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Magnetically Driven Motions in Solar Corona

  • B. V. Somov
  • S. I. Syrovatskii
Part of the International Astronomical Union / Union Astronomique Internationale book series (IAUS, volume 91)

Abstract

Solution of the nonlinear MHD problem of plasma flow in an increasing dipolar magnetic field is obtained in the approximation of a strong field. The distributions of plasma velocity, displacement, and density are calculated. The situation when the magnetic dipole is ‘increased’ by rapid process of magnetic reconnection or current sheet rupture is illustrated. Possible applications are discussed in connection with plasma ejections from chromosphere in corona.

Keywords

Field Line Current Sheet Solar Phys Magnetic Reconnection Solar Corona 
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References

  1. Platov, Yu.V., Somov, B.V., and Syrovatskii, S.I.: 1973, Solar Phys. 30, pp. 139–147.CrossRefADSGoogle Scholar
  2. Somov, B.V. and Syrovatskii, S.I.: 1972, Soviet Phys. JETP 34, pp. 332–335.ADSGoogle Scholar
  3. Syrovatskii, S.I.: 1969, Astrophys. Space Sci. 4, pp. 246–251.CrossRefADSGoogle Scholar
  4. Syrovatskii, S.I. and Somov, B.V.: 1979, Physical driving forces and models of coronal responses (Invited paper presented at this symposium) .Google Scholar
  5. Tanaka, K.: 1978, Solar Phys. 58, pp. 149–163.CrossRefADSGoogle Scholar

Copyright information

© IAU 1980

Authors and Affiliations

  • B. V. Somov
    • 1
  • S. I. Syrovatskii
    • 1
  1. 1.Lebedev Physical InstituteAcademy of Sciences of the USSRMoscowUSSR

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