Analysis of a magnetohydrodynamic stellar wind

Details Analysis of a magnetohydrodynamic stellar wind Analysis of a magnetohydrodynamic stellar wind

Feb 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986ap%26ss.119...33s&link_type=abstract

(IAU, Asian-Pacific Regional Meeting, 3rd, Kyoto, Japan, Sept. 30-Oct. 5, 1984) Astrophysics and Space Science (ISSN 0004-640X),

Statistics

Computation

Computational Astrophysics, Magnetohydrodynamic Waves, Stellar Winds, Curves (Geometry)

Scientific paper

Weber and Davis (1967) expressed the radial motion of a steady stellar wind by a nonlinear, ordinary differential equation of first order and first degree; the topology of the solutions exhibits two critical points, reflecting the slow and fast modes of magnetoacoustic waves, and one node, the Alfvenic point. Solutions around this point are presently analyzed by functional series expansions, using the method of undetermined coefficients. Three types of curves pass through the point. The leading term of the solution concerns gas pressure, gravitational energy, and magnetic energy.

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