Abstract
A structure of hot, strongly magnetized, relativistic stellar winds with anisotropic pressure is investigated. In particular, a pulsar wind is considered, where, due to radiative losses, P<SUB>parallel</SUB> is much greater than P. The fluid velocity is relativistic, while the temperature of the medium is ultrarelativistic. The basic system of equations is written and analyzed for a two-dimensional wind structure. This paper can be recognized as an astrophysical application of the results obtained in Tsikarishvili et al. (1992), where new equations of state were derived for an anisotropic medium with ultrarelativistic temperature. The solution is performed for the wind region beyond the light cylinder where the temperature is assumed to be ultrarelativistic.
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