Hostname: page-component-7c8c6479df-hgkh8 Total loading time: 0 Render date: 2024-03-29T12:08:17.028Z Has data issue: false hasContentIssue false

Long-Term Variability and Outburst Activity of FS Aurigae: Further Evidence for a Third Body in the System

Published online by Cambridge University Press:  23 April 2012

V. Neustroev
Affiliation:
Astronomy Division, Department of Physics, P.O. Box 3000, 90014 University of Oulu, Finland. email: vitaly@neustroev.net
G. Sjoberg
Affiliation:
American Assoc. of Variable Star Observers, 49 Bay State Road, Cambridge, MA 02138, USA
G. Tovmassian
Affiliation:
Instituto de Astronomia, UNAM, Apdo. Postal 877, Ensenada, Baja California, 22800 Mexico
S. Zharikov
Affiliation:
Instituto de Astronomia, UNAM, Apdo. Postal 877, Ensenada, Baja California, 22800 Mexico
T. Arranz Heras
Affiliation:
Observatorio “Las Pegueras”, Navas de Oro (Segovia), Spain
P. B. Lake
Affiliation:
American Assoc. of Variable Star Observers, 49 Bay State Road, Cambridge, MA 02138, USA
D. Lane
Affiliation:
Saint Marys University, Halifax, Nova Scotia, Canada The Abbey Ridge Observatory, Stillwater Lake, Nova Scotia, Canada
G. Lubcke
Affiliation:
American Assoc. of Variable Star Observers, 49 Bay State Road, Cambridge, MA 02138, USA
A. A. Henden
Affiliation:
American Assoc. of Variable Star Observers, 49 Bay State Road, Cambridge, MA 02138, USA
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

FS Aurigae is famous for a variety of uncommon and puzzling periodic photometric and spectroscopic variabilities which do not fit well into any of the established sub-classes of cataclysmic variables. Here we present preliminary results of long-term monitoring of the system, conducted during the 2010-2011 observational season. We show that the long-term variability of FS Aur and the character of its outburst activity may be caused by variations in the mass transfer rate from the secondary star as the result of eccentricity modulation of a close binary orbit induced by the presence of a third body on a circumbinary orbit.

Type
Contributed Papers
Copyright
Copyright © International Astronomical Union 2012

References

Georgakarakos, N. 2009, MNRAS, 392, 1253Google Scholar
Mazeh, T. & Shaham, J. 1979, A&A, 77, 145Google Scholar
Neustroev, V. V. 2002, A&A, 382, 974Google Scholar
Schreiber, M. R., Gänsicke, B. T., & Hessman, F. V. 2000, A&A, 358, 221Google Scholar
Tovmassian, G. H., et al. , 2003, PASP, 115, 725Google Scholar
Tovmassian, G. H., Zharikov, S. V., & Neustroev, V. V. 2007, ApJ, 655, 466Google Scholar
Tovmassian, G. H., et al. , 2010, arXiv:1009.5813Google Scholar