dc.contributor.author | Hoare, M.G. | |
dc.contributor.author | Drew, J.E. | |
dc.date.accessioned | 2009-12-01T14:16:29Z | |
dc.date.available | 2009-12-01T14:16:29Z | |
dc.date.issued | 1993 | |
dc.identifier.citation | Hoare , M G & Drew , J E 1993 , ' The ionization state of the winds from cataclysmic variables without classical boundary layers ' , Monthly Notices of the Royal Astronomical Society , vol. 260 , no. 3 , pp. 647-662 . | |
dc.identifier.issn | 0035-8711 | |
dc.identifier.other | dspace: 2299/4043 | |
dc.identifier.uri | http://hdl.handle.net/2299/4043 | |
dc.description | Original article can be found at: http://adsabs.harvard.edu/basic_search.html Copyright Royal Astronomical Society [Full text of this article is not available in the UHRA] | |
dc.description.abstract | 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. | en |
dc.language.iso | eng | |
dc.relation.ispartof | Monthly Notices of the Royal Astronomical Society | |
dc.subject | accretion disks | |
dc.subject | radiative transfer | |
dc.title | The ionization state of the winds from cataclysmic variables without classical boundary layers | en |
dc.contributor.institution | School of Physics, Astronomy and Mathematics | |
dc.description.status | Peer reviewed | |
rioxxterms.type | Journal Article/Review | |
herts.preservation.rarelyaccessed | true | |