CORONAL HOLE PLUMES AND ACTIVE REGION FAN LOOPS ARE STRUCTURES IN THE SOLAR CORONA THAT ARE MAINTAINED AT TEMPERATURES OF 1 MK FOR PERIODS OF HOURS TO DAYS. DR. YOUNG S PROJECT WILL INVESTIGATE HOW THESE STRUCTURES ARE HEATED BY UTILIZING DATA FROM NASA S SOLAR DYNAMICS OBSERVATORY (SDO) THE INTERFACE REGION IMAGING SPECTROGRAPH (IRIS) AND HINODE SPACECRAFT. DR. YOUNG HAS DIVIDED THE PROJECT INTO THREE WORK PACKAGES (WP): WP1: IDENTIFY LONG-TERM (HOURS) CORRELATIONS BETWEEN CORONAL EMISSION MAGNETIC FIELD STRENGTH AND PHOTOSPHERIC FLOW VELOCITIES USING SDO DATA. WP2: MAKE THE MOST DETAILED SURVEY YET OBTAINED OF SPECTROSCOPIC PROPERTIES (TEMPERATURE DENSITY ABUNDANCES VELOCITY) OF THE DIFFERENT PLUME TYPES USING EIS AND IRIS DATA. WP3: IDENTIFY SMALL-SCALE SHORT-TERM HEATING EVENTS IN PLUMES USING AIA EIS AND IRIS AND CORRELATE WITH MAGNETIC FIELD EVOLUTION FROM HMI AND SOT. WP1 AND WP3 CRITICALLY DEPEND ON THE ANALYSIS OF PHOTOSPHERIC IMAGING DATA AND DR. ATTIE PROPOSES TO PERFORM THE ANALYSIS DESCRIBED IN THE SECTIONS BELOW. DR. ATTIE IS UNIQUELY QUALIFIED FOR THIS WORK DUE TO HIS DEVELOPMENT OF A STATE-OF-THE-ART BALLTRACKING FRAMEWORK (ATTIE&INNES 2015; ATTIE ET AL. 2016) THAT ENABLES MAGNETIC FLUX CANCELLATION RATES AND PHOTOSPHERIC VELOCITIES TO BE ACCURATELY MEASURED FROM PHOTOSPHERIC IMAGING DATA.