Vector magnetic fields in prominences. II - HeI D3 Stokes profiles analysis for two quiescent prominences

Details Vector magnetic fields in prominences. II - HeI D3 Stokes profiles analysis for two quiescent prominences Vector magnetic fields in prominences. II - HeI D3 Stokes profiles analysis for two quiescent prominences

Apr 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985soph...96..277q&link_type=abstract

Solar Physics (ISSN 0038-0938), vol. 96, April 1985, p. 277-292.

Physics

31

D Lines, Helium Ions, Solar Magnetic Field, Solar Prominences, Spectrum Analysis, Stokes Theorem (Vector Calculus), Circular Polarization, Emission Spectra, Linear Polarization

Scientific paper

The Stokes components of HeI D3 emission in two quiescent prominences, using full spectral profile measurements, are analyzed to derive vector magnetic fields. Two independently developed schemes, based on the Hanle effect, are used for interpretation. They involve solutions of the statistical equilibrium equations for the HeI D3 multiplet, including the effect of coherency and full level crossing, which predict the magnetic field dependence of the observed polarization. Derived magnetic field vector solutions for each pair of linear polarization Stokes profiles corresponding to an observational point in the prominence are, intrinsically, not uniquely determined, and a set of possible solutions is usually obtained. However, mutual consistency of these solutions with those independently predicted by the form of the circular polarized component, allow, in almost all cases, rejection of all solutions of a set except one symmetrical pair. Of such a pair, a unique solution can be determined with a high confidence level by reference to independent potential field information. Field vectors are found usually to be close to horizontal and normal to the prominence surface, but extreme exceptions are found. Field values range from 6 G to 60 G. The derived vectorfield configurations and their magnitudes are briefly discussed relative to these prominences and to different quiescent prominence models.

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