| Abstract : | Quantitative information on vector magnetic field is crucial to understand various dynamics which take place in the solar atmosphere such as mechanisms of energy transport, plasma heating, triggering of flares/CMEs, formation and evolution of coronal features and many more. Magnetic field measurements at the photospheric heights are relatively well established and there has been a significant progress at the chromosphere as well. However, coronal magnetic field measurements are sparse. In this context, we have explored the diagnostic capabilities of spectral lines in the ultra-violet (EUV and FUV) wavelength range in terms of their sensitivity to the Hanle and the Zeeman effect. Spectral lines corresponding to electric-dipole (E1) and magnetic-dipole (M1) transition have been investigated. It is found that combinations of Hanle sensitive lines are best suited for probing the coronal magnetic field. In this presentation, we will explain how combinations of spectral lines with varied Hanle sensitivity but with identical temperature sensitivity can be used to infer the complete vector field information at the solar corona. |
