Disk models with convective viscosity

Details Disk models with convective viscosity Disk models with convective viscosity

Jul 1981

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1981apj...247..499v&link_type=abstract

Astrophysical Journal, Part 1, vol. 247, July 15, 1981, p. 499-502.

Mathematics

Logic

3

Astronomical Models, Convection, Galactic Nuclei, Galactic Structure, Luminosity, Quasars, Radiation Pressure, Stellar Mass Accretion, Viscosity

Scientific paper

Disk models are presented which show that for a central mass of 1-million solar masses the disks have a central convective zone that causes the accretion of matter by the central star. Disk luminosities are too low to explain the energy output of quasars if at a cosmological distance, but are adequate if at a noncosmological distance. Calculations of the vertical structure include viscosity produced by convection, and nuclear burning is negligible. A disk model for a central mass of 10-million solar masses is also calculated, and although it converges, the model is supported by radiation pressure and presents a density inversion at the center.

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