Wave-driven winds from cool stars. I - Some effects of magnetic field geometry

Details Wave-driven winds from cool stars. I - Some effects of magnetic field geometry Wave-driven winds from cool stars. I - Some effects of magnetic field geometry

Jun 1982

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982apj...257..264h&link_type=abstract

Astrophysical Journal, Part 1, vol. 257, June 1, 1982, p. 264-268.

Other

36

Cool Stars, Late Stars, Stellar Magnetic Fields, Stellar Winds, Magnetohydrodynamic Waves, Stellar Mass Ejection, Stellar Models, Velocity Distribution

Scientific paper

The wave-driven wind theory of Hartmann and MacGregor (1980) is extended to include effects due to non-radial divergence of the flow. Specifically, isothermal expansion within a flow tube whose cross-sectional area increases outward faster than the square of the radius near the stellar surface is considered. It is found that the qualitative conclusions of Hartmann and MacGregor concerning the physical properties of Alfven wave-driven winds are largely unaffected. In particular, mass fluxes of similar magnitude are obtained, and wave dissipation is still necessary to produce acceptably small terminal velocities. Increasingly divergent flow geometries generally lead to higher initial wind speeds and slightly lower terminal velocities. For some cases of extremely rapid flow tube divergence, steady supersonic wind solutions which extend to infinity with vanishing gas pressure cannot be obtained. In addition, departures from spherical symmetry can cause the relative Alfven wave amplitude delta-B/B to become approximately greater than 1 within several stellar radii of the base of the wind, suggesting that nonlinear processes may contribute to the wave dissipation required by the theory.

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