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.
Referencia bibliográfica

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

Fecha de publicación:
3
2012
Número de autores
15
Número de autores del IAC
2
Número de citas
9
Número de citas referidas
8
Descripción
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.
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Estrellas Binarias
El estudio de las estrellas binarias es una parte esencial de la astrofísica estelar. Una gran parte de las estrellas de nuestra Galaxia y de otras galaxias se ha formado en sistemas binarios o múltiples, por lo que entender la estructura y evolución de estos sistemas es importante desde el punto de vista estelar y galáctico. Un aspecto en el que
Pablo
Rodríguez Gil
En ejecución
Tipo
Con árbitro
Física estelar e interestelar (FEEI)

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