A5003623315- Astrophysics and Cosmic Phenomena
- Dark Matter and Cosmic Phenomena
- Gamma-ray bursts and supernovae
- Neutrino Physics Research
- Particle Detector Development and Performance
- Particle physics theoretical and experimental studies
- Radiation Detection and Scintillator Technologies
- Pulsars and Gravitational Waves Research
- Solar and Space Plasma Dynamics
- Astrophysical Phenomena and Observations
- Radiation Therapy and Dosimetry
- Atomic and Subatomic Physics Research
- Nuclear Physics and Applications
- Radio Astronomy Observations and Technology
- Luminescence Properties of Advanced Materials
- Astronomy and Astrophysical Research
- Particle Accelerators and Free-Electron Lasers
- Geophysics and Gravity Measurements
- Stellar, planetary, and galactic studies
- Astronomical Observations and Instrumentation
- Cosmology and Gravitation Theories
- Medical Imaging Techniques and Applications
- Galaxies: Formation, Evolution, Phenomena
- COVID-19 and healthcare impacts
- Gastric Cancer Management and Outcomes
Tokai University
2023-2025
Japan Surgical Society
2023-2024
Ritsumeikan University
2015-2024
The University of Tokyo
2003-2024
Kavli Institute for the Physics and Mathematics of the Universe
2022-2024
Institute for Cosmic Ray Research
2024
Louisiana State University
2017-2024
Kyoto University
1985-2024
Istituto Nazionale di Fisica Nucleare, Sezione di Pisa
2023
University of Siena
2023
The first results of the solar neutrino flux measurement from Super-Kamiokande are presented. shown here obtained data taken between 31 May 1996, and 23 June 1997. Using our recoil electrons with energies above 6.5 MeV, we infer total ${}^{8}\mathrm{B}$ neutrinos to be $2.42\ifmmode\pm\else\textpm\fi{}0.06(\mathrm{stat}{)}_{\ensuremath{-}0.07}^{+0.10}(\mathrm{syst})\ifmmode\times\else\texttimes\fi{}{10}^{6}\mathrm{cm}{}^{\ensuremath{-}2}{\mathrm{s}}^{\ensuremath{-}1}$. This result is...
Results from 1036 days of solar neutrino data accumulated in the upgraded Kamiokande detector (Kamiokande III) are presented. The $^{8}\mathrm{B}$ flux observed III is ${2.82}_{\ensuremath{-}0.24}^{+0.25}$ (stat) \ifmmode\pm\else\textpm\fi{} 0.27 (syst) \ifmmode\times\else\texttimes\fi{} ${10}^{6}$ ${\mathrm{cm}}^{\ensuremath{-}2}$${\mathrm{s}}^{\ensuremath{-}1}$; combined II and (2079 total) 2.80 0.19 0.33 ${\mathrm{cm}}^{\ensuremath{-}2}$${\mathrm{s}}^{\ensuremath{-}1}$, which 49% to 64%...
From an exposure of 25.5 kiloton-years the Super-Kamiokande detector, 900 muon-like and 983 electron-like single-ring atmospheric neutrino interactions were detected with momentum pe>100 MeV/c, pμ>200 visible energy less than 1.33 GeV. Using a detailed Monte Carlo simulation, ratio (μ/e)DATA/(μ/e)MC was measured to be 0.61±0.03(stat.)±0.05(sys.), consistent previous results from Kamiokande, IMB Soudan-2 experiments, smaller expected theoretical models production.
The flavor ratio of the atmospheric neutrino flux and its zenith angle dependence have been studied in multi-GeV energy range using an exposure 25.5 kiloton-years Super-Kamiokande detector. By comparing data to a detailed Monte Carlo simulation, (μ/e)DATA/(μ/e)MC was measured be 0.66±0.06(stat.)±0.08(sys.). In addition, strong distortion shape μ-like event distribution observed. number upward downward events found 0.52+0.07−0.06(stat.)±0.01(sys.), with expected value...
Neutrinos from the decay of $^{8}\mathrm{B}$ in Sun have been observed Kamiokande-II detector. Based on 450 days data time period January 1987 through May 1988; measured flux obtained with ${E}_{e}$\ensuremath{\ge}9.3 MeV is 0.46\ifmmode\pm\else\textpm\fi{}0.13(stat)\ifmmode\pm\else\textpm\fi{}0.08(sys) value predicted by standard solar model. Within experimental errors, agreement corresponding $^{37}\mathrm{Cl}$ radiochemical detector essentially same period.
A data sample of 1040 days from the Kamiokande II detector, consisting subsamples 450 at electron-energy threshold Ee≥9.3 MeV and 590 Ee≥7.5 MeV, yields a clear directional correlation solar-neutrino-induced electron events with respect to Sun measurement differential distribution. These provide unequivocal evidence for production B8 by fusion in Sun. The measured flux solar neutrinos two relative prediction standard model is 0.46±0.05(stat)±0.06(syst). total tested short-term time...
Extended results on the cosmic-ray electron $+$ positron spectrum from 11 GeV to 4.8 TeV are presented based observations with Calorimetric Electron Telescope (CALET) International Space Station utilizing data up November 2017. The analysis uses full detector acceptance at high energies, approximately doubling statistics compared previous result. CALET is an all-calorimetric instrument a total thickness of 30 ${X}_{0}$ normal incidence and fine imaging capability, designed achieve large...
