The ionization state of the winds from cataclysmic variables without classical boundary layers

Details The ionization state of the winds from cataclysmic variables without classical boundary layers The ionization state of the winds from cataclysmic variables without classical boundary layers

Feb 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993mnras.260..647h&link_type=abstract

Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 260, no. 3, p. 647-662.

Astronomy and Astrophysics

Astronomy

29

Accretion Disks, Boundary Layers, Cataclysmic Variables, Photoionization, Stellar Models, Stellar Winds, Radiative Transfer, Resonance Lines, Ultraviolet Spectra

Scientific paper

We have calculated a grid of detailed photoionization models for the stellar winds in non-magnetic cataclysmic variables. In the light of evidence which questions the existence of a classical hot, luminous boundary layer we investigate (i) models with cool, luminous boundary layers or (ii) models with no boundary layer at all, but with a moderately enhanced accretion rate in the disc. The ionization state predicted by these models is compared with that deduced from observations of the UV resonance lines in low-inclination nova-like variables. We find that the observed strength of the C IV and N v lines can be matched by models with luminous, cool boundary layers or with disc-only models where the accretion rate is 2 - 4 x 10 exp -8 solar mass/yr. The softer radiation field means that the required wind mass loss rates are only about 6 x 10 exp -10 solar mass/yr, i.e. only a few per cent of the accretion rate, in which case radiation pressure would be a viable mechanism for driving these winds.

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