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The generation of hard X-rays and relativistic protons observed during solar flares

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Abstract

The flare source of thermal X-rays above a magnetic arch in the corona arises from the dissipation of the magnetic energy of the current sheet formed at the reconnection of magnetic-field lines. The sources of hard X-rays emitted from the footpoints of the magnetic arch are beams of electrons accelerated in field-aligned currents induced by the Hall electric field generated in the current sheet. Both the hard X-rays detected above the active region and the type III radio emission are radiated by electrons accelerated in the field-aligned currents induced by Alfven waves. The solar cosmic rays are emitted promptly at the instant of the flare. It is important that the Lorentz electric field accelerates protons along the singular magnetic X line. The relativistic protons propagate along the interplanetary magnetic field. These protons have exponential spectra, typical for acceleration occurring in current sheets. A mechanism that is relevant for the generation of delayed cosmic rays, which demonstrate significant anisotropy and a power-law spectrum with γ ∼5, is also discussed.

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Authors and Affiliations

  1. Institute of Astronomy, Russian Academy of Sciences, ul. Pyatnitskaya 48, Moscow, 109017, Russia

    I. M. Podgorny

  2. Polar Geophysical Institute, Kola Science Center, Russian Academy of Sciences, Academgorodok str. 26a, Apatity, Murmanskaya oblast, 184209, Russia

    Yu. V. Balabin & E. V. Vashenyuk

  3. Lebedev Physical Institute, Russian Academy of Sciences, Leninskii pr. 53, Moscow, 117924, Russia

    A. I. Podgorny

Authors
  1. I. M. Podgorny
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  2. Yu. V. Balabin
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  3. E. V. Vashenyuk
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  4. A. I. Podgorny
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Original Russian Text © I.M. Podgorny, Yu.V. Balabin, E.V. Vashenyuk, A.I. Podgorny, 2010, published in Astronomicheskiĭ Zhurnal, 2010, Vol. 87, No. 7, pp. 704–716.

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Podgorny, I.M., Balabin, Y.V., Vashenyuk, E.V. et al. The generation of hard X-rays and relativistic protons observed during solar flares. Astron. Rep. 54, 645–656 (2010). https://doi.org/10.1134/S1063772910070085

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  • DOI: https://doi.org/10.1134/S1063772910070085

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