Abstract:In this paper, we show how to carry out a relatively more realistic and complete reconstruction of supernova neutrino spectra in the future large liquid-scintillator detectors, by implementing the method of singular value decomposition with a proper regularization. For a core-collapse supernova at a distance of 10 kpc in the Milky Way, itsν e spectrum can be precisely determined from the inverse beta-decay processν e þ p → e þ þ n, for which a 20 kiloton liquid-scintillator detector with the resolution similar… Show more
“…In this paper, we have improved the previous study in Ref. [34] in several important aspects. First, while the SN ν e energy spectrum can be precisely determined via the IBD data, the energy spectrum of ν e cannot be accurately extracted from the eES data.…”
Section: Introductionmentioning
confidence: 66%
“…The neutrino event rates in these channels for a JUNO-like detector have been calculated in Ref. [34] and will be recapped below for completeness.…”
Section: Supernova Neutrino Eventsmentioning
confidence: 99%
“…In Ref [34], the SN neutrino events of IBD, pES and eES channels have been simulated for The IBD channel is the golden channel for SN neutrino detection in LS detectors due to the time coincidence of the prompt and slow signals and the large cross section of the IBD reaction [38,39]. This channel is solely sensitive to ν e .…”
Section: B Sn Neutrino Eventsmentioning
confidence: 99%
“…In the previous work [34], we have already shown that it is possible to accomplish a complete reconstruction of the energy spectra of SN neutrinos ν e , ν e and ν x in a single large LS detector. One salient feature of the LS detector is its low energy threshold, which renders it capable of observing the recoiled protons resulting from the pES process that is mainly sensitive to SN ν x .…”
Section: Introductionmentioning
confidence: 99%
“…In Ref. [34], it has been assumed that ν e dominates over all other flavors in the eES channel and the detector response matrix between the initial neutrino energy and the observed event energy is approximately taken to be universal for all neutrinos. In the present work, this assumption is relaxed and the full detector response matrix will be implemented.…”
The model-independent reconstruction of the energy spectra of ν e , ν e and ν x (i.e., ν µ , ν τ 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 liquidscintillator detector (e.g., JUNO), namely, the inverse beta decay ν e + p → e + + n, the elastic neutrino-proton scattering ν+p → ν+p and the elastic neutrino-electron scattering ν+e − → ν+e − , and reconstruct the energy spectra of ν e , ν e and ν 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.
“…In this paper, we have improved the previous study in Ref. [34] in several important aspects. First, while the SN ν e energy spectrum can be precisely determined via the IBD data, the energy spectrum of ν e cannot be accurately extracted from the eES data.…”
Section: Introductionmentioning
confidence: 66%
“…The neutrino event rates in these channels for a JUNO-like detector have been calculated in Ref. [34] and will be recapped below for completeness.…”
Section: Supernova Neutrino Eventsmentioning
confidence: 99%
“…In Ref [34], the SN neutrino events of IBD, pES and eES channels have been simulated for The IBD channel is the golden channel for SN neutrino detection in LS detectors due to the time coincidence of the prompt and slow signals and the large cross section of the IBD reaction [38,39]. This channel is solely sensitive to ν e .…”
Section: B Sn Neutrino Eventsmentioning
confidence: 99%
“…In the previous work [34], we have already shown that it is possible to accomplish a complete reconstruction of the energy spectra of SN neutrinos ν e , ν e and ν x in a single large LS detector. One salient feature of the LS detector is its low energy threshold, which renders it capable of observing the recoiled protons resulting from the pES process that is mainly sensitive to SN ν x .…”
Section: Introductionmentioning
confidence: 99%
“…In Ref. [34], it has been assumed that ν e dominates over all other flavors in the eES channel and the detector response matrix between the initial neutrino energy and the observed event energy is approximately taken to be universal for all neutrinos. In the present work, this assumption is relaxed and the full detector response matrix will be implemented.…”
The model-independent reconstruction of the energy spectra of ν e , ν e and ν x (i.e., ν µ , ν τ 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 liquidscintillator detector (e.g., JUNO), namely, the inverse beta decay ν e + p → e + + n, the elastic neutrino-proton scattering ν+p → ν+p and the elastic neutrino-electron scattering ν+e − → ν+e − , and reconstruct the energy spectra of ν e , ν e and ν 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.
The deoximation of a wide range of ketoximes and aldoximes to their corresponding carbonyl compounds with high yields has been achieved using graphene oxide (GO) and sodium nitrite (NaNO2) as highly efficient catalysts and air as the green oxidant under mild conditions. The mechanism of deprotection and recycling use of catalyst were revealed in deep experiment. The carboxylic acid groups on the GO were essential for high catalytic activity.
Nuclear astrophysics is an interdisciplinary research field of nuclear physics and astrophysics, seeking for the answer to a question, how to understand the evolution of the universe with the nuclear processes which we learn. We review the research activities of nuclear astrophysics in east and southeast Asia which includes astronomy, experimental and theoretical nuclear physics, and astrophysics. Several hot topics such as the Li problems, critical nuclear reactions and properties in stars, properties of dense matter, r-process nucleosynthesis, and ν-process nucleosynthesis are chosen and discussed in further details. Some future Asian facilities, together with physics perspectives, are introduced.
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