Affiliation:
Remeis-Sternwarte Bamberg, Astronomisches Institut der Universität Erlangen-Nürnberg
B. Wolf
Affiliation:
Remeis-Sternwarte Bamberg, Astronomisches Institut der Universität Erlangen-Nürnberg

Extract

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SV Cen is a well known early-type contact binary. The less massive component is a slightly evolved B1 star. The secondary is of spectral type B4 III. The period of the system is P = 1.6585 days. SV Cen shows with Ṗ/P = -2 10-5 yr-1 one of the largest known period decreases. We carried out ground-based photoelectric and spectroscopic (coudé) observations at ESO, and high dispersion UV observations at VILSPA, with the aim

a) to derive new orbital parameters of SV Cen

b) to determine further epochs of minima (i.e. to study the period variations)

c) to look for possible mass loss indicators in the ultraviolet range.

Type
Session VIII - Effects of Mass Loss on the Evolution of Binary Stars
Information
International Astronomical Union Colloquium , Volume 59: Effects of Mass Loss on Stellar Evolution , 1981 , pp. 487 - 489
Copyright
Copyright © Reidel 1981

References

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