Investigation of coronal Loops on the solar atmosphere

In this thesis, physical properties (such as temperature, velocity etc.) of two warm coronal loops are investigated and then the magnetic fields, which are placed at the four foot-points of these loops, are analyzed in detail. These loops have observed on May 10, 2016 (Loop 1) and December 17, 2015 (Loop 2) and their active region (AR) numbers in National Oceanic Atmospheric Administration (NOAA) are AR12542 and AR12470, respectively. One of the loops (Loop 1) is connecting a plage region to a sunspot umbra. The analysis showed that temperatures of these loops are in the range of about 1.0 to 1.5 Million Kelvin (MK) and they are comprised in the category of warm loops. During the analysis, Solar Dynamics Observatory (SDO) and Goode Solar Telescope (GST) data were used to identify the events and understand the causes. The study indicates loop brightening were associated with magnetic flux emergence and cancellation processes observed in SDO's Helioseismic and Magnetic Imager and GST's Near InfraRed Imaging Spectrapolarimeter (HMI) data. The observed activity was driven by magnetic reconnection between small-scale emerging dipoles and large-scale pre-existing fields, suggesting that the reconnection occurred in the lower Chromosphere at the edge of an extended plage region, where the loops were rooted. We suggest that plasma, evaporated during these reconnection events, gradually filled the loops and as it cooled the visible density from propagated from one foot-point of the loop to another at a rate of 80-110 km s-1. This study also indicates that at least some of the bright loops seen in SDO Atmospheric Imaging Assembly (AIA) images rooted in sunspot umbra may be heated due to magnetic activity taking place at the remote (non-sunspot) foot-point.