Polarimetry of Solar Pores

Details Polarimetry of Solar Pores Polarimetry of Solar Pores

Mar 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996soph..164..311s&link_type=abstract

Solar Physics, Volume 164, Issue 1-2, pp. 311-320

Physics

12

Solar Magnetic Fields, Pores, Polarimetry

Scientific paper

We address the magnetic field structure of solar pores. The data were obtained at the Gregory Coudè telescope at Izaña using the AT1 CCD camera system to observe pores with three spectral lines: one magnetically sensitive line, recording all 4 Stokes profiles, and two g = 0 lines where only the intensity profiles were measured. The data reduction included the standard procedure (removing dark current and flatfielding) as well as destretching of the polarimetric spectra and removing the non-magnetic straylight by means of a 2-d deconvolution of the observed intensity variation using a Lucy-Richardson restoration algorithm. In the following analysis we first determined the temperature- and pressure stratification of the pore using the g = 0 lines and then applied an inversion of the Stokes profiles to get the parameters of the magnetic field. Across the pore we find a strong variation of the resulting field strength as well as of the inclination and the azimuth, consistent with the assumption of a canopy forming in the higher atmosphere.

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