Astronomy and Astrophysics – Astrophysics
Scientific paper
Dec 1998
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998tx19.confe.336f&link_type=abstract
Abstracts of the 19th Texas Symposium on Relativistic Astrophysics and Cosmology, held in Paris, France, Dec. 14-18, 1998. Eds.:
Astronomy and Astrophysics
Astrophysics
Scientific paper
The structure of the SS433 supercritical accretion disk derived from spectral and photometrical data is described. There are two regions of a hot gas emission (``HeII cocoons'') situated in the central parts of the disk around the both relativistic jet bases. They produce the broad double-peaked profiles, which are completely eclipsed by the optical star, but the receding HeII cocoon is not shadowed by the disk. The X-ray emitting jet bases are situated inside these cocoons. Absorption line radial velocities are found to be strongly dependent on the precessional phase, this allows for a study of structure of the gas outflow. In the disk plane gas outflows at a velocity of about 100 - 150 km/s, while above the disk plane the velocity increases sharply and reaches ~1500 km/s at a polar angle ~60^circ. The outer parts of the accretion disk are involved in the precession motion, which means that the slaved disk precession model is correct.
No associations
LandOfFree
The Supercritical Accretion Disk of SS433 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 Supercritical Accretion Disk of SS433, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and The Supercritical Accretion Disk of SS433 will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-768491