HS 2325+8205 - An Ideal Laboratory for Accretion Disk Physics

Bibcode
2012PASP..124..204P
DOI
10.1086/664959
Pyrzas, S.; Gänsicke, B. T.; Thorstensen, J. R.; Aungwerojwit, A.; Boyd, D.; Brady, S.; Casares, J.; Hickman, R. D. G.; Marsh, T. R.; Miller, I.; Ögmen, Y.; Pietz, J.; Poyner, G.; Rodríguez-Gil, P.; Staels, B.
Bibliographical reference

Publications of the Astronomical Society of the Pacific, Volume 124, issue 913, pp.204-211

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3
2012
Number of authors
15
IAC number of authors
2
Citations
9
Refereed citations
8
Description
We identify HS 2325+8205 as an eclipsing, frequently outbursting, dwarf nova with an orbital period of Porb = 279.841731(5) minutes. Spectroscopic observations are used to derive the radial velocity curve of the secondary star from absorption features and also from the Hα emission lines, originating from the accretion disk, yielding Ksec = Kabs = 237 ± 28 km s-1 and Kem = 145 ± 9 km s-1, respectively. The distance to the system is calculated to be 400(+200,-140) pc. A photometric monitoring campaign reveals an outburst recurrence time of ˜12--14 days. The combination of magnitude range (17--14 mag), high declination, and eclipsing nature and frequency of outbursts makes HS 2325+8205 the ideal system for ""real-time"" studies of the accretion disk evolution and behavior in dwarf nova outbursts.
Related projects
Representación de la variable cataclísmica SS Cygni (Chris Moran)
Binary Stars
The study of binary stars is essential to stellar astrophysics. A large number of stars form and evolve within binary systems. Therefore, their study is fundamental to understand stellar and galactic evolution. Particularly relevant is that binary systems are still the best source of precise stellar mass and radius measurements. Research lines
Pablo
Rodríguez Gil
In progress
Type
Refereed
Stellar & Interstellar Physics (FEEI)

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