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dc.contributor.authorHoare, M.G.
dc.contributor.authorDrew, J.E.
dc.identifier.citationHoare , 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.otherPURE: 157238
dc.identifier.otherPURE UUID: 7179052b-242a-49ab-8daf-52063ec7c68d
dc.identifier.otherdspace: 2299/4043
dc.descriptionOriginal article can be found at: Copyright Royal Astronomical Society [Full text of this article is not available in the UHRA]
dc.description.abstractWe 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.relation.ispartofMonthly Notices of the Royal Astronomical Society
dc.subjectaccretion disks
dc.subjectradiative transfer
dc.titleThe ionization state of the winds from cataclysmic variables without classical boundary layersen
dc.contributor.institutionSchool of Physics, Astronomy and Mathematics
dc.description.statusPeer reviewed
dc.relation.schoolSchool of Physics, Astronomy and Mathematics
rioxxterms.typeJournal Article/Review

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