Abstract

The reasons for nonstationary hydrodynamic flows in solar atmospere are reviewed. It is emphasized that a rapid local heating of corona or upper chromosphere can scarcely provide a very large mass of solar plasma ejections observed in corona and interplanetary space. We suggest that coronal transients and interplanetary ejections are produced by magnetic field evolving in solar atmosphere. Magnetic reconnection in current sheets can play essential role in this process. The suitable approximation of strong magnetic field is formulated. Some solutions of MHD equations in this approximation are demonstrated. Their applications to coronal conditions are discussed.

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