Abstract
HST UV observations of V795 Her reveal a strong 2.6-h orbital variation in the prominent UV lines, in contrast to earlier (IUE) evidence of a 4.8-h period. Only the C iv line contains a strong blue-shifted, wind formed absorption component. Several lines exhibit a ‘narrow’ absorption feature near rest velocity which may originate in the disk, and a blue-shifted emission feature which accounts for most of the line profile variability.
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© 1996 Kluwer Academic Publishers
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Rosen, S.R., Prinja, R.K., Drew, J.E., Mason, K.O., Howell, S.B. (1996). HST UV Observations of the Disk and Wind of V795 Her. In: Evans, A., Wood, J.H. (eds) Cataclysmic Variables and Related Objects. Astrophysics and Space Science Library, vol 208. Springer, Dordrecht. https://doi.org/10.1007/978-94-009-0325-8_13
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DOI: https://doi.org/10.1007/978-94-009-0325-8_13
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