not take into account the fact that stars may lie below 10th or above the 90th percentiles of the rotation distribution and does not take into account the large spread in X-ray luminosities for stars with a given mass, rotation rate, and luminosity (e.g. see Fig. 3 of @Reiners14).

![image](DensityCase2.pdf){width="43.00000%"} ![image](DensityCase14.pdf){width="43.00000%"} ![image](MolAtomCase2.pdf){width="43.00000%"} ![image](MolAtomCase14.pdf){width="43.00000%"} ![image](HDOCase2.pdf){width="43.00000%"} ![image](HDOCase14.pdf){width="43.00000%"}

In Fig. \[fig:hydrogrid\], the vertical structures of the gas temperature, outflow speed, and ionization fraction are shown for several of the cases calculated. In all cases, the absorption of the stellar XUV spectrum heats the gas to very large temperatures, causing the atmosphere to flow away from the planet hydrodynamically in the form of a transonic wind. At altitudes of $\sim$5000-20,000 km, the outflow speeds exceeds the escape velocity; this point is also the sonic point as required in a thermal pressure driven Parker wind and is marked by the crosses in Fig. \[fig:hydrogrid\]. In no case is the exobase found within the simulation domain.

The dependence on the input X-ray flux of the maximum gas temperature, the sonic point altitude, and the maximum ionization fraction are shown in Fig. \[fig:hydrogridFx\]. In the higher activity cases, the atmospheres are heated to higher temperatures, accelerated to 