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Astron. Astrophys. 337, 472-476 (1998)


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The orbital period of the SU Ursae Majoris star AK Cancri *

J. Arenas ** and R.E. Mennickent

Departamento de Física, Facultad de Ciencias Físicas y Matemáticas, Universidad de Concepción, Casilla 4009, Concepción, Chile (rmennick@stars.cfm.udec.cl)

Received 9 March 1998 / Accepted 23 June 1998

Abstract

A time resolved spectroscopic study of the SU UMa subtype dwarf nova AK Cancri is presented. An orbital period of [FORMULA] and a radial velocity half-amplitude of [FORMULA] 50(3) km s-1 were obtained from the radial velocity variations of the H[FORMULA] emission line. Assuming various observational constraints, we deduced a most likely mass ratio of [FORMULA] and stellar masses of [FORMULA] and [FORMULA], for the primary and secondary star, respectively. In addition, the dynamical solution indicates a low orbital inclination ([FORMULA]).

Key words: accretion, accretion disks – stars: fundamental parameters – stars: individual: AK Cnc – stars: novae, cataclysmic variables

* Based on observations obtained at Las Campanas Observatory, Chile
** Present Address: Department of Physics, Keele University, Keele, Staffordshire ST5 5BG, UK (jla@astro.keele.ac.uk)

Send offprint requests to: J. Arenas

© European Southern Observatory (ESO) 1998

Online publication: August 17, 1998

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