  We calculate the energy-differential rate for neutrino emission from
electron-nucleus bremsstrahlung in stellar interiors taking into account the
effects of electron screening and ionic correlations. We compare the
energy-differential and the net rates, as well as the average $\bar{\nu}_e$ and
$\bar{\nu}_x$ $(x = {\mu}, {\tau})$ energies, for this process with those for
$e^{\pm}$ pair annihilation, plasmon decay, and photo-neutrino emission over a
wide range of temperature and density. We also compare our updated energy loss
rates for the above thermal neutrino emission processes with the fitting
formulas widely used in stellar evolution models and determine the temperature
and density domain in which each process dominates. We discuss the implications
of our results for detection of $\bar{\nu}_e$ from massive stars during their
pre-supernova evolution and find that pair annihilation makes the predominant
contribution to the signal from the thermal emission processes.
