Remote sensing of the heliospheric solar wind using radio astronomy methods and numerical simulations |
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Authors: | S Ananthakrishnan |
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Institution: | (1) National Center for Radio Astrophysics, Tata Institute of Fundamental Research, Pune, India |
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Abstract: | The ground-based radio astronomy method of interplanetary scintillations (IPS) and spacecraft observations have shown, in
the past 25 years, that while coronal holes give rise to stable, reclining high speed solar wind streams during the minimum
of the solar activity cycle, the slow speed wind seen more during the solar maximum activity is better associated with the
closed field regions, which also give rise to solar flares and coronal mass ejections (CME’s). The latter events
increase significantly, as the cycle maximum takes place. We have recently shown that in the case of energetic flares one
may be able to track the associated disturbances almost on a one to one basis from a distance of 0.2 to 1 AU using IPS methods.
Time dependent 3D MHD models which are constrained by IPS observations are being developed. These models are able to simulate
general features of the solar-generated disturbances. Advances in this direction may lead to prediction of heliospheric propagation
of these disturbances throughout the solar system. |
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Keywords: | Sun heliosphere solar wind |
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