Speaker
Description
We present the analysis of spectropolarimetric data obtained with the CRISP instrument at the SST in the Ca II 845.2 nm line. We used the Weak-field approximation (WFA) to obtain information about the magnetic field present in chromospheric spicules and coronal rain clumps. Albeit being computationally simple to implement, to correctly apply the WFA requires a careful assessment of the conditions of the plasma. Magnetic fields of the order of hundreds of Gauss were inferred in a large number of spicule and coronal rain pixels. In the later case, the full magnetic field vector could be determined. We also combined simultaneous Ca II 845.2 nm and Hα intensity observations to estimate the temperature and non-thermal velocity of the plasma in coronal rain and spicules. The statistical distribution of the temperature of spicules (coronal rain) peaks at 15,000 K (20,000 K) and the microturbulent velocity lies in the range 5-20 km/s (0-15 km/s) and peaks at 12 km/s (5 km/s).
