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2002MNRAS.334..608V - Mon. Not. R. Astron. Soc., 334, 608-620 (2002/August-2)
Physical parameter eclipse mapping of the quiescent disc in V2051 Ophiuchi.
VRIELMANN S., STIENING R.F. and OFFUTT W.
Abstract (from CDS):
The quiescent disc (chromosphere) shows a prominent bright region with temperatures of 10500K around the impact region of the stream from the secondary with an extension towards smaller azimuths. The disc has a size of 0.53±0.03R_L1_and a mass accretion rate M{dot}=1015 to 1017g.s–1. The light curves must include an uneclipsed component, a hot chromosphere and/or a disc wind.
The PPEM method allows us to determine a new distance of 146±20pc, compatible with previous rough estimates. For the white dwarf we then reconstruct a temperature of 19600K, if the lower hemisphere of the white dwarf is occulted by the disc.
We suggest that the accretion disc is a sandwich of a cool, optically thick central disc with hot chromospheric layers on both sides, as was suggested for HT Cas. This chromosphere is the origin of the emission lines.
We find that although V2051 Oph is very similar to the SU UMa-type dwarf novae HT Cas, OY Car and Z Cha, there must be a substantial difference in order to explain its unique light curve. The reason for the difference could be a higher mass transfer rate caused by the more massive secondary, and/or a small but significant magnetic field of the white dwarf, just strong enough to disrupt the innermost disc.
Abstract Copyright: 2002 Blackwell Science Ltd
Journal keyword(s): accretion, accretion discs - binaries: eclipsing - stars: individual: V2051 Oph - novae, cataclysmic variables
Simbad objects: 5
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