Why does RZ Leonis Minoris, and unusual SU UMa star, have such a short supercycle?

Details Why does RZ Leonis Minoris, and unusual SU UMa star, have such a short supercycle? Why does RZ Leonis Minoris, and unusual SU UMa star, have such a short supercycle?

Aug 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995pasj...47l..25o&link_type=abstract

PASJ: Publications of the Astronomical Society of Japan (ISSN 0004-6264), vol. 47, no. 3, p. L25-L29

Astronomy and Astrophysics

Astronomy

36

Accretion Disks, Dwarf Novae, Mass Transfer, Stellar Mass Ejection, Tides, Angular Momentum, Light Curve, Stellar Models, Torque

Scientific paper

A new group of extreme SU UMa-type dwarf novae called either 'ER UMa (= PG 0943+521) stars' or 'RZ LMi stars,' has recently been discovered that exhibit extremely short superoutburst cycles (supercycles) of about 20-45 d. In particular, the star RZ LMi has a supercycle as short as 19 d. We examined the supercycle length by performing light-curve simulations based on the thermal-tidal instability model of SU UMa stars. It was demonstrated that an extremely short supercycle of RZ LMi may be reproduced if the strength of tidal torques during a superoutburst is much weaker in RZ LMi than in the star ER UMa with a supercylce of 43 d and in ordinary SU UMa stars.

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