The geometry and ionization structure of the wind in the eclipsing nova-like variables RW Tri and UX UMa

U.M. Noebauer, K.S. Long, S.A. Sim, C. Knigge

Research output: Contribution to journalArticle

21 Citations (Scopus)

Abstract

The UV spectra of nova-like variables are dominated by emission from the accretion disk, modified by scattering in a wind emanating from the disk. Here, we model the spectra of RW Tri and UX UMa, the only two eclipsing nova-like variables which have been observed with the Hubble Space Telescope in the far-ultraviolet, in an attempt to constrain the geometry and the ionization structure of their winds. Using our Monte Carlo radiative transfer code, we computed spectra for simply parameterized axisymmetric biconical outflow models and were able to find plausible models for both systems. These reproduce the primary UV resonance lines-N v, Si iv, and C iv-in the observed spectra in and out of eclipse. The distribution of these ions in the wind models is similar in both cases as is the extent of the primary scattering regions in which these lines are formed. The inferred mass-loss rates are 6%-8% of the mass accretion rates for the systems. We discuss the implication of our point models for our understanding of accretion disk winds in cataclysmic variables.
Original languageEnglish
Pages (from-to)1932-1945
Number of pages14
JournalAstrophysical Journal
Volume719
Issue number2
DOIs
Publication statusPublished - 20 Aug 2010

Bibliographical note

Copyright 2011 Elsevier B.V., All rights reserved.

Fingerprint Dive into the research topics of 'The geometry and ionization structure of the wind in the eclipsing nova-like variables RW Tri and UX UMa'. Together they form a unique fingerprint.

  • Cite this