Abstract
Abstract We report the result of a search for neutrinos in coincidence with solar flares from the GOES flare database. The search was performed on a 10.8 kton-year exposure of KamLAND collected from 2002 to 2019. This large exposure allows us to explore previously unconstrained parameter space for solar flare neutrinos. We found no statistical excess of neutrinos and established 90% confidence level upper limits of 8.4 × 107 cm−2 (3.0 × 109 cm−2) on the electron antineutrino (electron neutrino) fluence at 20 MeV normalized to the X12 flare, assuming that the neutrino fluence is proportional to the X-ray intensity.
Highlights
Solar flares are the largest explosions in the solar system, releasing energy between 1028–1033 erg in only tens of minutes (Schrijver et al 2012)
We present a search for solar flare neutrinos using the KamLAND data taken from 2002 March to 2019 September, which includes Solar cycle 23 and 24
Tmax 0 σ(Eν, Ee)dEe for the ES studies, where Ne is the number of electrons in the 6 m-radius spherical volume: 2.4 × 1032, Ee is the kinetic energy of recoil electron, σ(Eν, Ee) is the cross section of electron scattering with the incident neutrino of energy Eν, and Tmax is the maximum Ee
Summary
Solar flares are the largest explosions in the solar system, releasing energy between 1028–1033 erg in only tens of minutes (Schrijver et al 2012). In the standard flare model, solar flares accelerate protons up to about 200 GeV and nuclear reactions of accelerated protons generate pions in the solar atmosphere Decay of these pions produce high energy (>50 MeV) γ-rays and neutrinos. IceCUBE reported the first search for GeV-scale neutrinos related to intense γ-ray solar flares and constrained some of the parameter space associated with theoretical predictions for the neutrino flux (Abbasi et al 2021). With the assumption that the fluence of solar flare neutrinos is proportional to the flare X-ray peak flux, the statistics of this search is about 1.7 times larger than previous studies (Agostini et al 2021); this assumption allows straightforward direct comparison of our result to results from other experiments and theoretical predictions
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