Please use this identifier to cite or link to this item: http://hdl.handle.net/2248/364
Title: Structure and Dynamics of the Solar Wind
Authors: Vats, Hari Om
Keywords: Solar Wind;Solar Corona
Issue Date: 1986
Publisher: Indian Institute of Astrophysics, Bangalore
Citation: Kodaikanal Observatory Bulletins Series A, Vol. 6, pp. 86-96
Abstract: Due to high temperature and very small temperature gradient with height, the solar corona is not in hydrostatic equilibrium but is continuously expanding into the inter-planetary space. The expanding coronal plasma is known as the solar wind and its characteristics are studies by 'insitu' and indirect methods. In this paper, we shall highlight capabilities of indirect measurements carried out by the interplanetary scintillation (IPS) technique. A new method for estimation of the solar wind speed using IPS observations of a single station is described. The advantage of this method which is based on refractive scattering approach over the earlier procedures is discussed. It seems that this method can be satisfactorily used in almost all situations of scattering inthe solar wind. The determination of solar wind speed requires theoretical simulation of the observed spectra in most cases, but some of the observations which happen to satisfy the diffractive scattering limits are easier to deal with the new method.
URI: http://hdl.handle.net/2248/364
ISSN: 0374-3632
Appears in Collections:Kodaikanal Observatory Bulletins (1905 - 1997 )
IIAP Publications

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