Modeling solar wind with boundary conditions from interplanetary scintillations

14th Annual International Astrophysics Conference: Linear and Nonlinear Particle Energization throughout the Heliosphere and Beyond

物理学;天文学

Manoharan, P.^1 ; Kim, T.^1 ; Pogorelov, N.V.^1 ; Arge, C.N.^2 ; Manoharan, P.K.^3

Center for Space Plasma and Aeronomic Research, University of Alabama in Huntsville, United States^1

AFRL/RVBXS, United States^2

Radio Astronomy Centre, NCRA, Tata Institute of Fundamental Research, India^3

关键词: Astronomical observatories;    Interplanetary scintillation;    Multiple stars;    Solar photosphere;    Solar wind flow;    Solar wind velocity;    Transient process;    Wind simulation;   

Others  :  https://iopscience.iop.org/article/10.1088/1742-6596/642/1/012016/pdf
DOI  :  10.1088/1742-6596/642/1/012016

学科分类：天文学(综合)

来源: IOP

【 摘 要 】

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.