RELATIVISTIC, HOT STELLAR WINDS WITH ANISOTROPIC PRESSURE

The structure of hot, strongly magnetized, relativistic stellar winds with anisotropic pressure is investigated. In particular, a pulsar win d is considered, where, due to radiative losses, P-parallel to >> P-pe rpendicular to . The fluid velocity is relativistic, while the tempera ture of the medium is ultrarelativistic. The basic system of equations is written and analyzed for a two-dimensional wind structure. This pa per can be recognized as an astrophysical application of the results o btained in Tsikarishvili et al. (1992), where new equations of state w ere derived for an anisotropic medium with ultrarelativistic temperatu re. The solution is performed for the wind region beyond the light cyl inder where the temperature is assumed to be ultrarelativistic.