SUPER-EARTHS DISPLAY A LARGE DIVERSITY IN THEIR GAS-MASS FRACTIONS AND BULK DENSITIES. THIS DIVERSITY IS ESPECIALLY SURPRISING FOR OBSERVED EXOPLANETS RESIDING IN TIGHTLY-PACKED MULTIPLE-PLANET SYSTEMS. THESE OBSERVATIONS ARE CHALLENGING TO EXPLAIN BY GAS ACCRETION AND SUBSEQUENT SCULPTING BY PHOTO-EVAPORATION ALONE. WE PROPOSE TO INVESTIGATE IF THE LARGE OBSERVED RANGE IN EXOPLANET BULK DENSITIES MAY BE DUE TO ONE OR TWO GIANT IMPACTS THAT OCCURRED LATE IN THE DYNAMICAL EVOLUTION OF SUPER-EARTH SYSTEMS ONCE THE GAS DISK DISSIPATED. SUCH LATE GIANT IMPACTS ARE LIKELY TO BE COMMON BECAUSE SUPER-EARTHS THAT CONTAIN SEVERAL PERCENT OF THEIR TOTAL MASS IN HYDROGEN AND HELIUM MUST HAVE FORMED IN THE PRESENCE OF THE GAS DISK AND THEIR DYNAMICAL INTERACTION WITH THE DISK IS EXPECTED TO HAVE RESULTED IN MIGRATION AND EFFICIENT ECCENTRICITY DAMPING. THIS LEADS TO DENSELY-PACKED PLANETARY SYSTEMS. AS THE GAS DISK DISSIPATES MUTUAL GRAVITATIONAL EXCITATIONS BETWEEN THE PLANETS CAUSE THEIR ECCENTRICITY TO GROW CULMINATING IN ONE OR TWO GIANT IMPACTS BEFORE REACHING LONG-TERM ORBITAL STABILITY. IN OUR PAST WORK WE HAVE SHOWN THAT A GIANT IMPACT CAN EASILY REDUCE THE ENVELOPE-TO-CORE-MASS FRACTION OF AN EXOPLANET BY FACTORS OF 2 OR MORE LEADING TO CHANGES IN BULK DENSITIES OF FACTORS OF 2-4 (INAMDAR&SCHLICHTING 2016). HOWEVER THIS PAST WORK HAS FOCUSED ON THE MECHANICAL ASPECT OF THE IMPACT ONLY AND CONSISTED OF FOLLOWING THE SHOCK GENERATED AT THE IMPACT SITE AS IT PROPAGATES THROUGH THE PLANET AND ITS ATMOSPHERE. HERE WE PROPOSE TO COMPLEMENT THIS PAST WORK BY EXAMINING THE THERMAL ASPECT OF THE IMPACT BY CALCULATING THE HEATING OF THE PLANET S CORE DUE TO THE IMPACT AND THE RESULTING HEAT EXCHANGE BETWEEN THE CORE AND THE ENVELOPE. WE PLAN TO FOLLOW THE THERMAL EVOLUTION OF THE PLANET AND ITS ENVELOPE IN TIME. WE WILL PARAMETERIZE THE IMPACT PROPERTIES NEEDED FOR COMPLETE ATMOSPHERIC LOSS AND THOSE FOR PARTIAL ENVELOPE LOSS. WE WILL TEST HOW THE ATMOSPHERIC LOSS DEPENDS ON THE ATMOSPHERIC COMPOSITION THE TOTAL ATMOSPHERIC MASS AND THE LOCATION FROM THE HOST STAR. PRELIMINARY RESULTS SUGGEST THAT THE THERMAL ASPECT OF THE IMPACT MAY DOMINATE THE ATMOSPHERIC MASS LOSS FOR HYDROGEN AND HELIUM ATMOSPHERES. WE WILL COMBINE THE THERMAL MASS LOSS RESULTS WITH THE ATMOSPHERIC MASS LOSS RESULTS THAT WE OBTAINED FOR THE MECHANICAL/SHOCK COMPONENT OF THE PROBLEM (INAMDAR&SCHLICHTING 2016) TO DETERMINED THE TOTAL ENVELOPE LOSS IN EXOPLANET COLLISIONS. WE WILL THEN USE THESE RESULTS TO TEST IF THE OBSERVED DIVERSITY OF SUPER-EARTHS BULK COMPOSITIONS CAN BE EXPLAINED BY ATMOSPHERIC MASS LOSS DUE TO GIANT IMPACTS OR IF IT HAS TO BE ATTRIBUTED TO DIFFERENT FORMATION PATHS OF THESE SYSTEMS.