Zobrazeno 1 - 10
of 16 965
pro vyhledávání: '"OHMORI, K."'
Autor:
Jerjes W; Research and Development Unit, Hammersmith and Fulham PCN, London, UK; Faculty of Medicine, Imperial College London, London, UK. Electronic address: waseem.jerjes@nhs.net.
Publikováno v:
Orthopaedics & traumatology, surgery & research : OTSR [Orthop Traumatol Surg Res] 2024 Nov; Vol. 110 (7), pp. 103992. Date of Electronic Publication: 2024 Sep 07.
Autor:
Bharti, V., Sugawa, S., Mizoguchi, M., Kunimi, M., Zhang, Y., de Léséleuc, S., Tomita, T., Franz, T., Weidemüller, M., Ohmori, K.
Publikováno v:
Phys. Rev. Lett. 131, 123201 (2023)
We report the observation and control of ultrafast non-equilibrium many-body electron dynamics in Rydberg-excited spatially-ordered ultracold atoms created from a three-dimensional unity-filling atomic Mott insulator. By implementing time-domain Rams
Externí odkaz:
http://arxiv.org/abs/2201.09590
Akademický článek
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Autor:
Ando Y; Department of Chemistry, Tokyo Institute of Technology present name, Institute of Science Tokyo, 2-12-1 O-okayama, Meguro-ku, Tokyo, 152-8551, Japan., Hoshino T; Department of Chemistry, Tokyo Institute of Technology present name, Institute of Science Tokyo, 2-12-1 O-okayama, Meguro-ku, Tokyo, 152-8551, Japan., Tanaka N; Department of Chemistry, Tokyo Institute of Technology present name, Institute of Science Tokyo, 2-12-1 O-okayama, Meguro-ku, Tokyo, 152-8551, Japan., Maturi MM; Department of Chemistry, Tokyo Institute of Technology present name, Institute of Science Tokyo, 2-12-1 O-okayama, Meguro-ku, Tokyo, 152-8551, Japan., Nakazawa Y; Department of Chemistry, Tokyo Institute of Technology present name, Institute of Science Tokyo, 2-12-1 O-okayama, Meguro-ku, Tokyo, 152-8551, Japan., Fukazawa T; Department of Chemistry, Tokyo Institute of Technology present name, Institute of Science Tokyo, 2-12-1 O-okayama, Meguro-ku, Tokyo, 152-8551, Japan., Ohmori K; Department of Chemistry, Tokyo Institute of Technology present name, Institute of Science Tokyo, 2-12-1 O-okayama, Meguro-ku, Tokyo, 152-8551, Japan., Suzuki K; Department of Chemistry, Tokyo Institute of Technology present name, Institute of Science Tokyo, 2-12-1 O-okayama, Meguro-ku, Tokyo, 152-8551, Japan.; The Kitasato Institute, Kitasato University, 5-9-1, Shirokane, Minato-ku, Tokyo, 108-8641, Japan.
Publikováno v:
Angewandte Chemie (International ed. in English) [Angew Chem Int Ed Engl] 2024 Oct 10, pp. e202415108. Date of Electronic Publication: 2024 Oct 10.
Akademický článek
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Autor:
Ikeda M; Institute for the Advancement of Higher Education, Hokkaido University, Sapporo, Japan., Yamazaki A; KIKAI Institute for Coral Reef Sciences, Kikai Town, Japan.; Graduate School of Environmental Studies, Nagoya University, Nagoya, Japan., Ohmori K; Hokkaido Research Organization (Environmental and Geological Research Department, Geological Survey of Hokkaido), Sapporo, Japan., Chiang HW; High-Precision Mass Spectrometry and Environment Change Laboratory (HISPEC), Department of Geosciences, National Taiwan University, Taipei, Taiwan, ROC., Shen CC; High-Precision Mass Spectrometry and Environment Change Laboratory (HISPEC), Department of Geosciences, National Taiwan University, Taipei, Taiwan, ROC.; Research Center for Future Earth, National Taiwan University, Taipei, Taiwan., Watanabe T; KIKAI Institute for Coral Reef Sciences, Kikai Town, Japan. nabe@sci.hokudai.ac.jp.; Department of Natural History Sciences, Faculty of Science, Hokkaido University, Sapporo, Japan. nabe@sci.hokudai.ac.jp.; Research Institute for Humanity and Nature, Kyoto, Japan. nabe@sci.hokudai.ac.jp.
Publikováno v:
Scientific reports [Sci Rep] 2024 Nov 20; Vol. 14 (1), pp. 28787. Date of Electronic Publication: 2024 Nov 20.
