Astronomy and Astrophysics – Astrophysics
Scientific paper
Apr 2007
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007aps..aprj10003q&link_type=abstract
American Physical Society, APS April Meeting, April 14-17, 2007, abstract #J10.003
Astronomy and Astrophysics
Astrophysics
Scientific paper
Accretion of plasma onto a central object is responsible for many of the most energetic phenomena observed in astrophysics; stars, planets, and galaxies are also formed via such accretion disks. I summarize the physics of angular momentum and energy transport in astrophysical disks. A linear instability of differentially rotating plasmas -- the magnetorotational instability (MRI) -- amplifies magnetic fields and gives rise to MHD turbulence in accretion disks. Magnetic stresses due to MHD turbulence transport angular momentum, allowing plasma to accrete. In addition, the gravitational potential energy of the inflowing plasma is converted into heat via the action of MHD turbulence -- powering the radiation we see from accretion flows. I highlight recent work on the physics of a particular class of accretion flows onto black holes and neutron stars, in which the inflowing plasma is macroscopically collisionless and kinetic effects are crucial for the angular momentum and energy evolution of the accretion flow.
No associations
LandOfFree
Angular Momentum Transport in Astrophysical Accretion Flows does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.
If you have personal experience with Angular Momentum Transport in Astrophysical Accretion Flows, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Angular Momentum Transport in Astrophysical Accretion Flows will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-1684155