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We perform a detailed analysis of the thermal structure of the region abovethe post-eruption arcade for a flare that occurred on 2011 October 22. Duringthis event, a sheet of hot plasma is visible above the flare loops in the 131\AA\ bandpass of the Atmospheric Imaging Assembly (AIA) on the {\it SolarDynamics Observatory (SDO)}. Supra-arcade downflows (SADs) are observedtraveling sunward through the post-eruption plasma sheet. We calculatedifferential emission measures using the AIA data and derive an emissionmeasure weighted average temperature in the supra-arcade region. In areas wheremany SADs occur, the temperature of the supra-arcade plasma tends to increase,while in areas where no SADs are observed, the temperature tends to decrease.We calculate the plane-of-sky velocities in the supra-arcade plasma and usethem to calculate the potential heating due to adiabatic compression andviscous heating. Ten of the 13 SADs studied have noticeable signatures in boththe adiabatic and the viscous terms. The adiabatic heating due to compressionof plasma in front of the SADs is on the order of 0.1 - 0.2 MK/s, which issimilar in magnitude to the estimated conductive cooling rate. This resultsupports the notion that SADs contribute locally to the heating of plasma inthe supra-arcade region. We also find that in the region without SADs, theplasma cools at a rate slower than the estimated conductive cooling, indicatingadditional heating mechanisms may act globally to keep the plasma temperaturehigh.

An exploration of heating mechanisms in a supra-arcade plasma sheet formed after a coronal mass ejection