On the Time Distribution of Supernova Antineutrino Flux

Vissani, Francesco; Rosso, A. Gallo

doi:10.3390/sym13101851

Cited by 4 publications

(6 citation statements)

References 103 publications

(177 reference statements)

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“…The values of M A produced by lattice QCD in the last decade, and more frequently in the last years, have generally large errors and higher values in the dipole ansatz, sometimes finding smaller values using the z-expansion, as shown in Fig 5 of [52] by RQCD collaboration, whose own result is M A = 1.02 (10) GeV versus a value in the dipole approximation of M A = 1.31 (8) GeV.…”

Section: The Axial Form Factor Gmentioning

confidence: 99%

“…• As for the future galactic supernova, Super-Kamiokande (SK) will collect more than 5000 IBD events with a mass of 32.4 kiloton and for a typical galactic distance of 10kpc (see e.g. [10]), a number that scales with the square of the distance (10/d) 2 , and therefore it can be much larger for relatively closer events. 1 JUNO also expects to see a similar number of events.…”

Section: Jhep08(2022)212mentioning

confidence: 99%

“…where N p is the number of protons, which in Super-Kamiokande is particularly large: For the efficiency (E e ) we use, based on [10], the same expression, extended to lower energies, adopted for the analysis of SN1987A to describe the response of Kamiokande-II in its entire volume [55]: The resulting energy spectrum of positrons is plotted in figure 5 together with its 1σ variation coming from the overall uncertainty on the IBD cross section which we determined as discussed in the previous sections.…”

Section: Positron Emission From Ibd Signal In Super-kamiokandementioning

confidence: 99%

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An accurate evaluation of electron (anti-)neutrino scattering on nucleons

Ricciardi

Vignaroli

Vissani

2022

J. High Energ. Phys.

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Section: The Axial Form Factor Gmentioning

confidence: 99%

Section: Jhep08(2022)212mentioning

confidence: 99%

Section: Positron Emission From Ibd Signal In Super-kamiokandementioning

confidence: 99%

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An accurate evaluation of electron (anti-)neutrino scattering on nucleons

Ricciardi

Vignaroli

Vissani

2022

J. High Energ. Phys.

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“…The values of M A produced by lattice QCD in the last decade, and more frequently in the last years, have generally large errors and higher values in the dipole ansatz, sometimes finding smaller values using the z-expansion, as shown in Fig 5 of [51] by RQCD collaboration, whose own result is M A = 1.02 (10) GeV versus a value in the dipole approximation of M A = 1.31(8) GeV.…”

Section: The Axial Form Factor G1mentioning

confidence: 99%

“…For the efficiency (E e ) we use, based on [10], the same expression, extended to lower energies, adopted for the analysis of SN1987A to describe the response of Kamiokande-II in its entire volume [54]: The resulting energy spectrum of positrons is plotted in Fig. 5 together with its 1σ variation coming from the overall uncertainty on the IBD cross section which we determined as discussed in the previous sections.…”

Section: Positron Emission From Ibd Signal In Super-kamiokandementioning

confidence: 99%

An accurate evaluation of electron (anti-)neutrino scattering on nucleons

Ricciardi,

Vignaroli,

Vissani

2022

Preprint

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We discuss as accurately as possible the cross section of quasi-elastic scattering of electron (anti-) neutrinos on nucleons, also known as inverse beta decay in the case of antineutrinos. We focus on the moderate energy range from a few MeV up to hundreds of MeV, and which includes neutrinos from reactors and supernovae. We assess the uncertainty on the cross section, which is relevant to experimental advances and increasingly large statistical samples. We estimate the effects of second-class currents, showing that they are small and negligible for current applications. INTRODUCTIONThe cross section of the process νe + p → e + + n (IBD, from inverse beta decay), which enabled the first direct observation of (anti-)neutrinos [1], is still essential today at relatively low energies for detectors that are based on water or hydrocarbons, i.e., the most commonly used detectors such as scintillators or Cherenkov light detectors.The most accurate estimates available today were described about 20 years ago by Beacom and Vogel [2] and by Strumia and Vissani [3]. In this paper, we aim to update the discussion, in consideration of some general facts: 1) the importance of the reaction itself, 2) the experimental progress of neutrino detectors, 3) the progress relating to the parameters that determine the reaction itself, 4) to quantify the role of second-class currents (SCCs) [4], previously omitted, but which has been the subject of a recent debate [5][6][7].Furthermore, there is a specific quantitative point that deserves to be highlighted: it is important to update not only the value, but also the estimate of the uncertainty on the cross section of the IBD process. Indeed, the conservative estimate of the uncertainty at low energies on this IBD cross section, obtained in [3] is 0.4 %. This corresponds to a statistical error over 60,000 events and therefore it is potentially relevant in cases where the statistical sample is quite large. There are at least two cases of this type, which concern reactor antineutrinos (with typical energies of 3 MeV and up to 10 MeV) and those from supernovae (with typical energies of 20 MeV and perhaps up to 60-70 MeV). We discuss them below:• Reactor neutrino experiment Daya Bay [8] has collected 3.5 million events already. Similar considerations apply to the other reactor experiments with very high statistics. But also the future detector JUNO [9] designed to study events from distant reactors, with a very large fiducial volume, about 20 kiloton of scintillator liquid, expects to collect 83 events/day and therefore in 6 years will amount to a total of 180000 events.• As for the future galactic supernova, Super-Kamiokande (SK) will collect more than 5000 IBD events with a mass of 32.4 kiloton and for a typical galactic distance of 10kpc (see e.g. [10]), a number that scales with the

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Tachyonic Neutrinos: From the Cosmic Rays to Extragalactic Supernovae

Ehrlich¹

2023

Preprint

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The question of whether some neutrinos are tachyons remains unresolved although various evidence from cosmic ray and other data exists that the electron neutrino has an effective $m_\nu^2\approx -0.25 eV^2,$ which would require that one or more mass states is also tachyonic. In 2013 the $3+3$ model of the neutrino masses, which includes one tachyonic mass state, was proposed based on supernova SN 1987A neutrino data. Here we update evidence for tachyonic electron neutrinos and the $3+3$ model and discuss one test which could prove conclusive. The update of earlier evidence includes many new elements, including new data which makes the earlier cosmic ray evidence more robust, new results on cosmic ray composition, the ankle of the spectrum, leptonic cosmic ray data, and the statistical significance of finding the three large neutrino masses stipulated in the $3+3$ model. Barring a galactic supernova, which occur only around twice a century, a decisive test of the $3+3$ model could involve observing an extragalactic supernova neutrino burst, that is a cluster of neutrinos in a specific time window well beyond what chance would predict. Even though existing searches for such bursts have yielded only upper limits on the extragalactic supernova frequency within a certain distance, it is shown that the choice of a one-day window for possible neutrino clusters in time might be far more sensitive. A search using a one day time window could be done using existing data, and if a signal is found it would confirm the $3+3$ model. Of course, the absence of any day-long neutrino burst would not disprove the model, since it could mean only that the nearest supernova during the period when detectors were active was simply too far to be detected.

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On the Time Distribution of Supernova Antineutrino Flux

Cited by 4 publications

References 103 publications

An accurate evaluation of electron (anti-)neutrino scattering on nucleons

An accurate evaluation of electron (anti-)neutrino scattering on nucleons

An accurate evaluation of electron (anti-)neutrino scattering on nucleons

Tachyonic Neutrinos: From the Cosmic Rays to Extragalactic Supernovae

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