## I. INTRODUCTION 

The existence of neutrinos was postulated by Pauli in 1932 in order to explain the observed continuous electron spectrum accompanying nuclear beta decay. Based on the idea of Pauli, Fermi [1, 2] proposed the beta decay theory, while Bethe and Peierls [3–5] predicted an extremely small cross-section for the interaction of neutrino with matter, and Gamow [6, 7] and Pontecorvo [8] were the first to recognize the important role played by neutrinos in the evolution of stars. The neutrino emission processes may affect the properties of matter at high temperatures, and hence affect stellar evolution. 

Neutrino emission is known to play an important role in stellar evolution, especially in the late stages when the rate of evolution is almost fully dependent on energy loss via neutrinos. This refers to the stage of steady burning prior to the implosion of the stellar core, to the process of catastrophic core-collapse, and to the cooling of the neutron star which is formed. 

The explosion energy of the core-collapse is typically 10 53 erg which makes it one of the most impressive violent events in the universe. This energy comes from the explosion of the progenitor star, and only partly manifests itself in the shock wave that is launched somewhere at the boundary between the iron core of mass M$_{F e}$ = (1 . 2 − 2) M ⊙ and the inner most regions, collapsing into a neutron star. Even when the mechanism of the core-collapse is not yet understood in great detail, the most distinctive feature is the enormous energy of (3 − 5) × 10 53 erg = (10 − 15)% M$_{F e}$c 2 radiated in the form of neutrinos and antineutrinos of all flavors ( ν$_{e}$, ν$_{µ}$, ν$_{τ}$ ) during a burst of about 10 seconds. While such neutrinos were first observed in the supernova SN1987A, various observatories running or under design, like next generation large-size detectors, could provide us with the luminosity curve from a future (extra)galactic explosion and/or the observation of relic neutrinos from past supernovae. To disentangle the information from such neutrino signals represents a challenging task, since the crucial information from the explosion phenomenon and neutrino properties such as the neutrino hierarchy and the third neutrino mixing angle are intertwined. 

The detection of neutrinos from SN1987A by the Kamiokande II [9] and Irvine-Michigan- Brookhaven [10] detectors confirmed the standard model of core-collapse (type II) super- novae [11, 12] and provided a laboratory to study the properties of neutrinos [13–18] and exotic particles such as axions [19]. The collapse of stellar iron-core into a neutron star is preceded by a high-power pulse of neutrino emission. In general, a bolometric neutrino light 

