Hot accretion disks with pairs: Effects of magnetic field and thermal cyclocsynchrotron radiation

Details Hot accretion disks with pairs: Effects of magnetic field and thermal cyclocsynchrotron radiation Hot accretion disks with pairs: Effects of magnetic field and thermal cyclocsynchrotron radiation

Feb 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994apj...422..737k&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 422, no. 2, p. 737-745

Astronomy and Astrophysics

Astronomy

8

Accretion Disks, Astronomical Models, Cyclotron Radiation, Magnetic Fields, Mathematical Models, Thermal Radiation, Viscosity, Active Galactic Nuclei, Black Holes (Astronomy), Bremsstrahlung, X Ray Spectra

Scientific paper

We show the effects of thermal cyclosynchrotron radiation and magnetic viscosity on the structure of hot, two-temperature accretion disks. Magnetic field, B, is assumed to be randomly oriented and the ratio of magnetic pressure to either gas pressure, alpha = Pmag/Pgas, or the sum of the gas and radiation pressures, alpha = (Pmag/Pgas + Prad), is fixed. We find those effects do not change the qualitative properties of the disks, i.e., there are still two critical accretion rates related to production of e+/- pairs, (M dot)(Ucr) and (M dot)(Lcr), that affect the number of local and global disk solutions, as recently found by Bjoernsson and Svensson for the case with B = 0. However, a critical value of the alpha-viscosity parameter above which those critical accretion rates disappear becomes smaller than alphacr = 1 found in the case of B = 0, for Pmag = alpha(Pgas + Prad). If Pmag = alpha Pgas, on the other hand, alphacr is still about unity. Moreover, when Comptonized cyclosynchrotron radiation dominates Comptonized bremsstrahlung, radiation from the disk obeys a power law with the energy spectral index of approximately 0.5, in a qualitative agreement with X-ray observations of active galactic nuclei (AGNS) and Galactic black hole candidates. We also extend the hot disk solutions for Pmag = alpha(Pgas + Prad) to the effectively optically thick region, where they merge with the standard cold disk solutions. We find that the mapping method by Bjoernsson and Svensson gives a good approximation to the disk structure in the hot region and show where it breaks in the transition region. Finally, we find a region in the disk parameter space with no solutions due to the inability of Coulomb heating to supply enough energy to electrons.

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