High-resolution spectrographs on large ground-based telescopes have significant scientific potential for the atmospheric characterization of exoplanets. However, ground-based observations are limited by the Earth's own atmospheric absorption, particularly in the near-infrared. Detrending near-infrared spectra has traditionally relied on significant changes in the Doppler shift of planetary spectral lines across observations, typically limiting the technique to close-in hot Jupiters. However, in this work, we now demonstrate the feasibility of using ground-based high-resolution transmission spectroscopy to characterize the atmospheres of temperate planets on longer-period orbits. Using simulations of a temperate sub-Neptune, we show that planetary signals in transit may indeed be recovered when the change in the planet's radial velocity is very small, if sufficient out-of-transit spectra are observed. Our work will help to inform future observing strategies for long-period transiting exoplanets, and allow us to place precise constraints on the atmospheric chemical abundances of such planets with ground-based facilities.