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A mechanism for a class of solar coronal disturbances

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Abstract

In this paper, a new ideal magnetohydrodynamic (MHD) model is used to examine the dynamical response of the upper solar atmosphere to injection of cold mass from the photosphere akin to a surge. A significant new physical phenomenon is revealed: the formation of an almost stationary loop prominence in the atmosphere as a consequence of the ejected material. Simultaneously with the formation of this new loop, the simulation exhibits MHD waves that propagate outward (i.e., away from the loop) to excite coronal material. It is conjectured that these waves may trigger a class of coronal disturbances.

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Author notes

  1. Y. Q. Hu

    Present address: Department of Earth and Space Sciences, University of Science and Technology of China, Hefei, Peoples Republic of China

Authors and Affiliations

  1. University of Alabama in Huntsville, Alabama, USA

    S. T. Wu, Y. Q. Hu & S. Wang

  2. Space Environment Laboratory, ERL, National Oceanic and Atmospheric Administration, Boulder, Colorado, USA

    M. Dryer

  3. Space Sciences Laboratory, National Aeronautics and Space Administration, George C. Marshall Space Flight Center, Huntsville, Alabama, USA

    E. Tandberg-Hanssen

Authors
  1. S. T. Wu
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  2. Y. Q. Hu
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  3. S. Wang
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  4. M. Dryer
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  5. E. Tandberg-Hanssen
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Wu, S.T., Hu, Y.Q., Wang, S. et al. A mechanism for a class of solar coronal disturbances. Astrophys Space Sci 83, 189–194 (1982). https://doi.org/10.1007/BF00648551

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  • DOI: https://doi.org/10.1007/BF00648551

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