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We propose a new method for calculating spectra and luminosities for(anti)neutrinos produced in the pre-supernova environment by weak processeswith hot nuclei. It is based on the thermal quasiparticle random phaseapproximation (TQRPA), that allows microscopic thermodynamically consistentcalculations of the weak-interaction response of nuclei at finite temperatures.For realistic representative pre-supernova conditions from the stellarevolution code MESA, we compute (anti)neutrino luminosities and spectra arisingfrom neutral- and charged-current weak reactions with hot $^{56}$Fe and comparethem with the contribution of thermal processes. We find that the TQRPAapproach produces not only a higher total luminosity of electron neutrinos(mainly born in the electron capture reaction), compared to the standardtechnique based on the large-scale shell model (LSSM) weak-interaction rates,but also a harder neutrino spectrum. Besides, applying the TQRPA and LSSM, wefind that in the context of electron antineutrino generation, theneutral-current nuclear de-excitation (ND) process via neutrino-antineutrinopair emission is at least as important as the electron-positron pairannihilation process. We also show that flavor oscillations enhance thehigh-energy contribution of the ND process to the electron antineutrino flux.This could potentially be important for pre-supernova antineutrino registrationby the Earth's detectors.

Neutrinos from pre-supernova in the framework of TQRPA method