Abstract
The model-independent reconstruction of the energy spectra of $\overline{\nu}^{}_e$, $\nu^{}_e$ and $\nu^{}_x$ (i.e., $\nu^{}_\mu$, $\nu^{}_\tau$ and their antiparticles) from the future observation of a galactic core-collapse supernova (SN) is of crucial importance to understand the microscopic physics of SN explosions. To this end, we propose a practically useful method to combine the multi-channel detection of SN neutrinos in a large liquid-scintillator detector (e.g., JUNO), namely, the inverse beta decay $\overline{\nu}^{}_e + p \to e^+ + n$, the elastic neutrino-proton scattering $\nu + p \to \nu + p$ and the elastic neutrino-electron scattering $\nu + e^- \to \nu + e^-$, and reconstruct the energy spectra of $\overline{\nu}^{}_e$, $\nu^{}_e$ and $\nu^{}_x$ by making the best use of the observational data in those three channels. In addition, the neutrino energy spectra from the numerical simulations of the delayed neutrino-driven SN explosions are implemented to demonstrate the robustness of our method. Taking the ordinary matter effects into account, we also show how to extract the initial neutrino energy spectra in the presence of neutrino flavor conversions.
Highlights
Two dozen neutrino events from supernova (SN) 1987A, as observed by Kamiokande-II [1], Irvine-MichiganBrookhaven [2], and Baskan [3], have essentially confirmed the basic idea of the delayed neutrino-driven explosion mechanism for core-collapse SNe [4,5,6,7,8]
We propose a practically useful method to combine the multichannel detection of SN neutrinos in a large liquid-scintillator detector (e.g., JUNO), namely, the inverse beta decay νe þ p → eþ þ n, the elastic neutrino-proton scattering ν þ p → ν þ p and the elastic neutrino-electron scattering ν þ e− → ν þ e−, and reconstruct the energy spectra of νe, νe, and νx by making the best use of the observational data in those three channels
We focus on the time-integrated SN neutrino energy spectra and their reconstruction from simulated experimental data
Summary
Two dozen neutrino events from supernova (SN) 1987A, as observed by Kamiokande-II [1], Irvine-MichiganBrookhaven [2], and Baskan [3], have essentially confirmed the basic idea of the delayed neutrino-driven explosion mechanism for core-collapse SNe [4,5,6,7,8]. The central idea of our reconstruction method is to treat νe, νe, and νx energy spectra on the same footing in all three reaction channels, and build the overall detector response matrix according to their individual interactions with the target particles in the LS. We stress that such a model-independent approach is applicable to solar neutrinos (with two flavors νe and νμ=τ) and ultrahigh-energy cosmic neutrinos (with three flavors νe=νe, νμ=νμ, and ντ=ντ), when the statistics is sufficiently large in the relevant next-generation experiments.
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