POLARIMETRY OF SOLAR PORES

We address the magnetic field structure of solar pores. The data were obtained at the Gregory Coude telescope at Izana using the AT1 CCD cam era system to observe pores with three spectral lines: one magneticall y sensitive line, recording all 4 Stokes profiles, and two g = 0 lines where only the intensity profiles were measured. The data reduction i ncluded 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 observ ed intensity variation using a Lucy-Richardson restoration algorithm. In the following analysis we first determined the temperature- and pre ssure stratification of the pore using the g = 0 lines and then applie d an inversion of the Stokes profiles to get the parameters of the mag netic field. Across the pore we find a strong variation of the resulti ng field strength as well as of the inclination and the azimuth, consi stent with the assumption of a canopy forming in the higher atmosphere .