Results 91 to 100 of about 1,298,977 (255)
Final results of Borexino Phase-I on low-energy solar neutrino spectroscopy [PDF]
, 2013 Borexino has been running since May 2007 at the Laboratori Nazionali del Gran Sasso laboratory in Italy with the primary goal of detecting solar neutrinos.
G. Bellini +88 more
semanticscholar +1 more source
The Solar Neutrino Problem [PDF]
Annual Review of Astronomy and Astrophysics, 1995 The solar neutrino problem has persisted for almost three decades. Recent results from Kamiokande, SAGE, and GALLEX indicate a pattern of neutrino fluxes that is very difficult to reconcile with plausible variations in standard solar models. This situation is reviewed, and suggested particle physics solutions are discussed.
openaire +3 more sources
Anti-Neutrino Imprint in Solar Neutrino Flare [PDF]
Phys.Scripta T127:22-24,2006, 2006 Future neutrino detector at Megaton mass might enlarge the neutrino telescope thresholds revealing cosmic supernova background and largest solar flares neutrino. Indeed the solar energetic flare particles while scattering among themselves on Solar corona atmosphere must produce prompt charged pions, whose chain decays are source of solar (electron-muon)
arxiv +1 more source
The Charged Neutrino: A New Approach to the Solar Neutrino Problem
, 1994 We have considered the effect of the reduction of the solar neutrino flux on earth due to the deflection of the charged neutrino by the magnetic field of the solar convective zone.
Ignatiev, A. Yu., Joshi, G. C.
core +2 more sources
The Simplest Resonant Spin--Flavour Solution to the Solar Neutrino Problem [PDF]
, 2000 We re-analyse the resonant spin-flavour (RSF) solutions to the solar neutrino problem in the framework of analytic solutions to the solar magneto-hydrodynamics (MHD) equations.
Akhmedov +57 more
core +2 more sources
Precision measurement of the (7)Be solar neutrino interaction rate in Borexino. [PDF]
Physical Review Letters, 2011 The rate of neutrino-electron elastic scattering interactions from 862 keV (7)Be solar neutrinos in Borexino is determined to be 46.0±1.5(stat)(-1.6)(+1.5)(syst) counts/(day·100 ton). This corresponds to a ν(e)-equivalent (7)Be solar neutrino flux of (3.
G. Bellini +88 more
semanticscholar +1 more source
Solar Neutrino Observables Sensitive to Matter Effects
Advances in High Energy Physics, 2012 We discuss constraints on the coefficient AMSW which is introduced to simulate the effect of weaker or stronger matter potential for electron neutrinos with the current and future solar neutrino data.
H. Minakata, C. Peña-Garay
doaj +1 more source
Nuclear Physics B, 2017 It was suggested that a tension between the mass-squared differences obtained from the solar neutrino and KamLAND experiments can be solved by introducing the non-standard flavor-dependent interaction in neutrino propagation. In this paper we discuss the
Shinya Fukasawa, Osamu Yasuda
doaj +1 more source
Progress in Particle and Nuclear Physics, 2023 As a free, intensive, rarely interactive and well directional messenger, solar neutrinos have been driving both solar physics and neutrino physics developments for more than half a century. Since more extensive and advanced neutrino experiments are under construction, being planned or proposed, we are striving toward an era of precise and comprehensive
Xun-Jie Xu, Zhe Wang, Shaomin Chen
openaire +2 more sources
Journal of High Energy Physics, 2022 The recent XENON1T excess can be explained by the solar active-sterile neutrino conversion with bound electrons via light mediator. Nevertheless, the atomic effects are usually omitted in the solar neutrino explanations.
Shao-Feng Ge, Pedro Pasquini, Jie Sheng
doaj +1 more source