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It was found out that the distribution's shape of the in-ecliptic (as well asradial) component of the interplanetary magnetic field (IMF) significantlychanges with the heliocentric distance, which poorly corresponds to classicalmodels of the solar wind and the interplanetary magnetic field (IMF) expansion.For example, distributions of the radial photospheric and the source surface'smagnetic field in the ecliptic plane are Gaussian-like, the distribution of theradial IMF component at the Earth orbit demonstrates two-humped shape, and itbecomes again Gaussian-like at 3-4 AU. These differences lead to lack ofcorrespondence between simulations of the IMF behaviour at 1 AU andobservations. Our results indicate that picture of the IMF expansion into spaceis more complicated than usually considered, and the sector structure is notthe only source of the two-humped shape of the in-ecliptic or radial IMFcomponent. We have analysed data from different spacecraft at the distancesfrom 0.29 AU to 4 AU and found that the shape of the radial IMF componentdistribution strongly depends on a heliocentric distance and a heliolatitude.The "two-humped IMF" effect is most brightly expressed at low heliolatitudes at0.7-2 AU, but it fully disappears at 3-4 AU. There is also dependence of theIMF distributions' view on a solar cycle due to active processes, such as solarflares and CMEs. We suppose that the in-ecliptic solar wind field at 1 AU isinfluenced by solar active regions in a high degree, and actually thedistribution is the three-humped: two humps correspond to the IMF from themiddle and high heliolatitudes and the third one is the theoretically expecteddistribution from the solar field nearby the heliomagnetic equator. Vanishingof the IMF zero-component with the distance from the Sun partially could be aresult of a magnetic reconnection at the current sheets in the solar wind.

On the nature of the in-ecliptic interplanetary magnetic field's two-humped distribution at 1AU