  We present a coupled 3-D atmospheric dynamics and radiative transfer model to
predict the disk-integrated thermal emission spectra of transiting exoplanets
in edge-on orbits. We calculate spectra at high resolution to examine the
extent to which high-resolution emission spectra are influenced by 3-D
atmospheric dynamics and planetary rotation, and to determine whether and how
we can constrain thermal structures and atmospheric dynamics through
high-resolution spectroscopy. This study represents the first time that the
line-of-sight geometry and resulting Doppler shifts from winds and rotation
have been treated self-consistently in an emission spectrum radiative transfer
model, which allow us to assess the impact of the velocity field on thermal
emission spectra. We apply our model to predict emission spectra as a function
of orbital phase for three hot Jupiters, HD 209458b, WASP-43b and HD 189733b.
We find net Doppler shifts in modeled spectra due to a combination of winds and
rotation at a level of 1-3 km/s. These Doppler signatures vary in a
quasi-sinusoidal pattern over the course of the planets' orbits as the hot
spots approach and recede from the observer's viewpoint. We predict that
WASP-43b produces the largest Doppler shift due to its fast rotation rate. We
find that the net Doppler shift in an exoplanet's disk-integrated thermal
emission spectrum results from a complex combination of winds, rotation, and
thermal structure. However, we offer a simple method that estimates the
magnitude of equatorial wind speeds in hot Jupiters through measurements of net
Doppler shifts and lower resolution thermal phase curves.
