2012/03/05 by Kamiokande Collaboration, K. Ueno, K. Abe +121 · 1 citation
Engineering · Physics and Astronomy · #Neutrino #Particle accelerators and beam dynamics #Particle physics #Particle physics theoretical and experimental studies #Physics #Solar neutrino #Super-Kamiokande #Superconducting Materials and Applications #astro-ph.HE #astro-ph.SR #hep-ex
paper · pdf · doi:10.1016/j.astropartphys.2012.05.008
published as Astroparticle Physics 36 (2012) 131-136 · 15 pages, 6 figures
arxiv created 2012/03/05 · openalex publication_date 2012/06/02 · arxiv updated 2012/11/05 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
GUT monopoles captured by the Sun's gravitation are expected to catalyze proton decays via the Callan-Rubakov process. In this scenario, protons, which initially decay into pions, will ultimately produce νe, νμ and νμ. After undergoing neutrino oscillation, all neutrino species appear when they arrive at the Earth, and can be detected by a 50,000 metric ton water Cherenkov detector, Super-Kamiokande (SK). A search for low energy neutrinos in the electron total energy range from 19 to 55 MeV was carried out with SK and gives a monopole flux limit of FM(σ0/1 mb) < 6.3 × 10-24 (βM/10-3)2 cm-2 s-1 sr-1 at 90% C.L., where βM is the monopole velocity in units of the speed of light and σ0 is the catalysis cross section at βM=1. The obtained limit is more than eight orders of magnitude more stringent than the current best cosmic-ray supermassive monopole flux limit, FM < 1 × 10-15 cm-2 s-1 sr-1 for βM < 10-3 and also two orders of magnitude lower than the result of the Kamiokande experiment, which used a similar detection method.