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The accreting white dwarfs in BW Scl, BC UMa and SW UMa | | B.T. Gaensicke
; P. Szkody
; S.B. Howell
; E.M. Sion
; | | Date: |
18 Apr 2005 | | Journal: | Astrophys.J. 629 (2005) 451-460 | | Subject: | astro-ph | | Abstract: | We have observed the short-period dwarf novae BW Scl, BC UMa and SW UMa using the Hubble Space Telescope/Space Telescope Imaging Spectrograph. In all three systems, the white dwarf is the dominant source of far-ultraviolet flux, even though in BC UMa and SW UMa an additional continuum component contributes ~10% and ~20% of the 1400A flux, respectively. Fitting the data with detailed white dwarf model spectra, we determine the effective temperatures to be 14800+-900K (BW Scl), 15200+-1000K (BC UMa), and 13900+-900K (SW UMa). The additional continuum component in BC UMa and SW UMa is equally well described by either a blackbody or a power law, which could be associated with emission from the hot spot or from an optically thin accretion disk (or an optically thin layer on top of a colder optically thick disk), respectively. Modelling the narrow metal lines detected in the STIS spectra results in sub-solar abundances of carbon, oxygen and silicon for all three systems, and also suggests substantial supra-solar abundances of aluminium. The narrow absorption line profiles imply low white dwarf rotation rates, v sin(i)<=300km/s for the three white dwarfs. SW UMa is the only system that shows significant short-term variability in the far-ultraviolet range, which is primarily associated with the observed emission lines. | | Source: | arXiv, astro-ph/0504382 | | Services: | Forum | Review | PDF | Favorites | |
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