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Search for GUT monopoles at Super-Kamiokande
The Super-Kamiokande Collaboration,Ueno, K.,Abe, K.,Hayato, Y.,Iida, T.,Iyogi, K.,Kameda, J.,Koshio, Y.,Kozuma, Y.,Miura, M.,Moriyama, S.,Nakahata, M.,Nakayama, S.,Obayashi, Y.,Sekiya, H.,Shiozawa, M. North-Holland ; Elsevier Science Ltd 2012 Astroparticle physics Vol.36 No.1
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 ν<SUB>e</SUB>,ν<SUB>μ</SUB> and ν@?<SUB>μ</SUB>. 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 55MeV was carried out with SK and gives a monopole flux limit of F<SUB>M</SUB>(σ<SUB>0</SUB>/1mb)<6.3x10<SUP>-24</SUP>(β<SUB>M</SUB>/10<SUP>-3</SUP>)<SUP>2</SUP>cm<SUP>-2</SUP>s<SUP>-1</SUP>sr<SUP>-1</SUP> at 90% C.L., where β<SUB>M</SUB> is the monopole velocity in units of the speed of light and σ<SUB>0</SUB> is the catalysis cross section at β<SUB>M</SUB>=1. The obtained limit is several orders of magnitude more stringent than the current best cosmic-ray supermassive monopole flux limit for β<SUB>M</SUB><10<SUP>-2</SUP> and also two orders of magnitude lower than the result of the Kamiokande experiment, which used a similar detection method.
Nakayama, S.,Mauger, C.,Ahn, M.H.,Aoki, S.,Ashie, Y.,Bhang, H.,Boyd, S.,Casper, D.,Choi, J.H.,Fukuda, S.,Fukuda, Y.,Gran, R.,Hara, T.,Hasegawa, M.,Hasegawa, T.,Hayashi, K.,Hayato, Y.,Hill, J.,Ichikawa Elsevier 2005 Physics letters: B Vol.619 No.3
<P><B>Abstract</B></P><P>Neutral current single <SUP>π0</SUP> production induced by neutrinos with a mean energy of 1.3 GeV is measured using a 1000 ton water Cherenkov detector in the K2K long baseline neutrino experiment. The cross section for this process relative to the total charged current cross section is measured to be 0.064±0.001(stat.)±0.007(sys.). The momentum distribution of neutral current <SUP>π0</SUP>s from a water target is measured with high statistics for the first time.</P>
Goto, M.,Karita, S.,Yahaya, M.S.,Kim, W.,Nakayama, E.,Yamada, Y. Asian Australasian Association of Animal Productio 2003 Animal Bioscience Vol.16 No.1
Effects of supplementation with ruminal epithelial cells on fiber-degrading activity and cell growth of Ruminococcus albus (R. albus, strain 7) was tested using a basal substrate of rice straw and formulated concentrate. Cultures of R. albus alone and R. albus with rumen protozoa were grown at $39^{\circ}C$ for 48 h with an 8.4% crude protein (CP) substrate, 33% of the CP supplemented with either ruminal epithelial cells or defatted soybean meal. The ruminal epithelial cells had lower amounts of rumen soluble and degradable protein fractions as compared to defatted soybean meal, as determined by an enzymatic method, and the same was found with amino acid composition of protein hydrolysates. Ruminal epithelial cells were directly utilized by the R. albus, and resulted in greater growth of cell-wall free bacteria compared to defatted soybean meal. The effect of epithelial cells on bacterial growth was enhanced by the presence of rumen protozoa. In consistency with cultures of R. albus and R. albus with rumen protozoa, fermentative parameters such as dry matter degradability and total volatile fatty acid did not differ between supplementation with ruminal epithelial cells or defatted soybean meal.
T. Ogawa,M. Nakayama,M. Haraguchi,M. Kuwahara,M. Fukui,S. Matsuo,T. Okamoto 한국물리학회 2005 THE JOURNAL OF THE KOREAN PHYSICAL SOCIETY Vol.47 No.1
We have macroscopically and microscopically investigated the localized surface plasmons (LSPs)on Ag anoparticles embedded in porous TiO2 glass. We have prepared TiO2 glass containing Ag nanoparticles (Ag/TiO2) by the sol-gel process and changed the porosity of the TiO2 glass by drying under a high vacuum condition. Using a spectrometer, we have macroscopically measured the absorption spectra (ABS) on all Ag nanoparticles and using near-field scanning optical microscopy (NSOM), we have microscopically measured the scattering spectra on a single Ag nanoparticle in the Ag/TiO2 after each drying process. Fitting the spectra derived from the numerical calculation based on the Mie theory to that evaluated from the ABS and the NSOM measurements, we have evaluated the deviation of the full width at half maximum evaluated by the experimental measurements from that derived from the theoretical calculation (FWHM) and the bound (Hashin-Shtrikman bounds) of the porosity of the TiO2 glass by the use of the Hashin Shtrikman limit, similar to the literature [1]. It has been found that the FWHM of the scattering spectra on the single Ag nanoparticle can be much smaller than one of the ABS on all Ag nanoparticles in the Ag/TiO2. This result is due to that the ABS is influenced by the aggregation and the size distribution of all Ag nanoparticles. Furthermore, on extrapolating from the plot of FWHM vs porosity, the FWHM is reduced to zero when the porosity is about 15 %.
