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Pressure-induced Metal-insulator Transition of the Mott Insulator Ba2IrO4
Daisuke Orii,Masafumi Sakata,Atsushi Miyake,Katsuya Shimizu,Hirotaka Okabe,Masaaki Isobe,Eiji Takayama-Muromachi,Jun Akimitsu 한국물리학회 2013 THE JOURNAL OF THE KOREAN PHYSICAL SOCIETY Vol.63 No.3
The electrical resistivity of single crystals of the spin-orbit Mott insulator Ba2IrO4 has beenmeasured at pressures up to 30 GPa and at temperatures from 100 mK to 300 K. Ba2IrO4 showsa metal-insulator transition at around Pc = 24 GPa, though it does not show superconductivitydown to 100 mK. The low-temperature resistivity in the metallic state does not obey a conventionalFermi-liquid description. This suggests that carriers are incoherently scattered by antiferromagneticquantum spin fluctuations. The critical exponent for the metal-insulator transition is about 1.6,indicating that Ba2IrO4 is located near the boundary between a Mott and an Anderson insulator. This means that even in a single crystal, the effect of crystallographic disorder should not be ignored.
Image Enlargement with Back Projection of Lost High-frequency Components
Hideaki Kawano,Hideaki Orii,Hiroshi Maeda,Hiromi Fukushima,Norikazu Ikoma 제어로봇시스템학회 2009 제어로봇시스템학회 국제학술대회 논문집 Vol.2009 No.8
In this paper, in order to realize the image enlargement with high performance, we propose a new enlargement method, which restores high-frequency components lost in the interpolation-based methods, by using high-frequency esti-mation. The estimation is based on the eigenspace method proposed by Amano et al..The proposed enlargement method can generate lost high-frequency components by using pairs of low-and high-frequency components of the original image, and is referred as back projection for lost high-frequency components (BPLHF). Experimental results show the proposed method can achieve promising enlargement.
Horie, Takeo,Nakagawa, Masashi,Orii, Hidefumi,Tsuda, Motoyuki Korean Society of Photoscience 2002 Journal of Photosciences Vol.9 No.2
The anterior brain vesicle of ascidian larvae contains two distinct pigment cells. Ultrastructure of these pigment cells has been shown that the anterior pigment cell is an otolith for perception of gravity and the posterior pigment cell is an ocellus for light reception. The larva has remarkably simple central nervous system (CNS) composed of about 330 cells. We focused to study neural networks of visual systems. In the present paper, we report the whole structure of the photoreceptors of the ascidian larva visualized by an antibody against arrestin. Visual arrestin is the key protein for the termination of phototransduction and one of the abundant proteins in photoreceptors. Recently, we cloned an arrestin homologue gene, Ci-arr and the expression of Ci-arr was found to be restricted to the photoreceptors in the ocellus. To study the whole structure of the photoreceptors in the larva, we prepared an antibody against Ci-Arr. It is found that anti Ci-Arr antibody specifically stains the photoreceptors, including the cell bodies, the axons, and the nerve terminals. The photoreceptor cell bodies lies in row outside the pigment cup which penetrate the pigment cell and is continuous with the outer segments of the photoreceptor cell, inside the concavity of the pigments. The axons form bundle into a single tract. The tract extends toward the midline, where the nerve terminals diverge and seem to form synapses
Search for dinucleon decay into pions at Super-Kamiokande
Gustafson, J.,Abe, K.,Haga, Y.,Hayato, Y.,Ikeda, M.,Iyogi, K.,Kameda, J.,Kishimoto, Y.,Miura, M.,Moriyama, S.,Nakahata, M.,Nakajima, T.,Nakano, Y.,Nakayama, S.,Orii, A.,Sekiya, H.,Shiozawa, M.,Takeda, American Physical Society 2015 PHYSICAL REVIEW D - Vol.91 No.7
Richard, E.,Okumura, K.,Abe, K.,Haga, Y.,Hayato, Y.,Ikeda, M.,Iyogi, K.,Kameda, J.,Kishimoto, Y.,Miura, M.,Moriyama, S.,Nakahata, M.,Nakajima, T.,Nakano, Y.,Nakayama, S.,Orii, A.,Sekiya, H.,Shiozawa, American Physical Society 2016 Physical Review D Vol.94 No.5
<P>A comprehensive study of the atmospheric neutrino flux in the energy region from sub-GeV up to several TeV using the Super-Kamiokande (SK) water Cherenkov detector is presented in this paper. The energy and azimuthal spectra, and variation over time, of the atmospheric nu(e) + (nu) over bar (e) and nu(mu) + (nu) over bar (mu) fluxes are measured. The energy spectra are obtained using an iterative unfolding method by combining various event topologies with differing energy responses. The azimuthal spectra depending on energy and zenith angle, and their modulation by geomagnetic effects, are also studied. A predicted east-west asymmetry is observed in both the nu(e) and nu(mu) samples at 8.0 sigma and 6.0 sigma significance, respectively, and an indication that the asymmetry dipole angle changes depending on the zenith angle was seen at the 2.2 sigma level. The measured energy and azimuthal spectra are consistent with the current flux models within the estimated systematic uncertainties. A study of the long-term correlation between the atmospheric neutrino flux and the solar magnetic activity cycle is performed, and a weak preference for a correlation was seen at the 1.1 sigma level, using SK-I-SK-IV data spanning a 20-year period. For several particularly strong solar activity periods, corresponding to Forbush decrease events, no theoretical prediction is available but a deviation below the typical neutrino event rate is seen at the 2.4 sigma level. The seasonal modulation of the neutrino flux is also examined, but the change in flux at the SK site is predicted to be negligible, and, as expected, no evidence for a seasonal correlation is seen.</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>
Abe, K.,Haga, Y.,Hayato, Y.,Ikeda, M.,Iyogi, K.,Kameda, J.,Kishimoto, Y.,Miura, M.,Moriyama, S.,Nakahata, M.,Nakajima, T.,Nakano, Y.,Nakayama, S.,Orii, A.,Sekiya, H.,Shiozawa, M.,Takeda, A.,Tanaka, H. American Physical Society 2017 Physical Review D Vol.95 No.1
<P>We have searched for proton decay via p -> e(+) pi(0) and p -> mu(+) pi(0) using Super-Kamiokande data from April 1996 to March 2015, 0.306 megaton center dot years exposure in total. The atmospheric neutrino background rate in Super-Kamiokande IV is reduced to almost half that of phase I-III by tagging neutrons associated with neutrino interactions. The reach of the proton lifetime is further enhanced by introducing new signal criteria that select the decay of a proton in a hydrogen atom. No candidates were seen in the p -> e(+) pi(0) search. Two candidates that passed all of the selection criteria for p -> mu(+) pi(0) have been observed, but these are consistent with the expected number of background events of 0.87. Lower limits on the proton lifetime are set at tau/B(p -> mu(+) pi(0)) > 1.6 x 10(34) years and tau/B(p -> mu(+) pi(0) ) > 7.7 x 10(33) years at 90% confidence level.</P>