Advertisement

Springer Nature is making SARS-CoV-2 and COVID-19 research free. View research | View latest news | Sign up for updates

Magnetic reconnection in the corona and the loop prominence phenomenon

Abstract

Many classes of transient solar phenomena, such as flares, flare sprays, and eruptive prominences, cause major disruptions in the magnetic geometry of the overlying corona. Typically, the results from Skylab indicate that pre-existing closed magnetic loops in the corona are torn open by the force of the disruption. We examine here some of the theoretical consequences to be expected during the extended relaxation phase which must follow such events. This phase is characterized by a gradual reconnection of the outward-distended field lines. In particular, the enhanced coronal expansion which occurs on open field lines just before they reconnect appears adequate to supply the large downward mass fluxes observed in Ha loop prominence systems that form during the post-transient relaxation. In addition, this enhanced flow may produce nonrecurrent high speed streams in the solar wind after such events. Calculations of the relaxation phase for representative field geometries and the resulting flow configurations are described.

This is a preview of subscription content, log in to check access.

References

  1. Banks, P. M., Nagy, A. F., and Axford, W. I.: 1971, Planet. Space Sci., 19, 1053.

  2. Bruzek, A.: 1964, in W. Hess (ed.), AAS-NASA Symposium on the Physics of Solar Flares, Washington, D.C.

  3. Cox, D. P., and Tucker, W. H.: 1969, Astrophys. J. 157, 1157.

  4. Hundhausen, A. J., Bame, S. J., and Montgomery, M. D.: 1970, J. Geophys. Res. 75, 4631.

  5. Jefferies, J. T., and Orrall, F. Q.: 1963a, “The Solar Spectrum”, Utrecht.

  6. Jefferies, J. T., and Orrall, F. Q.: 1963b, Astrophys. J. 137, 1232.

  7. Jefferies, J. T., and Orrall, F. Q.: 1964, in W. Hess (ed.), AAS-NASA Symposium on the Physics of the Solar Flares, Washington, D.C.

  8. Jefferies, J. T., and Orrall, F. Q.: 1965, Astrophys. J. 141, 519.

  9. Kiepenheuer, K. O.: 1951, Pub. A.S.P. 63, 161.

  10. Kiepenheuer, K. O.: 1953, Acad. Naz. d. Lincei, Convegno Volta 11, 148.

  11. Kiepenheuer, K. O.: 1959, Zs. f. Ap. 48, 290.

  12. Kleczek, J.: 1963, Bull. Astr. Inst. Czechoslovakia 14, 167.

  13. Kleczek, J.: 1964, in W. Hess (ed.), AAS-NASA Symposium on the Physics of Solar Flares, Washington, D.C.

  14. MacQueen, R. M., Eddy, J. A., Gosling, J. T., Hildner, E., Munro, R. H., Newkirk, G. A., Jr., Poland, A. I., and Ross, C. L.: 1974, Astrophys. J. 187, L85.

  15. Menzel, D. H., and Doherty, L. R.: 1963, in J. W. Evans (ed.), ‘The Solar Corona’, IAU Symp. 16.

  16. Newkirk, G. Jr.: 1973, in R. Ramaty and R. G. Stone (eds.), Symposium on High Energy Phenomena on the Sun, NASA Goddard Spaceflight Center, Greenbelt, Maryland, NASA SP-342.

  17. Orrall, F. Q., and Zirker, J. B.: 1961, Astrophys. J. 134, 72.

  18. Orrall, F. Q., and Zirker, J. B.: 1963, in J. W. Evans (ed.), ‘The Solar Corona’, IAU Symp. 16.

  19. Parker, E. N.: 1958, Astrophys. J. 128, 664.

  20. Pneuman, G. W.: 1973, Solar Phys. 28, 247.

  21. Pneuman, G. W., and Kopp, R. A.: 1971, Solar Phys. 18, 258.

  22. Pneuman, G. W., and Kopp, R. A.: 1976, in preparation.

  23. Webb, D. F., Krieger, A. S., and Rust, D. M.: 1976, Solar Phys. 48, 159.

Download references

Author information

Additional information

New address: Los Alamos Scientific Laboratory, Los Alamos, N.M. 87545, U.S.A.

The National Center for Atmospheric Research is sponsored by the National Science Foundation.

Rights and permissions

Reprints and Permissions

About this article

Cite this article

Kopp, R.A., Pneuman, G.W. Magnetic reconnection in the corona and the loop prominence phenomenon. Sol Phys 50, 85–98 (1976). https://doi.org/10.1007/BF00206193

Download citation

Keywords

  • Flare
  • Solar Wind
  • Magnetic Reconnection
  • Relaxation Phase
  • High Speed Stream