Instabilities and time evolution of hot accretion disks with electron-positron pairs

Details Instabilities and time evolution of hot accretion disks with electron-positron pairs Instabilities and time evolution of hot accretion disks with electron-positron pairs

Apr 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990apj...352..495w&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 352, April 1, 1990, p. 495-505.

Physics

19

Accretion Disks, Electron-Positron Pairs, Galactic Nuclei, Galactic Radiation, Optical Thickness, X Ray Sources, Compton Effect, Digital Simulation, Electron Energy, Elementary Particles

Scientific paper

The evolution and stability of pair-supercritical accretion disks are examined. The microphysics of electron-positron pair processes are incorporated into a self-consistent accretion disk model, using the full set of time-dependent equations for a two-temperature disk cooled by bremsstrahlung protons with Comptonization included. It is found that the high pair density branch of pair subcritical disks is unstable to perturbations of the pair density. It is shown that optically thin, pair supercritical disks, i.e., hot disks radiating at above a few percent of the Eddington limit, have no steady state and unavoidably collapse down to a cool, optically thick state.

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