Astronomy and Astrophysics – Astronomy
Scientific paper
Apr 1994
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994a%26a...284..145v&link_type=abstract
Astronomy and Astrophysics (ISSN 0004-6361), vol. 284, no. 1, p. 145-155
Astronomy and Astrophysics
Astronomy
47
Novae, Stellar Mass Accretion, Stellar Models, Stellar Winds, Symbiotic Stars, Ultraviolet Astronomy, Ultraviolet Spectra, Iue, Red Giant Stars
Scientific paper
The nature of the hot radiation source in symbiotic systems is still controversial. In AG Peg, the hot component went into a thermonuclear outburst after a probably long phase of mass accretion from the cool giant companion. This outburst has been lasting for more than 150 years. During most of this phase the hot compact component has been losing mass through a stellar wind. We show that this wind can be traced in UV spectra, and we present a simple method for estimating the mass loss rate, which is of the order of 10-7 solar mass/yr at a velocity of approximately equal to 900 km/s. The strength of the wind has diminished by a factor of 5 during the last decade, and the outbursting star might soon reach its pre-outburst state. The cool giant companion also loses mass at a similar rate, leading to a collision region between the two stars. Evidence for such a collision zone could be obtained from X-ray observations or from radio images with high spatial emission resolution, showing directly the topology of the nebular emission region.
Nussbaumer Harry
Vogel Manfred
No associations
LandOfFree
The hot wind in the symbiotic nova AG Pegasi does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.
If you have personal experience with The hot wind in the symbiotic nova AG Pegasi, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and The hot wind in the symbiotic nova AG Pegasi will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-1254092