Pressure structure of solar coronal loops. III

Details Pressure structure of solar coronal loops. III Pressure structure of solar coronal loops. III

Dec 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992soph..142..249s&link_type=abstract

Solar Physics (ISSN 0038-0938), vol. 142, no. 2, p. 249-264.

Physics

3

Chandrasekhar Equation, Coronal Loops, Magnetohydrodynamic Turbulence, Pressure Oscillations, Solar Corona, Solar Activity, Solar Magnetic Field, Steady State

Scientific paper

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.

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