Numerical Simulations of MHD Turbulence in Accretion Disks

Details Numerical Simulations of MHD Turbulence in Accretion Disks Numerical Simulations of MHD Turbulence in Accretion Disks

Apr 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009aspc..406....9f&link_type=abstract

Numerical Modeling of Space Plasma Flows: ASTRONUM-2008 ASP Conference Series, Vol. 406, proceedings of the conference held 8-13

Astronomy and Astrophysics

Astronomy

Scientific paper

The magnetorotational instability (MRI) is the most likely source of MHD turbulence in accretion disks. Recently, it has been realized that microscopic diffusion coefficients (viscosity and resistivity) are important in determining the saturated state of the turbulence and thereby the rate of angular momentum transport within the disc. In this paper, we present a set of numerical simulations of MRI--induced MHD turbulence in which we investigate the dependence of α, the rate of angular momentum transport, on these coefficients. We present various methods used to control the relative amount of physical versus numerical dissipation in such calculations. The results of the simulations show that α is an increasing function of the magnetic Prandtl number Pm, the ratio of viscosity over resistivity. In the absence of a mean field, we also find that MRI--induced MHD turbulence decays at low Pm.

Affiliated with

Also associated with

No associations

Rating

Numerical Simulations of MHD Turbulence in Accretion Disks 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 Numerical Simulations of MHD Turbulence in Accretion Disks, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Numerical Simulations of MHD Turbulence in Accretion Disks will most certainly appreciate the feedback.

Rate now

Comments { 0 }

Profile ID: LFWR-SCP-O-1238352