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Peculiarities of the plasma mechanism of radio emission from late-type stars

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Abstract

The plasma mechanism of radio emission in the coronas of late-type stars is shown to be considerably more efficient than that in the solar corona because of the high plasma temperature in their magnetic arches. This is attributable to an increase in the length of plasma-wave conversion into electromagnetic waves and a decrease in the optical depth of collisional wave absorption. Magnetic-arch filamentation results in a decrease in the intensity of the fundamental-tone radio emission and in the relative dominance of the second-harmonic radio emission. The efficiency of the fundamental-tone radio emission increases with plasma density in a coronal arch. The plasma mechanism accounts for the high brightness temperature of the flare radio emission from stars (≥1014 K).

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Authors and Affiliations

  1. Institute of Applied Physics, Russian Academy of Sciences, ul. Ul’yanova 46, Nizhnii Novgorod, 603600, Russia

    V. V. Zaitsev

  2. Pulkovo Astronomical Observatory, Russian Academy of Sciences, Pulkovskoe sh. 65, St. Petersburg, 196140, Russia

    E. G. Kupriyanova & A. V. Stepanov

Authors
  1. V. V. Zaitsev
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  2. E. G. Kupriyanova
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  3. A. V. Stepanov
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__________

Translated from Pis’ma v Astronomicheski\(\overset{\lower0.5em\hbox{$\smash{\scriptscriptstyle\smile}$}}{l} \) Zhurnal, Vol. 26, No. 11, 2000, pp. 855–861.

Original Russian Text Copyright © 2000 by Za\(\overset{\lower0.5em\hbox{$\smash{\scriptscriptstyle\smile}$}}{l} \)tsev, Kupriyanova, Stepanov.

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Zaitsev, V.V., Kupriyanova, E.G. & Stepanov, A.V. Peculiarities of the plasma mechanism of radio emission from late-type stars. Astron. Lett. 26, 736–742 (2000). https://doi.org/10.1134/1.1323280

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