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dc.contributor.authorDrew, J.E.
dc.contributor.authorProga, D.
dc.date.accessioned2009-04-24T14:35:45Z
dc.date.available2009-04-24T14:35:45Z
dc.date.issued2000
dc.identifier.citationDrew , J E & Proga , D 2000 , ' Radiation-driven accretion disk winds ' , New Astronomy Reviews , vol. 44 , no. 1-2 , pp. 21-26 . https://doi.org/10.1016/S1387-6473(00)00007-5
dc.identifier.issn1387-6473
dc.identifier.otherPURE: 179405
dc.identifier.otherPURE UUID: f1058d7a-0bdf-4913-9659-100f90fa1e25
dc.identifier.otherdspace: 2299/3298
dc.identifier.otherScopus: 0034165232
dc.identifier.urihttp://hdl.handle.net/2299/3298
dc.descriptionOriginal article can be found at: http://www.sciencedirect.com/science/journal/13876473 Copyright Elsevier B.V. [Full text of this record is not available in the UHRA]
dc.description.abstractThe concept of an ‘effective' Eddington limit as a lower bound on the system luminosity required for mass loss to be radiation pressure driven is discussed and shown to fall in the interesting regime for high-state non-magnetic CV (nMCV). The results of recent hydrodynamical models of radiation-driven disk winds (Proga et al. 1998, Proga 1999) are summarised. Mass loss rates predicted by these models are then compared with observational constraints. It is shown that either mass accretion rates in high-state nMCV are a factor of 2–3 larger than presently supposed or that radiation pressure alone is not quite sufficient to drive the observed hypersonic flows.en
dc.language.isoeng
dc.relation.ispartofNew Astronomy Reviews
dc.subjectcataclysmic variables
dc.titleRadiation-driven accretion disk windsen
dc.contributor.institutionSchool of Physics, Astronomy and Mathematics
dc.description.statusPeer reviewed
rioxxterms.versionofrecordhttps://doi.org/10.1016/S1387-6473(00)00007-5
rioxxterms.typeJournal Article/Review
herts.preservation.rarelyaccessedtrue


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