Please use this identifier to cite or link to this item:
Title: Pressure structure of solar coronal loops. III
Authors: Sreedharan, T. D
Sasidharan, K
Satya Narayanan, A
Krishan, V
Keywords: Solar Corona;Solar activity;solar magnetic field
Issue Date: Dec-1992
Publisher: Springer Netherlands
Citation: Solar Physics, Vol. 142, No. 2, pp. 249 - 264
Abstract: The theory of ideal magnetohydrodynamic turbulence in cylindrical geometry is used to study the steady-state structure of a coronal loop. The pressure profile is derived from MHD equations by representing the velocity and magnetic fields as the superposition of Chandrasekhar-Kendall functions. Such a representation brings out the three-dimensional structure of the pressure in the coronal loop. The radial, azimuthal, and axial variations of the pressure for a constant density loop are discussed in detail. The pressure has an oscillatory behavior for different azimuthal angles at some radial positions. This study predicts more features in pressure than can be compared with the presently available observations.
Appears in Collections:IIAP Publications

Files in This Item:
File Description SizeFormat 
Vinod.pdf1.12 MBAdobe PDFView/Open

Items in DSpace are protected by copyright, with all rights reserved, unless otherwise indicated.