A Model for a Peculiar SU Ursae Majoris-Type Dwarf Nova ER Ursae Majoris

Details A Model for a Peculiar SU Ursae Majoris-Type Dwarf Nova ER Ursae Majoris A Model for a Peculiar SU Ursae Majoris-Type Dwarf Nova ER Ursae Majoris

Apr 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995pasj...47l..11o&link_type=abstract

Publications of the Astronomical Society of Japan, v.47, p.L11-L14.

Astronomy and Astrophysics

Astronomy

44

Accretion Disks, Stars: Dwarf Novae, Stars: Individual (Er Uma), Stars: Su Uma Stars

Scientific paper

A cataclysmic variable star, ER Ursae Majoris (=PG 0943+521), was recently discovered by Kato and Kunjaya (1995) to be an SU UMa-type dwarf nova having an extremely short superoutburst cycle of 43 d. Here, we present light-curve simulations of this star based on the thermal-tidal instability model for SU UMa-type dwarf nova proposed by the present author (Osaki 1989, AAA 50.064.103). It is demonstrated that the observed light curve of this star is very well reproduced as the case of an SU UMa star having a high mass-transfer rate: near to the borderline between nova-like stars and SU UMa-type dwarf novae.

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