Аннотация:The results of observations of low-flying satellites crossing the daytime sector of the auroral zone and of high-apogee satellites in the equatorial plane of the magnetosphere were analyzed in order to identify the main processes leading to the formation of daytime polar cusps. Data from the DMSP F7 satellite were used to analyze the latitudinal characteristics of ion precipitation in the cusp region and to study the latitudinal profile of ion pressure in the cusp depending on the IMF parameters. A significant difference was found in identifying the cusp boundaries using an automated data processing system and direct analysis of satellite observations. It is shown that for small negative values of the Bz-component of the IMF (<Bz> = –3.0 nT), a characteristic feature of the cusp is the latitudinal profile of the ion pressure (Pi) with a width of ~1° of latitude with two maxima, one of which is located in the equatorial and the other in the polar part of the cusp. For large negative Bz values (–6, –8 nT), the polar maximum in the latitudinal profile Pi vanishes; only the equatorial maximum remains, the Pi level at the maximum increases, and the width of the cusp decreases to ~0.7°. For Bz IMF > 0, the most characteristic is the Pi profile with a maximum ion pressure in the polar part of the cusp. The cusp for Bz > 0 is located at higher latitudes than for Bz < 0, and its average latitudinal dimensions increase to ~1.4° of latitude. In the prenoon sector MLT, the most typical for periods with a large negative By-component of the IMF (<By> = –6.3 nT, <Bz> = –1.7 nT) is a cusp with a width of ~1.4° of latitude with a flat top in the latitudinal Pi profile. Comparison of the pressure distributions observed at low heights with data from high-apogee satellites confirmed the possibility of describing the formation of the cusp as a diamagnetic cavity and using observations in the cusp to determine the ion pressure in the magnetosheath.
