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Search for dark matter WIMPs using upward through-going muons in Super-Kamiokande
Desai, S.,Ashie, Y.,Fukuda, S.,Fukuda, Y.,Ishihara, K.,Itow, Y.,Koshio, Y.,Minamino, A.,Miura, M.,Moriyama, S.,Nakahata, M.,Namba, T.,Nambu, R.,Obayashi, Y.,Sakurai, N.,Shiozawa, M.,Suzuki, Y.,Takeuch American Physical Society 2004 PHYSICAL REVIEW D - Vol.70 No.8
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.
Poster Session : Role of the C-terminal amino acids in β2-microglobulin amyloid formation
( J Kim ),( Motomiya Y ),( Ueda M ),( Nakamura M ),( Saito S ),( Misumi Y ),( Himeno S ),( Obayashi K ),( Shinriki S ),( Meung W ),( Sengba U ),( Kai H ),( Ando Y ) 한국생화학분자생물학회 (구 한국생화학회) 2007 생화학분자생물학회 춘계학술발표논문집 Vol.2007 No.-
Tanaka, T.,Abe, K.,Hayato, Y.,Iida, T.,Kameda, J.,Koshio, Y.,Kouzuma, Y.,Miura, M.,Moriyama, S.,Nakahata, M.,Nakayama, S.,Obayashi, Y.,Sekiya, H.,Shiozawa, M.,Suzuki, Y.,Takeda, A.,Takenaga, Y.,Ueno, IOP Publishing 2011 The Astrophysical journal Vol.742 No.2
<P>We present the result of an indirect search for high energy neutrinos from Weakly Interacting Massive Particle (WIMP) annihilation in the Sun using upward-going muon (upmu) events at Super-Kamiokande. Data sets from SKI-SKIII (3109.6 days) were used for the analysis. We looked for an excess of neutrino signal from the Sun as compared with the expected atmospheric neutrino background in three upmu categories: stopping, non-showering, and showering. No significant excess was observed. The 90% C. L. upper limits of upmu flux induced by WIMPs of 100 GeV c(-2) were 6.4 x 10(-15) cm(-2) s(-1) and 4.0 x 10(-15) cm(-2) s(-1) for the soft and hard annihilation channels, respectively. These limits correspond to upper limits of 4.5 x 10(-39) cm(-2) and 2.7 x 10(-40) cm(-2) for spin-dependent WIMP-nucleon scattering cross sections in the soft and hard annihilation channels, respectively.</P>
First study of neutron tagging with a water Cherenkov detector
The Super-Kamiokande Collaboration,Watanabe, H.,Zhang, H.,Abe, K.,Hayato, Y.,Iida, T.,Ikeda, M.,Kameda, J.,Kobayashi, K.,Koshio, Y.,Miura, M.,Moriyama, S.,Nakahata, M.,Nakayama, S.,Obayashi, Y.,Ogawa, North-Holland 2009 Astroparticle physics Vol.31 No.4
A first study of neutron tagging is conducted in Super-Kamiokande, a 50,000 ton water Cherenkov detector. The tagging efficiencies of thermal neutrons are evaluated in a 0.2% GdCl<SUB>3</SUB>-water solution and pure water. They are determined to be, respectively, 66.7% for events above 3MeV and 20% with corresponding background probabilities of 2x10<SUP>-4</SUP> and 3x10<SUP>-2</SUP>. This newly developed technique may enable water Cherenkov detectors to identify ν@?<SUB>e</SUB>'s from astrophysical sources as well as those produced by commercial reactors via the delayed coincidence scheme.
DRAG REDUCTION OF A PICKUP TRUCK BY A REAR DOWNWARD FLAP
J. HA,S. JEONG,S. OBAYASHI 한국자동차공학회 2011 International journal of automotive technology Vol.12 No.3
The drag reduction of a pickup truck by a rear flap add-on was examined through CFD simulations and wind tunnel experiments. When installed at the rear edge of the roof, the flap increased the cabin back surface pressure coefficient, causing the downwash of the bed flow to be inclined on the tailgate. Thus, the attachment of the bed flow to the tailgate was eliminated; consequently, the drag coefficient was reduced with increasing flap length and downward angle despite the enlarged reverse flow in the wake. However, the drag coefficient did not decrease any further after a specific downward angle was reached because the bed flow increased the drag force at the tailgate and the flap lowered the pressure field above the flap. To maximize the drag reduction effect, the rear downward flap should be designed to have an optimum downward angle.
SEARCH FOR ASTROPHYSICAL NEUTRINO POINT SOURCES AT SUPER-KAMIOKANDE
Thrane, E.,Abe, K.,Hayato, Y.,Iida, T.,Ikeda, M.,Kameda, J.,Kobayashi, K.,Koshio, Y.,Miura, M.,Moriyama, S.,Nakahata, M.,Nakayama, S.,Obayashi, Y.,Ogawa, H.,Sekiya, H.,Shiozawa, M.,Suzuki, Y.,Takeda, IOP Publishing 2009 The Astrophysical journal Vol.704 No.1
<P>It has been hypothesized that large fluxes of neutrinos may be created in astrophysical 'cosmic accelerators.' The primary background for a search for astrophysical neutrinos comes from atmospheric neutrinos, which do not exhibit the pointlike directional clustering that characterizes a distant astrophysical signal. We perform a search for neutrino point sources using the upward-going muon data from three phases of operation (SK-I, SK-II, and SK-III) spanning 2623 days of live time taken from 1996 April 1 to 2007 August 11. The search looks for signals from suspected galactic and extragalactic sources, transient sources, and uncataloged sources. While we find interesting signatures from two objects-RX J1713.7-3946 (97.5% CL) and GRB 991004D (95.3% CL)-these signatures lack compelling statistical significance given trial factors. We set limits on the flux and fluence of neutrino point sources above energies of 1.6 GeV.</P>