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Modeling for the Performance Analysis of a Tubular SOFC/MGT Hybrid Power System
T. W. Song(송태원),J. L. Sohn(손정락),J. H. Kim(김재환),T. S. Kim(김동섭),S. T. Ro(노승탁),K. Suzuki 대한기계학회 2004 대한기계학회 춘추학술대회 Vol.2004 No.4
Performance of a solid oxide fuel cell (SOFC) can be enhanced by converting thermal energy of its high temperature exhaust gas to mechanical power using a micro gas turbine (MGT). A MGT plays also an important role to pressurize and warm up inlet gas streams of the SOFC. In this study, the influence of performance characteristics of the tubular SOFC on the hybrid power system is discussed. For this purpose, detailed heat and mass transfer with reforming and electrochemical reactions in the SOFC are mathematically modeled, and their results are reflected to the performance analysis. The analysis target is 220kWe SOFC/MGT hybrid system based on the tubular SOFC developed by Siemens-Westinghouse. Special attention is paid to the ohmic losses in the tubular SOFC counting not only current flow in radial direction, but also current flow in circumferential direction through the anode and cathode.
ANGULAR CLUSTERING OF FIR-SELECTED GALAXIES IN THE AKARI ALL-SKY SURVEY
Pollo, A.,Takeuchi, T.T.,Suzuki, T.L.,Oyabu, S. The Korean Astronomical Society 2012 天文學論叢 Vol.27 No.4
We present the first measurement of the angular two-point correlation function for AKARI $90{\mu}m$ point sources, detected outside of the Milky Way plane and selected as candidates for extragalactic sources. This is the first measurement of the large-scale angular clustering of galaxies selected in the far-infrared after IRAS. We find a positive clustering signal in both hemispheres extending up to ~ 40 degrees, without any significant fluctuations at larger scales. The observed correlation function is well fitted by a power law function. However, southern galaxies seem to be more strongly clustered than northern ones and the difference is statistically significant. The reason for this difference - technical or physical - is still to be found.
Simulation of a Polarimeter for a Spin - Polarized Positron Beam
J. H. Kim,F. Saito,N. Suzuki,L. Wei,Y. Nagashima,T. Kurihara,A. Goto,Y. Itoh,Y. S. Lee,T. Hyodo 한국진공학회(ASCT) 2002 Journal of Korean Vacuum Science & Technology Vol.6 No.3
A performance of a new positron polarimeter is investigated by simulation using a charged-particle trajectory program. The results of the ray tracing are presented along with the details of the design parameters and projected system performance. A ray tracing analysis indicates that this design is capable of effectively transmitting positrons at beam energies varying from 0.1 to 30 keV within the beam diameter of 2-6 ㎜. However, the observed reflection of the positrons(1ower than 2 keV) at 12 kGauss indicated that further refinement of beam design is needed to produce a better positron polarimeter.
REVISITING THE MICROLENSING EVENT OGLE 2012-BLG-0026: A SOLAR MASS STAR WITH TWO COLD GIANT PLANETS
Beaulieu, J.-P.,Bennett, D. P.,Batista, V.,Fukui, A.,Marquette, J.-B.,Brillant, S.,Cole, A. A.,Rogers, L. A.,Sumi, T.,Abe, F.,Bhattacharya, A.,Koshimoto, N.,Suzuki, D.,Tristram, P. J.,Han, C.,Gould, A American Astronomical Society 2016 The Astrophysical Journal Vol.824 No.2
<P>Two cold gas giant planets orbiting a G-type main-sequence star in the galactic disk were previously discovered in the high-magnification microlensing event OGLE-2012-BLG-0026. Here, we present revised host star flux measurements and a refined model for the two-planet system using additional light curve data. We performed high angular resolution adaptive optics imaging with the Keck and Subaru telescopes at two epochs while the source star was still amplified. We detected the lens flux, H = 16.39 +/- 0.08. The lens, a disk star, is brighter than predicted from the modeling in the original study. We revisited the light curve modeling using additional photometric data from the B&C telescope in New Zealand and CTIO 1.3 m H-band light curve. We then include the Keck and Subaru adaptive optic observation constraints. The system is composed of a similar to 4-9 Gyr lens star of M-lens = 1.06 +/- 0.05 M circle dot at a distance of D-lens = 4.0 +/- 0.3 kpc, orbited by two giant planets of 0.145 +/- 0.008 M-Jup and 0.86 +/- 0.06 M-Jup, with projected separations of 4.0 +/- 0.5 au and 4.8 +/- 0.7 au, respectively. Because the lens is brighter than the source star by 16 +/- 8% in H, with no other blend within one arcsec, it will be possible to estimate its metallicity using subsequent IR spectroscopy with 8-10 m class telescopes. By adding a constraint on the metallicity it will be possible to refine the age of the system.</P>
OBSERVATIONS OF THE NEAR-INFRARED SPECTRUM OF THE ZODIACAL LIGHT WITH CIBER
Tsumura, K.,Battle, J.,Bock, J.,Cooray, A.,Hristov, V.,Keating, B.,Lee, D. H.,Levenson, L. R.,Mason, P.,Matsumoto, T.,Matsuura, S.,Nam, U. W.,Renbarger, T.,Sullivan, I.,Suzuki, K.,Wada, T.,Zemcov, M. IOP Publishing 2010 The Astrophysical journal Vol.719 No.1