Accretion disk evaporation by a coronal siphon flow

Details Accretion disk evaporation by a coronal siphon flow Accretion disk evaporation by a coronal siphon flow

Aug 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994a%26a...288..175m&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 288, no. 1, p. 175-182

Astronomy and Astrophysics

Astrophysics

281

Accretion Disks, Dwarf Novae, Mass Flow, Stellar Coronas, Ultraviolet Emission, White Dwarf Stars, X Rays, Boundary Conditions, Mass Flow Rate, Mathematical Models, Stellar Models, Stellar Winds, Temperature Distribution, X Ray Spectra

Scientific paper

We study the structure of a corona above a dwarf nova accretion disk. The interaction between the cool disk and the hot corona is investigated with a one-zone model. The result is that a siphon flow evaporates the corona. The material partially accretes through the coronal layers on to the white dwarf, partially is lost via a wind. Consequences are a hole in the inner accretion disk near the white dwarf and therefore a retarded change of the disk to the hot state in the beginning of an outburst. This shows up as a delay of the UV radiation.

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