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2003PASP..115.1308P - Publ. Astron. Soc. Pac., 115, 1308-1329 (2003/November-0)
Superhumps in cataclysmic binaries. XXIV. Twenty more dwarf novae.
PATTERSON J., THORSTENSEN J.R., KEMP J., SKILLMAN D.R., VANMUNSTER T., HARVEY D.A., FRIED R.E., JENSEN L., COOK L.M., REA R., MONARD B., McCORMICK J., VELTHUIS F., WALKER S., MARTIN B., BOLT G., PAVLENKO E., O'DONOGHUE D., GUNN J., NOVAK R., MASI G., GARRADD G., BUTTERWORTH N., KRAJCI T., FOOTE J. and BESHORE E.
Abstract (from CDS):
Periods, as usual, can be measured to high accuracy, and these are of special interest since they carry dynamical information about the binary. We still have not quite learned how to read the music, but a few things are clear. The fractional superhump excess {epsiv}[=(Psh-Po)/Po] varies smoothly with Po. The scatter of the points about that smooth curve is quite low, and can be used to limit the intrinsic scatter in M1, the white dwarf mass, and the mass-radius relation of the secondary. The dispersion in M1does not exceed 24%, and the secondary-star radii scatter by no more than 11% from a fixed mass-radius relation. For the well-behaved part of {epsiv}(Po) space, we estimate from superhump theory that the secondaries are 18%±6% larger than theoretical ZAMS stars. This affects some other testable predictions about the secondaries: at a fixed Po, it suggests that the secondaries are (compared with ZAMS predictions) 40%±14% less massive, 12%±4% smaller, 19%±6% cooler, and less luminous by a factor of 2.5(7). The presence of a well-defined mass-radius relation, reflected in a well-defined {epsiv}(Po) relation, strongly limits effects of nuclear evolution in the secondaries.
Abstract Copyright: ∼
Journal keyword(s): accretion, accretion disks - Stars: Binaries: Close - Stars: Novae, Cataclysmic Variables - stars: individual (AO Octantis) - Stars: Individual: Constellation Name: BC Ursae Majoris - stars: individual (GX Cassiopeiae) - stars: individual (HO Delphini) - stars: individual (HV Virginis) - stars: individual (KK Telescopii) - stars: individual (KS Ursae Majoris) - stars: individual (KV Andromedae) - stars: individual (KV Dracnonis) - stars: individual (LL Andromedae) - stars: individual (MM Hydrae) - stars: individual (NY Serpentis) - stars: individual (QW Serpentis) - stars: individual (RX J1155.4-5641) - stars: individual (RZ Leonis) - stars: individual (RZ Sagittae) - stars: individual (TU Crateris) - stars: individual (V2051 Ophiuchi) - stars: individual (WX Ceti) - stars: individual
Simbad objects: 26
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