Radiative viscosity and its stabilization of the thermal instability in accretion disks

Details Radiative viscosity and its stabilization of the thermal instability in accretion disks Radiative viscosity and its stabilization of the thermal instability in accretion disks

Jun 1981

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1981pazh....7..352l&link_type=abstract

(Pis'ma v Astronomicheskii Zhurnal, vol. 7, June 1981, p. 352-357.) Soviet Astronomy Letters, vol. 7, May-June 1981, p. 194-197.

Astronomy and Astrophysics

Astronomy

Black Holes (Astronomy), Gas Viscosity, Neutron Stars, Stellar Mass Accretion, Stellar Radiation, Thermal Instability, Dynamic Stability, Radiation Pressure, Turbulent Diffusion

Scientific paper

The radiative viscosity in the accretion disk around a black hole or neutron star is shown to exceed the viscosity of the fully ionized gas. The Reynolds number will reach a minimum in the zone where the bulk of the energy is released, and thermal stability will set in, altering the local accretion rate, temporarily suppressing the turbulence, and producing a distinctive variability in the radiation emitted by the disk. Differential rotation is shown to counteract thermal and dynamical instability in the outer part of the accretion disk and around a supermassive black hole.

Affiliated with

Also associated with

No associations

Rating

Radiative viscosity and its stabilization of the thermal instability in accretion disks 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 Radiative viscosity and its stabilization of the thermal instability in accretion disks, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Radiative viscosity and its stabilization of the thermal instability in accretion disks will most certainly appreciate the feedback.

Rate now

Comments { 0 }

Profile ID: LFWR-SCP-O-995215