Two-dimensional steady-state pressure structure in a coronal loop. I - Superposition of two Chandrasekhar-Kendall functions (n = 0, M = 0; N = 1, M = 0)

Details Two-dimensional steady-state pressure structure in a coronal loop. I - Superposition of two Chandrasekhar-Kendall functions (n = 0, M = 0; N = 1, M = 0) Two-dimensional steady-state pressure structure in a coronal loop. I - Superposition of two Chandrasekhar-Kendall functions (n = 0, M = 0; N = 1, M = 0)

Jul 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991soph..134...99c&link_type=abstract

Solar Physics (ISSN 0038-0938), vol. 134, July 1991, p. 99-107; Comment, p. 109. Research supported by Council of Science and Te

Physics

2

Coronal Loops, Pressure Distribution, Solar Corona, Chandrasekhar Equation, Solar Magnetic Field, Steady State

Scientific paper

The steady-state pressure profile within a solar coronal loop is presently investigated by expressing the magnetic field and fluid velocity in terms of two Chandrasekhar-Kendall functions. A radial and axial pressure structure is found for the constant-density loops; while at the base of the loop the pressure increases steeply outwards along the radius, it decreases slowly at the apex. The radial pressure variation is minimal at L/5, where L is the foot-to-foot length of the loop. Pressure increases from the base up to z = 3L/8 along the loop axis, and then decreases up to the apex; at the surface, however, the pressure decreases from the base to the apex.

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