Limits on sterile neutrino mixing using atmospheric neutrinos in Super-Kamiokande
Abe, K.,Haga, Y.,Hayato, Y.,Ikeda, M.,Iyogi, K.,Kameda, J.,Kishimoto, Y.,Miura, M.,Moriyama, S.,Nakahata, M.,Nakano, Y.,Nakayama, S.,Sekiya, H.,Shiozawa, M.,Suzuki, Y.,Takeda, A.,Tanaka, H.,Tomura, T. American Physical Society 2015 PHYSICAL REVIEW D - Vol.91 No.5
Good Scalability of Study of Spin Torque Transfer MRAMs with Perpendicular Magnetization MTJs
H. Yoda,T. Kishi,T. Nagase,M. Yoshikawa,E. Kitagawa,T. Daibou,K. Nishiyama,T. Kai,N. Shimomura,M. Nakayama,M. Amano,H. Aikawa,S. Takahashi,S. Ikegawa,M. Nagamine,J. Ozeki,S. Yuasa,Y. Nakatani,M. Oogan 한국자기학회 2008 한국자기학회 학술연구발표회 논문개요집 Vol.- No.-
Test of Lorentz invariance with atmospheric neutrinos
Abe, K.,Haga, Y.,Hayato, Y.,Ikeda, M.,Iyogi, K.,Kameda, J.,Kishimoto, Y.,Miura, M.,Moriyama, S.,Nakahata, M.,Nakano, Y.,Nakayama, S.,Sekiya, H.,Shiozawa, M.,Suzuki, Y.,Takeda, A.,Tanaka, H.,Tomura, T. American Physical Society 2015 PHYSICAL REVIEW D - Vol.91 No.5
Real-time supernova neutrino burst monitor at Super-Kamiokande
Abe, K.,Haga, Y.,Hayato, Y.,Ikeda, M.,Iyogi, K.,Kameda, J.,Kishimoto, Y.,Miura, M.,Moriyama, S.,Nakahata, M.,Nakano, Y.,Nakayama, S.,Sekiya, H.,Shiozawa, M.,Suzuki, Y.,Takeda, A.,Tanaka, H.,Tomura, T. North-Holland ; Elsevier Science Ltd 2016 Astroparticle physics Vol.81 No.-
<P>We present a real-time supernova neutrino burst monitor at Super-Kamiokande (SIC). Detecting supernova explosions by neutrinos in real time is crucial for giving a clear picture of the explosion mechanism. Since the neutrinos are expected to come earlier than light, a fast broadcasting of the detection may give astronomers a chance to make electromagnetic radiation observations of the explosions right at the onset. The role of the monitor includes a fast announcement of the neutrino burst detection to the world and a determination of the supernova direction. We present the online neutrino burst detection system and studies of the direction determination accuracy based on simulations at SK. (C) 2016 Elsevier B.V. All rights reserved.</P>
Solar neutrino measurements in Super-Kamiokande-IV
Abe, K.,Haga, Y.,Hayato, Y.,Ikeda, M.,Iyogi, K.,Kameda, J.,Kishimoto, Y.,Marti, Ll.,Miura, M.,Moriyama, S.,Nakahata, M.,Nakajima, T.,Nakayama, S.,Orii, A.,Sekiya, H.,Shiozawa, M.,Sonoda, Y.,Takeda, A. American Physical Society 2016 Physical Review D Vol.94 No.5
<P>Upgraded electronics, improved water system dynamics, better calibration and analysis techniques allowed Super-Kamiokande-IV to clearly observe very low-energy B-8 solar neutrino interactions, with recoil electron kinetic energies as low as similar to 3.5 MeV. Super-Kamiokande-IV data-taking began in September of 2008; this paper includes data until February 2014, a total livetime of 1664 days. The measured solar neutrino flux is (2.308 +/- 0.020)(stat)(-0.040)(+0.039) (syst)) x 10(6)/(cm(2) sec) assuming no oscillations. The observed recoil electron energy spectrum is consistent with no distortions due to neutrino oscillations. An extended maximum likelihood fit to the amplitude of the expected solar zenith angle variation of the neutrino-electron elastic scattering rate in SK-IV results in a day/night asymmetry of (-3.6 +/- 1.6(stat) +/- 0.6(syst)%. The SK-IV solar neutrino data determine the solar mixing angle as sin(2)theta(12) = 0.327(-0.031)(+0.026), all SK solar data (SK-I, SK-II, SK III and SK-IV) measures this angle to be sin(2)theta(12) = 0.334(-0.023)(+0.027), the determined mass-squared splitting is Delta m(21)(2) = 4.8(-0.8)(+1.5) x 10(-5) eV(2).</P>