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Some tails of ram-pressure stripped galaxies are detected in HI, some inHalpha, and some in X-ray (but never all three so far). We use numericalsimulations to probe the conditions for the production of X-ray bright tails,demonstrating that the primary requirement is a high pressure intraclustermedium (ICM). This is because the stripped tail is mostly in pressureequilibrium with the ICM, but mixing leaves it with densities and temperaturesintermediate between the cold gas in the disk and the hot ICM. Given a highenough ICM pressure, this mixed gas lies in the X-ray bright region of thephase diagram. We compare the simulations to observations of the ram pressurestripped tail of ESO 137-001, showing excellent agreement in the total measuredX-ray and Halpha emission and non-flaring morphology of the tail, andconsistent HI measurements. Using these comparisons we constrain the level ofmixing and efficiency of heat conduction in the intracluster medium (ICM)

How To Light It Up: Simulating Ram-Pressure Stripped X-ray Bright Tails