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Design and Construction of GINZA KABUKIZA
Kawamura, Hiroshi,Ishibashi, Yoji,Morofushi, Tsutomu,Saragai, Yasuyuki,Inubushi, Akira,Yasutomi, Ayako,Fuse, Naohiko,Yoshifuku, Manabu,Saitoh, Kouji Council on Tall Building and Urban Habitat Korea 2016 International journal of high-rise buildings Vol.5 No.3
This paper describes the structural solution for the design of a 29-story high-rise tower, which features a large office space above the Kabukiza Theatre. Kabuki is a type of Japanese traditional drama, and Kabukiza is the home building of Kabuki. GINZA KABUKIZA is the fifth generation of the Kabukiza Theatre, the first of which was built in 1889. In order to support 23 stories of office space above the theater - featuring a large void in plan - two 13-meter-deep mega-trusses, spanning 38.4 meters, are installed at the fifth floor of the building. Steelwork is used as a primary material for the structure above-ground, and a hybrid response control system using a buckling-restrained brace and oil damper is adopted in order to achieve a high seismic performance. This paper also describes the erection process of installing hydraulic jacks directly above the mega-truss at column bases, in order to keep the structure above the truss level during construction. The temple architecture of the previous Kabukiza is carefully restored by incorporating contemporary light-weight materials supported by steelwork.
External Noise Can Cause Complex Effective Dynamics in Pattern-Forming Systems
Yoshiki Kuramoto,Yoji Kawamura 한국물리학회 2007 THE JOURNAL OF THE KOREAN PHYSICAL SOCIETY Vol.50 No.1I
To demonstrate how nonlocally coupled oscillator systems can precisely be handled theoretically, we study a particular class of phenomena in which external noise generates complex effective dynamics in spatially uniform systems. The systems studied are large assemblies of oscillators with nonlocal coupling, and a theory is presented to explain this counter-intuitive behavior. Our theory is based on the phase reduction method, which is applied twice, i.e., firstly for eliminating all degrees of freedom other than phase and secondly for transforming a stochastic phase equation to an equation governing the order parameter phase. The validity of our theory is confirmed by a comparison with numerical simulations.m
Minamidani, Tetsuhiro,Tanaka, Takanori,Mizuno, Yoji,Mizuno, Norikazu,Kawamura, Akiko,Onishi, Toshikazu,Hasegawa, Tetsuo,Tatematsu, Ken'ichi,Takekoshi, Tatsuya,Sorai, Kazuo,Moribe, Nayuta,Torii, Kazufu American Institute of Physics 2011 The Astronomical journal Vol.141 No.3
<P>In order to precisely determine the temperature and density of molecular gas in the Large Magellanic Cloud, we made observations of the optically thin <SUP>13</SUP>CO(J = 3-2) transition using the ASTE 10 m telescope toward nine peaks where <SUP>12</SUP>CO(J = 3-2) clumps were previously detected with the same telescope. The molecular clumps include those in giant molecular cloud (GMC) Types I (with no signs of massive star formation), II (with H <SPAN CLASS='sml'>II</SPAN> regions only), and III (with H <SPAN CLASS='sml'>II</SPAN> regions and young star clusters). We detected <SUP>13</SUP>CO(J = 3-2) emission toward all the peaks and found that their intensities are 3-12 times lower than those of <SUP>12</SUP>CO(J = 3-2). We determined the intensity ratios of <SUP>12</SUP>CO(J = 3-2) to <SUP>13</SUP>CO(J = 3-2), R<SUP>12/13</SUP><SUB>3-2</SUB>, and <SUP>13</SUP>CO(J = 3-2) to <SUP>13</SUP>CO(J = 1-0), R<SUP>13</SUP><SUB>3-2/1-0</SUB>, at 45'' resolution. These ratios were used in radiative transfer calculations in order to estimate the temperature and density of the clumps. The clumps have a kinetic temperature range of T<SUB>kin</SUB> = 15-200 K and a molecular hydrogen gas density range of n(H<SUB>2</SUB>) = 8 × 10<SUP>2</SUP>-7 × 10<SUP>3</SUP> cm<SUP>–3</SUP>. We confirmed that the higher density clumps have higher kinetic temperature and that the lower density clumps have lower kinetic temperature to better accuracy than in previous work. The kinetic temperature and density increase generally from a Type I GMC to a Type III GMC. We interpret that this difference reflects an evolutionary trend of star formation in molecular clumps. The R<SUP>13</SUP><SUB>3-2/1-0</SUB> and kinetic temperature of the clumps are well correlated with the Hα flux, suggesting that the heating of molecular gas with density n(H<SUB>2</SUB>) = 10<SUP>3</SUP>-10<SUP>4</SUP> cm<SUP>–3</SUP> can be explained by stellar far-ultravoilet photons.</P>