In this paper, we present the analysis and results of a direct measurement cosmic-ray proton spectrum with CALET instrument onboard International Space Station, including detailed assessment systematic uncertainties. The observation period used in is from October 13, 2015 to August 31, 2018 (1054 days). We have achieved very wide energy range necessary carry out measurements 50 GeV 10 TeV covering, for first time space, single whole interval previously investigated most cases separate...
The method of $^{8}\mathrm{B}$ solar-neutrino measurement by means the reaction ${\ensuremath{\nu}}_{e}e\ensuremath{\rightarrow}{\ensuremath{\nu}}_{e}e$ in Kamiokande II detector is described detail. A data sample 1040 live days time period January 1987 through April 1990 yields a clear directional correlation solar-neutrino-induced electron events with respect to Sun and differential energy distribution. measured flux solar neutrinos from subsamples 450 at threshold...
This paper reports the first discovery of TeV gamma-ray emission from a supernova remnant made with CANGAROO 3.8 m Telescope. gamma rays were detected at sky position and extension coincident north-east (NE) rim shell-type Supernova (SNR) SN1006 (Type Ia). has been most likely candidate for an extended Gamma-ray source, since clear synchrotron X-ray rims was recently observed by ASCA (Koyama et al. 1995), which is strong evidence existence very high energy electrons up to hundreds in SNR....
First results of a cosmic-ray electron and positron spectrum from 10 GeV to 3 TeV is presented based upon observations with the CALET instrument on International Space Station starting in October, 2015. Nearly half million events are included analysis. an all-calorimetric total vertical thickness 30 ${X}_{0}$ fine imaging capability designed achieve large proton rejection excellent energy resolution well into region. The observed over can be fit single power law spectral index...
A precise measurement of the cosmic-ray proton spectrum with Calorimetric Electron Telescope (CALET) is presented in energy interval from 50 GeV to 60 TeV, and observation a softening above 10 TeV reported. The analysis based on data collected during ∼6.2 years smooth operations aboard International Space Station covers broader range respect previous flux by CALET, an increase available statistics factor ∼2.2. Above few hundred we confirm our progressive spectral hardening higher...
We present the results of a direct measurement cosmic-ray helium spectrum with CALET instrument in operation on International Space Station since 2015. The observation period covered by this analysis spans from October 13, 2015, to April 30, 2022 (2392 days). very wide dynamic range allowed for collection data over large energy interval, ∼40 GeV ∼250 TeV, first time single low Earth orbit. measured shows evidence deviation flux power law more than 8σ progressive spectral hardening few...
We have detected sub-TeV gamma-ray emission from the direction of Galactic center (GC) using CANGAROO-II Imaging Atmospheric Cerenkov Telescope. a statistically significant excess at energies greater than 250 GeV. The flux was 1 order magnitude lower that Crab Nebula TeV with soft spectrum proportional to E-4.6±0.5. signal centroid is consistent GC direction, and observed profile pointlike source. Our data suggest GeV source 3EG J1746-2851 identical this source, we study combined spectra...
We have searched for proton decay via p→e+π0 using data from a 25.5kton˙yr exposure of the Super-Kamiokande detector. find no candidate events with an expected background induced by atmospheric neutrinos 0.1 events. From these data, we set lower limit on partial lifetime τ/Bp→e+π0 to be 1.6×1033years at 90% confidence level.Received 19 May 1998DOI:https://doi.org/10.1103/PhysRevLett.81.3319©1998 American Physical Society
An analysis of the Mikheyev-Smirnov-Wolfenstein effect using 1040 days Kamiokande-II data is reported, which provides constraints on neutrino-oscillation parameters. The measured recoil-electron energy spectrum alone leads to conclusion that adiabatic region, 7.2\ifmmode\times\else\texttimes\fi{}${10}^{\mathrm{\ensuremath{-}}4}$${\mathrm{sin}}^{2}$2\ensuremath{\theta}6.3\ifmmode\times\else\texttimes\fi{}${10}^{\mathrm{\ensuremath{-}}3}$,...
The flux of upward through-going muons minimum (mean) threshold energy >1.6 (3.0) GeV is measured, based on a total 372 events observed by the Kamiokande II+III detector during 2456 live days. muon was Φobs=[1.94±0.10(stat.)−0.06+0.07sys.)]×10−13cm−2s−1sr−1, which compared to an expected value Φtheo=[2.46±0.54(theo.)]×10−13cm−2s−1sr−1. observation in agreement with prediction within errors. zenith-angle dependence supports previous indication neutrino oscillations made using sub- and...
Searches for possible day-night and semiannual variations of the $^{8}\mathrm{B}$ solar neutrino flux are reported based on 1040 days Kamiokande-II data. Within statistical error, no such short-time were observed. The limit difference sets a constraint neutrino-oscillation parameters. A region defined by ${\mathrm{sin}}^{2}$2\ensuremath{\theta}>0.02...
In this paper, we present the measurement of energy spectra carbon and oxygen in cosmic rays based on observations with Calorimetric Electron Telescope International Space Station from October 2015 to 2019. Analysis, including detailed assessment systematic uncertainties, results are reported. The measured kinetic per nucleon $10\text{ }\text{ }\mathrm{GeV}/n$ $2.2\text{ }\mathrm{TeV}/n$ an all-calorimetric instrument a total thickness corresponding 1.3 nuclear interaction length. observed...