Speaker
Description
High-resolution broad-band observations of the Sun reveal a multitude of small-scale structures, everywhere in the photosphere. The increase in resolution usually comes with the cost of increased noise and decreased polarimetric signal.
In this contribution we present an approach inspired by stellar astrophysics, in particular the study of stellar magnetism. We use least-squares deconvolution (LSD) of spectro-polarimetric data to combine the signal from many simultaneously observed spectral lines in spatially highly resolved (∼ 0.07”) Sunrise-III/SUSI observations into a single combined profile. As first results we obtain high-resolution high-contrast Stokes V/I maps that allow for the spatial resolution of weak signals against a 2.5e−4 root-mean-square (RMS) continuum noise background.
In these maps we find patches of both magnetic polarities with a range of Stokes V signal levels, as well as parasitic opposite polarity signals at the border of patches with stronger Stokes V signals. Further analysis of these signals is ongoing.