Variations of the solar-wind stream structure in the region of subsonic flow during the 11-year solar cycle |
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| Authors: | N A Lotova V N Obridko K V Vladimirskii |
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| Institution: | (1) Institute of Terrestrial Magnetism, Ionosphere, and Radio Propagation, Russian Academy of Sciences, Troitsk, Moscow oblast, 142092, Russia;(2) Lebedev Institute of Physics, Russian Academy of Sciences, Leninski pr. 53, Moscow, 117942, Russia |
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| Abstract: | The large-scale stream structure of the solar wind near the Sun and its evolution during the 11-year solar activity cycle are investigated. The study is based on observations of scattering of the radiation from compact natural radio sources at radial distances R≤14R S (R S is the solar radius). Regular observations were conducted in 1981–1998 on the RT-22 and DKR-1000 radio telescopes of the Russian Academy of Sciences at Pushchino, at λ=1.35 cm and 2.7 m, respectively. The radial dependences of the interplanetary scintillations m(R) and the scattering angle 2?(R) are considered together with the structure of large-scale magnetic fields in the solar corona at R=2.5R S. The entire range of variations in the level of scattering and the associated heliolatitude flow structures in the subsonic solar wind forms over the 11-year solar cycle, as a direct result of the large-scale structure of the evolving magnetic fields at the source of the solar-wind streamlines. |
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