By J. O. Stenflo (auth.), K. N. Nagendra, J. O. Stenflo (eds.)
Novel tools for high-precision imaging polarimetry have opened new probabilities, not just for diagnostics of magnetic fields, but additionally for exploring results in radiative scattering, atomic physics, spectral line formation and radiative move. The observational advances have motivated quite a few theoretical advancements, for example in vector radiative move and methods for inverting polarized line profiles. the current quantity offers a entire and up to date account of this speedily evolving and interdisciplinary box of technology. it really is in line with the oral displays given on the 2d overseas Workshop on Solar Polarization held in Bangalore, India, in October 1998.
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Additional resources for Solar Polarization: Proceedings of an International Workshop held in Bangalore, India, 12–16 October 1998
Example text
The diffraction from each sinusoidal grating (corresponding to one Fourier component) has to be determined. The coherent sum of all these sinusoidal diffraction gratings has to be considered when calculating the Mueller matrix for the scattering process. This is obviously adernanding job that is outside the scope of this investigation. In the following we construct a model of the influence of polarized, instrumentally scattered light on precision linear polarization measurements above the limb.
1), and, more recently, with the inclusion of coherent scattering in the formalism. These last results (Sect. 2) are obtained by working in the atomic rest frame within the 2-level atom approximation (with unpolarized lower level). In Sects.
Results für the quiet Sun We have made a large number of recordings of the scattering polarization in the Ca I 4227 and Sr II 4078 A lines in different solar regions, at various latitudes, center-to-limb distances, and times. Usually the observations have been made around the spring or fall equinox, when the instrumental polarization of the Gregory-Coude telescope is minimal. In Paper I the Q / I profiles (with Q defined as the linear polarization oriented parallel to the nearest solar limb) of the Ca I line were analyzed, in Paper H the behavior of the Q/ land U / I profiles of the Sr II line were explored.