The structure and parameters of flare streams in relation to the location of the flare and to the configuration of the large-scale magnetic field on the sun are considered. The following results are obtained: (1) The flare streams spread in a rather wide angle (&lgr;m?¿60¿). (2) The velocity of the streams ejected by the flares in the sun's western hemisphere is 1.5 time higher than that of the streams ejected by eastern flares. (3) The sign of Bz being fixed, the sign of Bx within the stream is determined by the location of the flare with respect to the solar equator. (4) The exponent of the polytrope for the solar wind the stream is determined by the location of the flare with respect to the solar equator. (4) The exponent of the polytrope for the solar wind plasma (&ggr;=1.4--1.7) is close to or less than the adiabatic one.