Helical magnetic fields in filaments

Details Helical magnetic fields in filaments Helical magnetic fields in filaments

Nov 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994soph..155...69r&link_type=abstract

Solar Physics (ISSN 0038-0938), vol. 155, no.1, p. 69-97

Physics

210

Helical Flow, Solar Corona, Solar Magnetic Field, Solar Prominences, Stellar Models, Synoptic Measurement, Zeeman Effect

Scientific paper

For both even and odd-numbered solar cycles, right-hand heliform filaments predominate at middle and high latitudes in the northern hemisphere while left-handed ones predominate in the south. This recent discovery has prompted a re-examination of past measurements of magnetic fields in prominences. This re-examination indicates that Rsust (1967), in his interpretation of solar cycle 20 measurements in terms of the Kippenhahn-Schlueter model, and Leroy, Bommeir, and Sahal-Brechot (1984), in their interpretation of solar cycle 21 measurements in terms of the Kuperus-Raadu model were both misled by the global pattern of helicity. While the original magnetic field measurements are consistent with the new results about heliform magnetic fields in filaments, neither of the well-known classes of two-dimensional models can produce both the proper axial field direction and the observed pattern of helicity. A global, subsurface velocity pattern that would twist the fields before emergence as filaments seems to be required. In this paper a twisted-flux-rope-model consistent with the new understanding of filament fields is presented. The model is based on a constant-alpha solution of the magnetostatic equations, where electric current density j(r) = alpha B(r). The model filament has dimensions in general agreement with observations. It is shown to be stable if the length is less than 140,00 km to 1,400,00 km, depending on the value of alpha. The model also provides a new explanation of eruptive prominences and for the origin of the entrained material.

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