  Applying TQRPA calculations of Gamow--Teller strength functions in hot
nuclei, we compute the (anti)neutrino spectra and energy loss rates arising
from weak processes on hot $^{56}$Fe under pre-supernova conditions. We use a
realistic pre-supernova model calculated by the stellar evolution code MESA.
Taking into account both charged and neutral current processes, we demonstrate
that weak reactions with hot nuclei can produce high-energy (anti)neutrinos. We
also show that, for hot nuclei, the energy loss via (anti)neutrino emission is
significantly larger than that for nuclei in their ground state. It is found
that the neutral current de-excitation via the $\nu\bar\nu$-pair emission is
presumably a dominant source of antineutrinos. In accordance with other
studies, we confirm that the so-called single-state approximation for neutrino
spectra might fail under certain pre-supernova conditions. }
