On the structure of the interplanetary magnetic field under non-stationary boundary conditions |
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| Authors: | Ludmila T?ísková Igor S Veselovskij Reviewer L K?ivský |
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| Institution: | (1) Geophysical Institute, Czechosl. Acad. Sci., Prague;(2) Institute of Nuclear Physics of the Moscow State University, Moscow |
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| Abstract: | Summary The structure of the interplanetary magnetic field (IMF) is investigated theoretically in a kinematic approximation under frozen-in conditions in the solar wind and non-stationary boundary conditions. As an example, a time-dependent model of the IMF, created in the case of a change of the general magnetic field of the Sun represented by the dipole term, is analyzed. Very simple assumptions as to the field of velocities in the solar wind are made. The results show the formation of zero IMF points of two types(O, X). Points of theO-type are formed and move radially in the equatorial plane. They are surrounded by magnetic clouds with loops of lines of force. Points of theX-type are formed and move radially above the poles.
        mu   u u ¶rt; a a m ma  nam aum n (  ) uamu nu uuu nu uu mu m u ma uaau uu.  am nua ama ¶rt; , ua nu uuu aum n  a, n¶rt;ma ¶rt;un , auu m u.  mum n m m ¶rt;a nm u n¶rt;nu. mam naam aau  m ¶rt; mun(O, X). uO-muna uam u ¶rt;um a¶rt;ua  amua nmu. u aumu aau nmu u uu. uX-muna uam u ¶rt;um a¶rt;ua a¶rt; nau.
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