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Astron. Astrophys. 363, 1029-1039 (2000)

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Time-resolved optical studies and Doppler imaging of the eclipsing dwarf nova V893 Scorpii *

K. Matsumoto 1, R.E. Mennickent 2 and T. Kato 1

1 Kyoto University, Faculty of Science, Department of Astronomy, Sakyo-ku, Kyoto 606-8502, Japan (katsura@kusastro.kyoto-u.ac.jp; tkato@kusastro.kyoto-u.ac.jp)
2 Universidad de Concepción, Departamento de Física, Casilla 160-C, Concepción, Chile (rmennick@stars.cfm.udec.cl)

Received 2 September 1999 / Accepted 21 September 2000


We present time-resolved optical spectroscopic and photometric observations of the re-discovered dwarf nova V893 Sco. The orbital period of [FORMULA] derived from the radial velocity and equivalent width variations of the H[FORMULA] emission line is confirmed. The photometric light curves clearly show the eclipse of the accretion disk. A mass of the white dwarf [FORMULA]0.5-0.6[FORMULA] is derived from the orbital amplitude [FORMULA] and the eclipse constraint. The mass ratio is likely small enough to make V893 Sco an SU UMa-type dwarf nova, though this object has shown only normal outbursts in its light curve. Time-resolved Doppler maps for the emission lines show two isolated H[FORMULA] emission regions, which are associated with a strong hot spot and the irradiated secondary star.

Key words: accretion, accretion disks – stars: binaries: close – stars: individual: V893 Sco – stars: novae, cataclysmic variables

* Based on observations obtained at ESO La Silla Observatory (ESO Proposal 61.D-0395)

Send offprint requests to: K. Matsumoto

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© European Southern Observatory (ESO) 2000

Online publication: December 5, 2000