Photospheric line-tying conditions for the MHD stability of coronal magnetic fields

Details Photospheric line-tying conditions for the MHD stability of coronal magnetic fields Photospheric line-tying conditions for the MHD stability of coronal magnetic fields

Jun 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986soph..105..307h&link_type=abstract

Solar Physics (ISSN 0038-0938), vol. 105, June 1986, p. 307-312.

Physics

33

Density Distribution, Magnetohydrodynamic Stability, Photosphere, Solar Corona, Solar Magnetic Field, Boundary Value Problems

Scientific paper

Using the localised, ballooning ordering, the effect of a density stratification on the ideal MHD stability of magnetic fields is investigated. It is found that, when the photospheric density is very much greater than the coronal value, the line tying conditions are best simulated by assuming that all coronal disturbances vanish at the photospheric boundary. This is commonly known as the rigid wall conditions.

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