Other
Scientific paper
Nov 1975
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1975mnras.173..357o&link_type=abstract
Monthly Notices of the Royal Astronomical Society, vol. 173, Nov. 1975, p. 357-379.
Other
40
Braking, Magnetic Effects, Magnetic Field Configurations, Stellar Magnetic Fields, Stellar Winds, Boundary Conditions, Boundary Value Problems, Crab Nebula, Equations Of Motion, Pulsars
Scientific paper
The exact equation which determines the steady, axisymmetric structure of the poloidal magnetic field in the stellar wind problem is derived from the transfield component of the equation of motion in the case of an isothermal corona. It has a critical point at the Alfvenic point and the critical condition there yields the boundary condition for the solution inside the Alfvenic point. Thus the result obtained by Weber & Davis for their assumed radial field can be generalized as follows: conditions downstream from the Alfvenic point influence neither the flow structure nor the field structure upstream. Then the field structure that deviates least from the equilibrium in the transfield direction is selected inside the Alfvenic point from a variety of the poloidal fields assumed for the three non-dimensional parameters measuring the coronal temperature, the field strength and the centrifugal force, respectively, at the coronal base.
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