|STRUCTURE AND EVOLUTION OF SOLAR FILAMENTS AS OBSERVED BY MAST TELESCOPE|
|N. Srivastava., Udaipur Solar Observatory, email@example.com|
|S. Mathew, Udaipur Solar Observatory, PRL, firstname.lastname@example.org|
|R. Ankala, Udaipur Solar Observatory, PRL, email@example.com|
|P. Venkatakrishnan, Udaipur Solar Observatory, PRL, firstname.lastname@example.org|
|R. Bireddy, Udaipur Solar Observatory, PRL, email@example.com|
|H-alpha Observations suggest that there is a continuous spectrum of filaments ranging from active region filaments, intermediate filaments to quiescent filaments. Quiescent filaments are generally tall with many barbs in comparison to the active region filaments which are low and have barbs show thread like structures which emerge from the main body or the spine of the filament. We present a study of filaments based on high resolution observations obtained from the newly installed Multi-Application Solar Telescope at the Udaipur Solar Observatory (USO). We will examine the changes in magnetic flux as observed by HMI (aboard SDO) in the region surrounding the H-alpha barb location. Simultaneous observations in H-alpha and g-band will also be obtained to understand rooting of the chromospheric barbs into the photosphere. This study will improve our understanding of the stability of filaments.