Relativistic Stellar-Wind Torques

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Abstract
Several authors have calculated the torque on the Sun owing to the solar wind. We extend those treat- ments to encompass both special- and geneial-relativistic effects. A direct parallel treatment is feasible, and the major correction is, as would be expected, from the increased effective mass density of a rela- tivistic fluid. The treatment may be extended approximately to the limit of zero mass loss, wherein the toi que is entirely from the electromagnetic energy radiated by the rotating magnetic moment of the star. Application to rotational models of pulsars is illustrated with the conclusion that NP 0532, for ex- ample, would have a magiietic moment of order 3 X 1tY~ gauss cm3 (within certain assumptions regard- ing the rate of mass loss). Centrifugal forces are capable of accelerating the plasma to ultrarelativistic velocities, even in the magnetohydrodynamic approximation. The existence of pulsars therefore suggests a new and highly efficient source of relativistic particles

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