Flares, Magnetic Reconnections and Accretion Disk Viscosity

Details Flares, Magnetic Reconnections and Accretion Disk Viscosity Flares, Magnetic Reconnections and Accretion Disk Viscosity

Jul 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001hst..prop.9078w&link_type=abstract

HST Proposal ID #9078

Astronomy and Astrophysics

Astrophysics

Hst Proposal Id #9078 Hot Stars

Scientific paper

Accretion disks are invoked to explain a host of astrophysical phenomena, from protostellar objects to AGN. And yet the mechanism allowing accretion disks to operate are completely unknown. This proposal seeks to observe the ``smoking gun'' signature of magnetically-driven viscosity in accretion disks. Magnetically-induced viscosity is a plausible and generally accepted hypothesis {for esthetic reasons}, but it is completely untested. Determining the cause of accretion disk viscosity is of major significance to all accretion-disk powered systems {e.g. CVs, X-ray binaries, AGN and protostellar disks}. These data will also firmly establish the importance of magnetic fields in accretion disks. Because of its known flaring properites, we will observe the accretion disk in EM Cyg simulataneously with STIS/FUV and CHANDRA. The simultaneous X-rays are absolutely necessary for the unambiguous detection of accretion disk magnetic reconnection flares.

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