Buoyancy-limited magnetic viscosity in quasi-stellar object accretion disk models

Details Buoyancy-limited magnetic viscosity in quasi-stellar object accretion disk models Buoyancy-limited magnetic viscosity in quasi-stellar object accretion disk models

Jul 1989

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989apj...342...49s&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 342, July 1, 1989, p. 49-63.

Statistics

Computation

45

Accretion Disks, Astronomical Models, Computational Astrophysics, Quasars, Active Galactic Nuclei, Buoyancy, Field Strength, Magnetic Fields, Radiation Pressure, Turbulence Effects

Scientific paper

Alpha models of astrophysical accretion disks assume an ad hoc viscous stress which scales locally as the total pressure. It is shown here that, if turbulent magnetic Maxwell stresses are the source of this viscosity in quasi-stellar object accretion disk models, then the stress cannot follow the assumed alpha-law in the radiation pressure-dominated inner region of the disk.

Affiliated with

Also associated with

No associations

Rating

Buoyancy-limited magnetic viscosity in quasi-stellar object accretion disk models 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 Buoyancy-limited magnetic viscosity in quasi-stellar object accretion disk models, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Buoyancy-limited magnetic viscosity in quasi-stellar object accretion disk models will most certainly appreciate the feedback.

Rate now

Comments { 0 }

Profile ID: LFWR-SCP-O-1703587