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Paper: Probing the Solar Corona Using the VLBA
Volume: 340, Future Directions in High Resolution Astronomy: The 10th Anniversary of the VLBA
Page: 440
Authors: Kortenkamp, P.S.; Spangler, S.R.; Mutel, R.L.
Abstract: In the absence of in situ spacecraft measurements inside 0.3 AU, remote sensing observations of the solar wind throughout its acceleration region (5 to 50 Rsolar) provide information on characteristics of plasma turbulence, which may assess the role such turbulence plays in heating the corona and accelerating the solar wind. We have used the Very Long Baseline Array interferometer to observe the radio sources 3C273 and 3C279 at solar elongations of 18 and 32 Rsolar respectively and at frequencies of 2.26, 4.98, and 8.41 GHz. We measured solar-wind-induced temporal fluctuations in the interferometer phase which contain information on the level and propagation speed of solar wind density fluctuations. Radio images were also created and analyzed to determine the magnitude and anisotropy of the angular broadening due to the solar wind turbulence.
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