"Radiation-driven winds from stars and Active Galactic Nucle"
A. V. Dorodnitsyn (IKI)
Abstract:
It
is now clearly understood that the problem of mass loss is crucially
important both from the point of view of it’s influence on the evolution
of stars and for the explanation of physical processes and
observational data in active galactic nuclei (AGN). Evolution of massive
stars is accompanied by mass loss as strong as 10-4 -10-6
M_sun/yr. Absorption of the radiation by continuum opacity is
responsible for such an evolutionary significant mass loss in cold massive
stars. Massive hot stars may have winds as fast as v_{inf}=2000 km/s that
is three orders of magnitude faster then that of the massive evolved stars.
The momentum is transferred from the radiation to outflowing plasma due to
absorption in different line transitions. This mechanism of radiation
acceleration is probably responsible for the acceleration of winds from
accretion discs in AGN as well. It was recently recognized (Dorodnitsyn A.,
2003) that if the wind is accelerated from the vicinity of the black hole,
Sobolev
mechanism should be revisited considerably in order to take into account
influence of the strong gravitational field on the radiation.
Detailed analytical and numerical analysis had revealed a significant
difference between a wind form AGN that is predicted by a standard
line-driven wind theory and a developed approach.