  We study how better resolving the cooling length of galactic outflows affect
their energetics. We perform radiative-hydrodynamical galaxy formation
simulations of an isolated dwarf galaxy ($M_{\star}=10^{8}\, \mathrm{M}_\odot$)
with the Ramses-RTZ code, accounting for non-equilibrium cooling and chemistry
coupled to radiative transfer. Our simulations reach a spatial resolution of
$18 \, \mathrm{pc}$ in the interstellar medium (ISM) using a traditional
quasi-Lagrangian scheme. We further implement a new adaptive mesh refinement
(AMR) strategy to resolve the local gas cooling length, allowing us to
gradually increase the resolution in the stellar-feedback-powered outflows,
from $\geq 200 \, \mathrm{pc}$ to $18 \, \mathrm{pc}$. The propagation of
outflows into the inner circumgalactic medium (CGM) is significantly modified
by this additional resolution, but the ISM, star formation and feedback remain
by and large the same. With increasing resolution in the diffuse gas, the hot
outflowing phase ($T > 8 \times 10^{4} \, \mathrm{K}$) systematically reaches
overall higher temperatures and stays hotter for longer as it propagates
outwards. This leads to two-fold increases in the time-averaged mass and metal
outflow loading factors away from the galaxy ($r=5\, \mathrm{kpc}$), a
five-fold increase in the average energy loading factor, and a $\approx$50 per
cent increase in the number of sightlines with $N_{\text{OVI}} \geq 10^{13}\,
\mathrm{cm}^{-2}$. Such a significant boost to the energetics of outflows
without new feedback mechanisms or channels strongly motivates future studies
quantifying the efficiency with which better-resolved multiphase outflows
regulate galactic star formation in a cosmological context.
