Evolution of Flare Generated Magnetohydrodynamic Shock in Solar Wind
1Department of PhysicsS.S.V.CollegeHapur, U.P.-245101 India
2Department Of MathematicsS.C.CollegeBallia,U.P.-277001, India
3Department of Physics IFTM University Moradabad U.P.-244102 India
Email of Corresponding Author:- subodhphysicsccs@gmail.com
http://dx.doi.org/10.22147/jusps-B/280501
A self-similar spherically symmetric model is constructed to describe a blast wave in the solar wind produced by a solar flare. The shock wave is assumed to advance into a conducting gas streaming with a constant velocity ahead of the shock. Numerical solutions are obtained for the distribution of flow variables within the shocked gas for the special choice of parameters and for uniform and non-uniform distribution of density in ambient solar atmosphere. In particular, the time of transit of the shock at the earth’s orbit is calculated. It is observed that the streaming ambient solar atmosphere reducesvariations in flow variables in crossing the shock at earth’s orbit
Copy the following to cite this article:
S.K. SHARMA1, S.N. OJHA2 and NEERAJ KUMAR3, "Evolution of Flare Generated Magnetohydrodynamic Shock in Solar Wind", Journal of Ultra Scientist of Physical Sciences, Volume 28, Issue 5, Page Number , 2016Copy the following to cite this URL:
S.K. SHARMA1, S.N. OJHA2 and NEERAJ KUMAR3, "Evolution of Flare Generated Magnetohydrodynamic Shock in Solar Wind", Journal of Ultra Scientist of Physical Sciences, Volume 28, Issue 5, Page Number , 2016Available from: http://www.ultraphysicalsciences.org/paper/593/
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