Observations of the sw sextantis star uu aquarii
Nov, 199723 pages
Published in:
- Mon.Not.Roy.Astron.Soc. 294 (1998) 689
e-Print:
- astro-ph/9711230 [astro-ph]
DOI:
- 10.1046/j.1365-8711.1998.01321.x,
- 10.1111/j.1365-8711.1998.01321.x (publication)
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Abstract: (arXiv)
We present 14 nights of medium resolution (1-2\AA) spectroscopy of the eclipsing cataclysmic variable UU Aquarii obtained during a high accretion state in 1995 August-October. UU Aqr appears to be an SW Sextantis star, as noted by Baptista, Steiner, & Horne (1996), and we discuss its spectroscopic behavior in the context of the SW Sex phenomenon. Emission line equivalent width curves, Doppler tomography, and line profile simulation provide evidence for the presence of a bright spot at the impact site of the accretion stream with the edge of the disk, and a non-axisymmetric, vertically- and azimuthally-extended absorbing structure in the disk. The absorption has maximum depth in the emission lines around orbital phase 0.8, but is present from to . An origin is explored for this absorbing structure (as well as the other spectroscopic behavior of UU Aqr) in terms of the explosive impact of the accretion stream with the disk.Note:
- 23 pages (with 3 tables); 12 postscript figures (figs. 6-9,11 are low resolution versions); accepted for publication in MNRAS; a single postscript file containing the text and figures (including high resolution versions of figs. 6-9,11) is available at http://www.astro.washington.edu/hoard/vitae/vitae.html#MNRAS97
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