Modeling solar wind with boundary conditions from interplanetary scintillations

Interplanetary scintillations make it possible to create three-dimensional, time- dependent distributions of the solar wind velocity. Combined with the magnetic field observations in the solar photosphere, they help perform solar wind simulations in a genuinely time-dependent way. Interplanetary sci...

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Bibliographic Details
Published in:Journal of physics. Conference series 2015-09, Vol.642 (1), p.12016
Main Authors: Manoharan, P, Kim, T, Pogorelov, N V, Arge, C N, Manoharan, P K
Format: Article
Language:English
Subjects:
ASTRONOMY AND ASTROPHYSICS
Boundary conditions
Celestial bodies
Photosphere
Physics
Saturn
Solar magnetic field
Solar wind
Solar wind velocity
Time dependence
Wind speed
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Summary:Interplanetary scintillations make it possible to create three-dimensional, time- dependent distributions of the solar wind velocity. Combined with the magnetic field observations in the solar photosphere, they help perform solar wind simulations in a genuinely time-dependent way. Interplanetary scintillation measurements from the Ooty Radio Astronomical Observatory in India provide directions to multiple stars and may assure better resolution of transient processes in the solar wind. In this paper, we present velocity distributions derived from Ooty observations and compare them with those obtained with the Wang-Sheeley-Arge (WSA) model. We also present our simulations of the solar wind flow from 0.1 AU to 1 AU with the boundary conditions based on both Ooty and WSA data.
ISSN:1742-6588
1742-6596
DOI:10.1088/1742-6596/642/1/012016