General Relativistic Hydrodynamics with Viscosity

Details General Relativistic Hydrodynamics with Viscosity General Relativistic Hydrodynamics with Viscosity

Apr 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005aps..aprm10002d&link_type=abstract

American Physical Society, APS April Meeting, April 16-19, 2005, abstract #M10.002

Astronomy and Astrophysics

Astrophysics

Scientific paper

Viscosity and magnetic fields drive differentially rotating stars toward uniform rotation, and this process has important consequences in many astrophysical contexts. Here, we present the first numerical evolutions of rapidly rotating stars with shear viscosity in full general relativity. We self-consistently include viscosity in our relativistic hydrodynamic code by solving the fully relativistic Navier-Stokes equations in a BSSN formulation. We demonstrate the ability of our code to accurately follow both the secular viscous evolution of differentially rotating stars for many rotation periods, as well as dynamical evolution. We also investigate the ability of viscosity to drive bar or disk formation.

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