Dwarf Nova Outbursts. I. The UV Delay

Details Dwarf Nova Outbursts. I. The UV Delay Dwarf Nova Outbursts. I. The UV Delay

Dec 1998

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998aca....48..677s&link_type=abstract

Acta Astronomica, v.48, pp.677-693, (1998).

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25

Binaries: Close, Novae: Cataclysmic Variables

Scientific paper

Models of dwarf nova outbursts are calculated for a range of relevant parameters: the masses of the components which determine the orbital period and the radius of the disk, the mass transfer rate, and the viscosity parameter alpha. The visual (lambda 5500 A) and ultraviolet (lambda 1200 A) light curves are calculated using black body and Kurucz fluxes. The resulting UV delays show strong dependence on model parameters and, in particular, confirm the existence of a dichotomy between Type A and Type B outbursts. The model predicted UV delays agree quite well with observations, with the "best-fit" for alphahot between 0.1 and 0.2. Earlier, negative conclusions and the controversy around the "problem of UV delay" resulted primarily from incorrect outer boundary conditions and other model simplifications.

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