  Galaxy evolution is regulated by the interplay between galactic disks and
their surrounding medium. We study this interplay by examining how the galactic
coronal emission efficiency of stellar feedback depends on the (surface and
specific) star formation rates (SFRs) and other parameters for a sample of 52
Chandra-observed nearby highly inclined disk galaxies. We first measure the
star forming galactic disk sizes, as well as the SFRs of these galaxies, using
data from the Wide-Field Infrared Survey Explorer, and then show that 1) the
specific 0.5-2~keV luminosity of the coronal emission correlates with the
specific SFR in a {\sl sub-linear} fashion: on average, $L_X/L_K \propto
(SFR/M_*)^{\Gamma}$ with $\Gamma =0.29\pm0.12$; 2) the efficiency of the
emission $ L_X/SFR$ decreases with increasing surface SFR ($I_{SFR}$; $\Gamma =
-0.44\pm0.12$); and 3) the characteristic temperature of the X-ray-emitting
plasma weakly correlates with $I_{SFR}$ ($\Gamma = 0.08\pm0.04$). These
results, somewhat surprising and anti-intuitive, suggest that a) the linear
correlation between $L_X$ and SFR, as commonly presented, is largely due to the
correlation of these two parameters with galaxy mass; b) much of the mechanical
energy from stellar feedback likely drives global outflows with little X-ray
cooling and with a mass-loading efficiency decreasing fast with increasing
$I_{SFR}$ ($\Gamma \lesssim -0.5$); c) these outflows heat and inflate the
medium around the galactic disks of massive galaxies, reducing its radiative
cooling rate, whereas for relatively low-mass galaxies, the energy in the
outflows is probably dissipated in regions far away from the galactic disks.
