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Event Detail Information

Event Detail Information

SpeakerYan-Fei Jiang (Harvard University)
Date Oct 9, 2013
Time 12:00 pm  
Location 464 Loomis
Sponsor Department of Physics
Phone 3124045023
Event type Seminar
Views 3215

Structures and thermal properties of the black hole

accretion disks in the radiation pressure dominated regime will be

discussed. Angular

momentum transfer in the disk is provided by the turbulence generated by

the magneto-rotational instability (MRI), which is calculated


with a recently developed 3D radiation

magneto-hydrodynamics (MHD) code based on Athena.

The thermal instability of the radiation pressure

dominated disks is studied with vertically stratified shearing box

simulations. I always find that the radiation

pressure dominated disks either collapse or expand until we have to stop

the simulations. During the thermal runaway, the heating and cooling

rates from the simulations are consistent with the general criterion of

thermal instability. However, details of the thermal runaway are

different from the predictions of the standard alpha disk model. We also

identify the key reasons why previous simulations do not find the

instability. A new mechanism to generate high temperature corona above the

accretion disk is also found from these simulations.

The thermal instability has many important implications for

understanding the observations of both X-ray binaries and Active

Galactic Nuclei.

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