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Title: 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 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.
 [1] ;  [1] ;  [1] ;  [2] ;  [3]
  1. Univ. of Alabama, Huntsville, AL (United States). Center for Space Plasma and Aeronomic Research
  2. AFRL/RCBXS (United States)
  3. Tata Inst. of Fundamental Research, Bombay (India). Radio Astronomy Centre, NCRA
Publication Date:
OSTI Identifier:
Grant/Contract Number:
SC0008334; OCI-1144120
Accepted Manuscript
Journal Name:
Journal of Physics. Conference Series
Additional Journal Information:
Journal Volume: 642; Journal ID: ISSN 1742-6588
IOP Publishing
Research Org:
Univ. of Alabama, Huntsville, AL (United States)
Sponsoring Org:
USDOE Office of Science (SC), Fusion Energy Sciences (FES) (SC-24); National Science Foundation (NSF)
Country of Publication:
United States