Hostname: page-component-586b7cd67f-gb8f7 Total loading time: 0 Render date: 2024-11-25T16:37:10.495Z Has data issue: false hasContentIssue false
  • English
  • Français

HST UV Observations of the Disk and Wind of V795 Her

Published online by Cambridge University Press:  12 April 2016

S. R. Rosen ,
R. K. Prinja ,
J. E. Drew ,
K. O. Mason  and
S. B. Howell
S. R. Rosen
Affiliation:
Leicester University, Leicester, LE1 7RH, UK
R. K. Prinja
Affiliation:
University College London, London, WC1E 6BT, UK
J. E. Drew
Affiliation:
Imperial College London, London, SW7 2BZ, UK
K. O. Mason
Affiliation:
MSSL, Holmbury St. Mary, RH5 6NT, UK
S. B. Howell
Affiliation:
Planetary Sciences Institute, Tuscon, AZ, USA

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

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.

Type
Non-Magnetic Cataclysmic Variables
Information
International Astronomical Union Colloquium , Volume 158: Cataclysmic Variables and Related Objects , 1996 , pp. 43 - 44
Copyright
Copyright © Kluwer 1996

References

1. Prinja, R.K., Rosen, S.R., Suppelli, K., 1991, MNRAS, 248, 40 Google Scholar
2. Prinja, R.K., Drew, J.E., Rosen, S.R., 1992, MNRAS, 256, 219 Google Scholar
3. Prinja, R.K., Rosen, S.R., 1993, MNRAS, 262, 37pGoogle Scholar
4. Shatter, A.W., 1990, Ap. J., 354, 708 Google Scholar