Magnetic viscosity in weakly ionized protostellar discs

Details Magnetic viscosity in weakly ionized protostellar discs Magnetic viscosity in weakly ionized protostellar discs

Mar 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997mnras.286...97r&link_type=abstract

Monthly Notices of the Royal Astronomical Society, Volume 286, Issue 1, pp. 97-103.

Astronomy and Astrophysics

Astronomy

6

Accretion, Accretion Discs, Instabilities, Magnetic Fields, Stars: Formation

Scientific paper

It has been shown that a self-consistent magnetic dynamo can operate in a fully ionized accretion disc and so provide an effective (magnetic) viscosity. Parker's instability (magnetic buoyancy) in weakly ionized protostellar discs is considered. Combined with the Balbus-Hawley instability in a similar medium, magnetic reconnection and the dynamo model are generalized for weakly ionized discs. The increased rate of reconnection and the decreased growth rate of the Balbus-Hawley instability from increased azimuthal fields have opposite effects. It is found that the Shakura-Sunyaev viscosity parameter does not change for very weakly ionized protostellar accretion discs (alpha_SS~0.4).

Affiliated with

Also associated with

No associations

Rating

Magnetic viscosity in weakly ionized protostellar discs 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 Magnetic viscosity in weakly ionized protostellar discs, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Magnetic viscosity in weakly ionized protostellar discs will most certainly appreciate the feedback.

Rate now

Comments { 0 }

Profile ID: LFWR-SCP-O-874812