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tokens: brackets refer to the inverted mass hierarchy. Different columns give the numbers for different detection channels: the superscripts CC and el refer, respectively, to the dominant charged current process (inverse beta decay or absorption on the Ar nucleus) and to neutrino-electron scattering. The subscript β indicates the contribution of the β processes to those two channels. The total number of events is given in the last column. The results for Betelgeuse ( D = 0.2 kpc) can be obtained by rescaling by a factor of 25. Table 4 Same as Table 3 , but for the Progenitor The tables confirm that a large LS like JUNO has the best potential, due to its sensitivity at low energy, with events (depending on the type of progenitor) recorded from a star at D = 1 kpc. For these events, the contribution of the β p is at the level of 10%–30%, and is larger for the inverted mass hierarchy, for which the flux is larger; see Section 4.1 . For Betelgeuse, a spectacular signal of more than 200 events in two hours could be seen. One can define (optimistically) the horizon of the detector, D h , as the distance for which one signal event is expected. We find that JUNO has a horizon . Although it is disadvantaged by the higher energy threshold, SuperKamiokande and DUNE can observe presupernova neutrinos for the closest stars. For the most massive progenitor, SuperKamiokande could reach a horizon and record events for D = 0.2 pc. Of these, ∼10%–20% would be from β p. Looking further into the future, the larger water Cherenkov detector HyperKamiokande (Abe et al. 2011a )—with a mass 20 times the mass of SuperKamiokande—might become a reality. Assuming an identical performance as SuperKamiokande, HyperKamiokande will have a statistics of up to thousands of events, and a horizon of . 10 10 Due to its mass, HyperKamiokande will have a level of background that is ∼20 times higher than that of SuperKamiokande, and probably a higher energy threshold as well. Therefore, its performance will be worse, and the figures given here have to be taken as best case scenarios. At DUNE, a detection is possible only for the closest stars; the number of events varies between and , depending on the parameters, for . For the most optimistic scenario (the more massive progenitor and the inverted mass hierarchy), the horizon can reach . DUNE will observe a strong component due to β p, at the level of of the total signal. Therefore, in principle LAr has the best capability to probe the isotopic evolution of supernova progenitors. 5. Discussion We have presented a new calculation of the total neutrino flux from beta processes in a presupernova star, inclusive of time-dependent emissivities and neutrino energy spectra. This is part of a complete and detailed calculation of presupernova neutrino fluxes from most relevant processes—beta and thermal—done using the state-of-the-art stellar evolution code MESA. The beta neutrino flux is strongest in the channel, where it is comparable to the flux