Particle Acceleration and the Formation of Relativistic Outflows in Viscous Disks with Shocks

Details Particle Acceleration and the Formation of Relativistic Outflows in Viscous Disks with Shocks Particle Acceleration and the Formation of Relativistic Outflows in Viscous Disks with Shocks

Jan 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010aas...21540411b&link_type=abstract

American Astronomical Society, AAS Meeting #215, #404.11; Bulletin of the American Astronomical Society, Vol. 42, p.226

Astronomy and Astrophysics

Astronomy

Scientific paper

We investigate the Green's function energy/space distribution of the relativistic particles accelerated in viscous, advection-dominated accretion disks containing standing, centrifugally-supported shock waves. The dynamical structure of the accreting gas is described using a new model for viscous, shocked disks recently reported by the authors, and a rigorous mathematical method is employed to solve the transport equation for the relativistic particle distribution. We find that the concentrated particle acceleration occurring in the vicinity of the standing shock can channel a significant fraction of the gravitational potential energy of the accretion flow into a population of relativistic particles that diffuse vertically out of the disk, carrying away both energy and entropy and allowing the remaining gas to accrete. The distribution of the escaping particles displays a relatively flat power-law shape at high energies. We demonstrate that our formalism can explain the bulk properties of the jet outflows observed in M87 and the Galactic center.

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