Institution
Tokyo Institute of Technology
Education•Tokyo, Tôkyô, Japan•
About: Tokyo Institute of Technology is a education organization based out in Tokyo, Tôkyô, Japan. It is known for research contribution in the topics: Catalysis & Thin film. The organization has 46775 authors who have published 101656 publications receiving 2357893 citations. The organization is also known as: Tokyo Tech & Tokodai.
Topics: Catalysis, Thin film, Laser, Phase (matter), Polymerization
Papers published on a yearly basis
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National Institutes of Natural Sciences, Japan1, Tokyo Institute of Technology2, Osaka University3, Max Planck Society4, Goddard Space Flight Center5, University of Hawaii at Hilo6, Kanagawa University7, Nagoya University8, Princeton University9, Ibaraki University10, Academia Sinica Institute of Astronomy and Astrophysics11, Institute for the Physics and Mathematics of the Universe12, University of Washington13, University of Toronto14, College of Charleston15, Graduate University for Advanced Studies16, Spanish National Research Council17, Hokkaido University18, Tohoku University19
TL;DR: In this article, high-resolution 1.6 μm polarized intensity (PI) images of the circumstellar disk around the Herbig Ae star AB Aur at a radial distance of 22 AU (015) up to 554 AU (385) were obtained by the high-contrast instrument HiCIAO with the dual-beam polarimetry.
Abstract: We report high-resolution 1.6 μm polarized intensity (PI) images of the circumstellar disk around the Herbig Ae star AB Aur at a radial distance of 22 AU (015) up to 554 AU (385), which have been obtained by the high-contrast instrument HiCIAO with the dual-beam polarimetry. We revealed complicated and asymmetrical structures in the inner part (140 AU) of the disk while confirming the previously reported outer (r 200 AU) spiral structure. We have imaged a double ring structure at ~40 and ~100 AU and a ring-like gap between the two. We found a significant discrepancy of inclination angles between two rings, which may indicate that the disk of AB Aur is warped. Furthermore, we found seven dips (the typical size is ~45 AU or less) within two rings, as well as three prominent PI peaks at ~40 AU. The observed structures, including a bumpy double ring, a ring-like gap, and a warped disk in the innermost regions, provide essential information for understanding the formation mechanism of recently detected wide-orbit (r > 20 AU) planets.
288 citations
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TL;DR: In this paper, an analytical method is presented which enables the crater and flank wear of tungsten carbide tools to be predicted for a wide variety of tool shapes and cutting conditions in practical turning operations based on orthogonal cutting data from machining and two wear characteristic constants.
288 citations
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University of Tokyo1, Boston University2, Brookhaven National Laboratory3, University of California, Irvine4, California State University5, George Mason University6, Gifu University7, University of Hawaii at Manoa8, Kobe University9, Los Alamos National Laboratory10, Louisiana State University11, University of Maryland, College Park12, University of Chicago13, Stony Brook University14, Niigata University15, Osaka University16, Seoul National University17, Tohoku University18, Tokai University19, Tokyo Institute of Technology20, University of Warsaw21, University of Washington22, Stanford University23
TL;DR: In this article, a search for day-night variations in the solar neutrino flux resulting from neutrinos oscillations has been carried out using the 504 day sample of solar NE data obtained at Super-Kamiokande.
Abstract: A search for day-night variations in the solar neutrino flux resulting from neutrino oscillations has been carried out using the 504 day sample of solar neutrino data obtained at Super-Kamiokande. The absence of a significant day-night variation has set an absolute flux independent exclusion region in the two neutrino oscillation parameter space.
287 citations
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TL;DR: In this paper, it was shown that the polarization of the chemical bonds at metal semiconductor interfaces could quantitatively explain the experimentally observed strength of Fermi level pinning on different semiconductors, without regard to the actual distribution of gap states.
