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The stream structure of the solar supercorona

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Abstract

The scattering properties of the solar-wind plasma in the region of a subsonic flow at the distances R∼(10–16)R⊙ from the Sun were studied by the radio occultation method in 1988–92. The long-term dynamics of the large-scale structure of solar wind in this region is similar to the well-known variations of the corona observed in optics. The generality of long-term evolution in the stream structure of flows at different distances from the Sun indicates the existence of a single mechanism of acceleration of the large-scale flows giving rise to solar wind.

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Authors
  1. N. A. Lotova
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  2. K. V. Vladimirskii
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  3. O. A. Korelov
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Additional information

Institute of Geomagnetism, the lonosphere, and Radio-Wave Propagation, Russian Academy of Sciences, Troitsk, Moscow region; P. N. Lebedev Physical Institute, Russian Academy of Sciences, Moscow; Radiophysical Research Institute, Niznhy Novogorod. Translated from Izvestiya Vysshikh Uchebnykh Zavedenii, Radiofizika, Vol. 38, No. 9, pp. 920–925, September, 1995.

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Lotova, N.A., Vladimirskii, K.V. & Korelov, O.A. The stream structure of the solar supercorona. Radiophys Quantum Electron 38, 598–601 (1995). https://doi.org/10.1007/BF01037843

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  • DOI: https://doi.org/10.1007/BF01037843

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