Relativistic particle transport in hot accretion disks

Details Relativistic particle transport in hot accretion disks Relativistic particle transport in hot accretion disks

Feb 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994apjs...90..949b&link_type=abstract

Astrophysical Journal Supplement Series (ISSN 0067-0049), vol. 90, no. 2, p. 949-953

Astronomy and Astrophysics

Astronomy

7

Accretion Disks, Active Galactic Nuclei, Astronomical Models, Particle Acceleration, Relativistic Particles, Transport Theory, Black Holes (Astronomy), Energy Dissipation, Gamma Ray Bursts, High Energy Interactions, Protons, Quasars, Rotational Spectra, Stochastic Processes

Scientific paper

Accretion disks around rapidly rotating black holes provide one of the few plausible models for the production of intense radiation in Acitve Galactic Nuclei (AGNs) above energies of several hundred MeV. The rapid rotation of the hole increases the binding energy per nucleon in the last stable orbit relative to the Schwarzschild case, and naturally leads to ion temperatures in the range 1012 - 1013 K for sub-Eddington accretion rates. The protons in the hot inner region of a steady, two-temperature disk form a reservoir of energy that is sufficient to power the observed Energetic Gamma Ray Experiment Telescope (EGRET) outbursts if the black hole mass is 1010 solar mass. Moreover, the accretion timescale for the inner region is comparable to the observed transient timescale of approximately 1 week. Hence EGRET outbursts may be driven by instabilities in hot, two-temperature disks around supermassive black holes. In this paper we discuss turbulent (stochastic) acceleration in hot disks as a possible source of GeV particles and radiation. We constrain the model by assuming the turbulence is powered by a collective instability that drains energy from the hot protons. We also provide some ideas concerning new, high-energy Penrose processes that produce GeV emission be directly tapping the rotational energy of Kerr black holes.

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