The magnetic sensitivity of the solar spectrum is caused by the Zeeman effect and by a variety of less familiar physical mechanisms by means of which a magnetic field can create and destroy spectral line polarization. This paper highlights how plasma diagnostic tools based on them could help us to explore the magnetism of the quiet regions of the

We report tests of inversion methods applied to complex Stokes spectra generated by realistic MHD simulations. The average magnetic field strength of the simulations used is of 30 and 140 G, which we believe is representative of quiet solar regions. The behaviour of the Fe I at 1.56 mu m and 630 nm lines is analyzed. The tests have been done with

We investigate the validity of the Stokes V amplitude ratio as an indicator of the magnetic field strength in solar inter-network regions with the help ofMHD simulations. We show that the Stokes V amplitude ratio of the Fe I 15652-15648 Å lines and Fe I 5247-5250 Å lines show a good correlation with the magnetic field strength even for magnetic

Not Available

Not Available

Inversion techniques are presently the most powerful tools to deduce magnetic, dynamic, and thermal properties of the solar plasma from polarization line profiles. The reliability and robustness of Stokes inversions have been confirmed many times by means of numerical tests. Part of the solar physics community, however, is still worried about the