Abstract: The insensitivity of experimentally observed Schottky barrier height (SBH) to the metal work function, a phenomenon known as Fermi level pinning, has traditionally been attributed to the presence of interface states in the band gap of the semiconductor. A recent theory showed that the polarization of the chemical bonds at metal semiconductor interfaces could quantitatively account for the experimentally observed strength of Fermi level pinning on different semiconductors, without regard to the actual distribution of gap states. This bond polarization theory thus provides a coherent explanation of the Fermi level pinning effect, on the one hand, and the experimentally observed dependence of the SBH on interface structure, on the other hand. The method used in this theory, the electrochemical potential equalization method hitherto employed only in molecular physics, and its limitations are here discussed in detail, especially in the context of application to solid interfaces. Similarities and differences between this theory and the metal induced gap state theory are also discussed.
287 citations
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TL;DR: In this paper, the authors report on γ-ray observations of the Crab Pulsar and Nebula using 8 months of survey data with the Fermi Large Area Telescope (LAT).
Abstract: We report on γ -ray observations of the Crab Pulsar and Nebula using 8 months of survey data with the Fermi Large Area Telescope (LAT). The high quality light curve obtained using the ephemeris provided by the Nan¸cay and Jodrell Bank radio telescopes shows two main peaks stable in phase with energy. The first γ -ray peak leads the radio main pulse by (281 ± 12 ± 21) μs, giving new constraints on the production site of non-thermal emission in pulsar magnetospheres. The first uncertainty is due to γ -ray statistics, and the second arises from the rotation parameters. The improved sensitivity and the unprecedented statistics afforded by the LAT enable precise measurement of the Crab Pulsar spectral parameters: cut-off energy at Ec = (5.8 ± 0.5 ± 1.2) GeV, spectral index of Γ = (1.97 ± 0.02 ± 0.06) and integral photon flux above 100 MeV of (2.09 ± 0.03 ± 0.18) × 10−6 cm−2 s−1. The first errors represent the statistical error on the fit parameters, while the second ones are the systematic uncertainties. Pulsed γ -ray photons are observed up to ∼20 GeV which precludes emission near the stellar surface, below altitudes of around 4–5 stellar radii in phase intervals encompassing the two main peaks. A detailed phase-resolved spectral analysis is also performed: the hardest emission from the Crab Pulsar comes from the bridge region between the two γ -ray peaks while the softest comes from the falling edge of the second peak. The spectrum of the nebula in the energy range 100 MeV–300 GeV is well described by the sum of two power laws of indices Γsync = (3.99 ± 0.12 ± 0.08) and ΓIC = (1.64 ± 0.05 ± 0.07), corresponding to the falling edge of the synchrotron and the rising edge of the inverse Compton (IC) components, respectively. This latter, which links up naturally with the spectral data points of Cherenkov experiments, is well reproduced via IC scattering from standard magnetohydrodynamic nebula models, and does not require any additional radiation mechanism.
287 citations
Authors
Showing all 46967 results
Name | H-index | Papers | Citations |
---|---|---|---|
Matthew Meyerson | 194 | 553 | 243726 |
Yury Gogotsi | 171 | 956 | 144520 |
Masayuki Yamamoto | 171 | 1576 | 123028 |
H. Eugene Stanley | 154 | 1190 | 122321 |
Takashi Taniguchi | 152 | 2141 | 110658 |
Shu-Hong Yu | 144 | 799 | 70853 |
Kazunori Kataoka | 138 | 908 | 70412 |
Osamu Jinnouchi | 135 | 885 | 86104 |
Hector F. DeLuca | 133 | 1303 | 69395 |
Shlomo Havlin | 131 | 1013 | 83347 |
Hiroyuki Iwasaki | 131 | 1009 | 82739 |
Kazunari Domen | 130 | 908 | 77964 |
Hideo Hosono | 128 | 1549 | 100279 |
Hideyuki Okano | 128 | 1169 | 67148 |
Andreas Strasser | 128 | 509 | 66903 |