The filamentary structure in sunspots

Details The filamentary structure in sunspots The filamentary structure in sunspots

Mar 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984chjss...3..261h&link_type=abstract

(Chinese Journal of Space Science, vol. 3, 1983, p. 261-268) Chinese Astronomy and Astrophysics (ISSN 0275-1062), vol. 8, March

Astronomy and Astrophysics

Astrophysics

Equilibrium Equations, Penumbras, Perturbation Theory, Solar Magnetic Field, Solar Prominences, Sunspots, Dynamic Stability, Magnetostatics

Scientific paper

An analytical model of the filamentary structure of sunspots is developed within the framework of magnetostatic-equilibrium theory and a small-perturbation assumption, neglecting convective motion and considering dynamic equilibrium only. Following the method of Hu et al. (1983), zeroeth and first order solutions of the nonaxisymmetric equilibrium equations are obtained, corresponding to the overall structure of the sunspot and to its filamentary structures. The dark filaments of the penumbral region are shown to be related to stronger magnetic fields, as observed by Beckers and Schroeter (1968).

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