Determination of mass flow rates in AM Herculis binaries. I. General method and application to UZ Fornacis.

Details Determination of mass flow rates in AM Herculis binaries. I. General method and application to UZ Fornacis. Determination of mass flow rates in AM Herculis binaries. I. General method and application to UZ Fornacis.

Jun 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996a%26a...310..526r&link_type=abstract

Astronomy and Astrophysics, v.310, p.526-532

Astronomy and Astrophysics

Astrophysics

15

White Dwarfs, Stars: Mass-Loss, Stars: Magnetic Fields, Stars: Individual: Uz For, Novae, Cataclysmic Variables

Scientific paper

We compute cyclotron spectra of a magnetic white dwarf heated by a stream of free falling protons which loose their energy by Coulomb encounters with atmospheric electrons. Given the temperature structure of such atmosphere, we consider the variation of the field strength with height in the atmosphere. For a given surface field strength B, cyclotron spectra are then calculated as a function of the mass flow rate ˙(m). From a comparison with observed low-state spectra of the AM Herculis binary UZ For, we determine for the first time directly the range of mass flow rates in the accretion spot, 10^-4^<~˙(m)<~1g/cm^2^/s. The spot displays a core-halo structure, with the core(s) producing the higher and the halo the lower harmonics. The total low-state accretion rate of UZ For is ~3x10^13^g/s and the spot size is ~4x10^15^cm^2^. The best fit to the cyclotron spectrum is achieved with a two spot model (B_1_=~53MG, B_2_=~48MG) with the low field sub-spot contributing about 15% to the spectral flux.

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