Stationary and axisymmetric magnetized equilibria of stars and winds

Details Stationary and axisymmetric magnetized equilibria of stars and winds Stationary and axisymmetric magnetized equilibria of stars and winds

Jun 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011iaus..274..437y&link_type=abstract

Advances in Plasma Astrophysics, Proceedings of the International Astronomical Union, IAU Symposium, Volume 274, p. 437-440

Astronomy and Astrophysics

Astrophysics

Stars: Magnetic Fields, Stars: Rotation, Stars: Winds, Outflows

Scientific paper

We present a new formulation to compute numerically stationary and axisymmetric equilibria of magnetized and self-gravitating astrophysical fluids. Under the assumption of ideal MHD, the stream function for the flow can be chosen as a basic variable with which the Euler-Maxwell equations are cast into a set of basic equations, i.e. a generalized Bernoulli equation and a Grad-Shafranov-like equation by employing various integral conditions. A novel feature of this formulation is that systems with stars, disks and winds are treated in a simple unified picture and the magnetic field structures can contain both poloidal and toroidal components.

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