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The relative amount of high temperature plasma has been found to be a usefuldiagnostic to determine the frequency of coronal heating on sub-resolutionstructures. When the loops are infrequently heated, a broad emission measure(EM) over a wider range of temperatures is expected. A narrower EM is expectedfor high frequency heating where the loops are closer to equilibrium. The softX-ray spectrum contains many spectral lines that provide high temperaturediagnostics, including lines from Fe XVII-XIX. This region of the solarspectrum will be observed by the Marshall Grazing Incidence Spectrometer(MaGIXS) in 2020. In this paper, we derive the expected spectral linesintensity in MaGIXS to varying amounts of high temperature plasma todemonstrate that a simple line ratio of these provides a powerful diagnostic todetermine the heating frequency. Similarly, we examine ratios of AIA channelintensities, filter ratios from a XRT, and energy bands from the FOXSI soundingrocket to determine their sensitivity to this parameter. We find that bothFOXSI and MaGIXS provide good diagnostic capability for high-temperatureplasma. We then compare the predicted line ratios to the output of a numericalmodel and confirm the MaGIXS ratios provide an excellent diagnostic for heatingfrequency.

Solar Active Region Heating Diagnostics from High Temperature Emission using the Marshall Grazing Incidence X-ray Spectrometer (MaGIXS)