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Radiation effects on the MHD wave behavior in the solar corona

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Abstract

The effect of radiation losses on the dispersion and damping of magnetohydrodynamic waves in the solar corona is studied. The conditions are determined under which radiation losses are most appreciable. A damping of kink modes of coronal loops with plasma temperatures within 106–106.3 K and 106.3–107 K are compared. It is concluded that the radiation damping dominates in the temperature range 106–106.3 K, which can cause the observed fast damping of kink oscillations of coronal loops. Radiation losses should be taken into account in full magnetohydrodynamic equations with radiative transfer.

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Authors and Affiliations

  1. Kalmyk State University, Elista, Russia

    B. B. Mikhalyaev & O. V. Khongorova

  2. Skobeltsyn Institute of Nuclear Physics, Lomonosov Moscow State University, Moscow, Russia

    I. S. Veselovskii

  3. Space Research Institute, Russian Academy of Sciences, Moscow, Russia

    I. S. Veselovskii

Authors
  1. B. B. Mikhalyaev
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  2. I. S. Veselovskii
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  3. O. V. Khongorova
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Original Russian Text © B.B. Mikhalyaev, I.S. Veselovskii, O.V. Khongorova, 2013, published in Astronomicheskii Vestnik, 2013, Vol. 47, No. 1, pp. 53–60.

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Mikhalyaev, B.B., Veselovskii, I.S. & Khongorova, O.V. Radiation effects on the MHD wave behavior in the solar corona. Sol Syst Res 47, 50–57 (2013). https://doi.org/10.1134/S0038094612060056

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  • DOI: https://doi.org/10.1134/S0038094612060056

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