Autor:
Bachelet, E., Shin, I. -G., Han, C., Fouqué, P., Gould, A., Menzies, J. W., Beaulieu, J. -P., Bennett, D. P., Bond, I. A., Dong, Subo, Heyrovský, D., Marquette, J. B., Marshall, J., Skowron, J., Street, R. A., Sumi, T., Udalski, A., Abe, L., Agabi, K., Albrow, M. D., Allen, W., Bertin, E., Bos, M., Bramich, D. M., Chavez, J., Christie, G. W., Cole, A. A., Crouzet, N., Dieters, S., Dominik, M., Drummond, J., Greenhill, J., Guillot, T., Henderson, C. B., Hessman, F. V., Horne, K., Hundertmark, M., Johnson, J. A., Jørgensen, U. G., Kandori, R., Liebig, C., Mékarnia, D., McCormick, J., Moorhouse, D., Nagayama, T., Nataf, D., Natusch, T., Nishiyama, S., Rivet, J. -P., Sahu, K. C., Shvartzvald, Y., Thornley, G., Tomczak, A. R., Tsapras, Y., Yee, J. C., Batista, V., Bennett, C. S., Brillant, S., Caldwell, J. A. R., Cassan, A., Corrales, E., Coutures, C., Prester, D. Dominis, Donatowicz, J., Kubas, D., Martin, R., Williams, A., Zub, M., de Almeida, L. Andrade, DePoy, D. L., Gaudi, B. S., Hung, L. -W., Jablonski, F., Kaspi, S., Klein, N., Lee, C. -U., Lee, Y., Koo, J. -R., Maoz, D., Muñoz, J. A., Pogge, R. W., Polishook, D., Shporer, A., Abe, F., Botzler, C. S., Chote, P., Freeman, M., Fukui, A., Furusawa, K., Harris, P., Itow, Y., Kobara, S., Ling, C. H., Masuda, K., Matsubara, Y., Miyake, N., Ohmori, K., Ohnishi, K., Rattenbury, N. J., Saito, To., Sullivan, D. J., Suzuki, D., Sweatman, W. L., Tristram, P. J., Wada, K., Yock, P. C. M., Szymański, M. K., Soszyński, I., Kubiak, M., Poleski, R., Ulaczyk, K., Pietrzyński, G., Wyrzykowski, Ł., Kains, N., Snodgrass, C., Steele, I. A., Alsubai, K. A., Bozza, V., Browne, P., Burgdorf, M. J., Novati, S. Calchi, Dodds, P., Dreizler, S., Finet, F., Gerner, T., Hardis, S., Harpsøe, K., Hinse, T. C., Kerins, E., Mancini, L., Mathiasen, M., Penny, M. T., Proft, S., Rahvar, S., Ricci, D., Scarpetta, G., Schäfer, S., Schönebeck, F., Southworth, J., Surdej, J., Wambsganss, J.
Microlensing detections of cool planets are important for the construction of an unbiased sample to estimate the frequency of planets beyond the snow line, which is where giant planets are thought to form according to the core accretion theory of pla
Externí odkaz:
http://arxiv.org/abs/1205.6323
Autor:
Choi, J. -Y., Shin, I. -G., Han, C., Udalski, A., Sumi, T., Gould, A., Bozza, V., Dominik, M., Fouqué, P., Horne, K., Szymański, M. K., Kubiak, M., Soszyński, I., Pietrzyński, G., Poleski, R., Ulaczyk, K., Pietrukowicz, P., Kozłowski, S., Skowron, J., Wyrzykowski, Ł., Abe, F., Bennett, D. P., Bond, I. A., Botzler, C. S., Chote, P., Freeman, M., Fukui, A., Furusawa, K., Itow, Y., Kobara, S., Ling, C. H., Masuda, K., Matsubara, Y., Miyake, N., Muraki, Y., Ohmori, K., Ohnishi, K., Rattenbury, N. J., Saito, To., Sullivan, D. J., Suzuki, D., Suzuki, K., Sweatman, W. L., Takino, S., Tristram, P. J., Wada, K., Yock, P. C. M., Bramich, D. M., Snodgrass, C., Steele, I. A., Street, R. A., Tsapras, Y., Alsubai, K. A., Browne, P., Burgdorf, M. J., Novati, S. Calchi, Dodds, P., Dreizler, S., Fang, X. -S., Grundahl, F., Gu, C. -H., Hardis, S., Harpsøe, K., Hinse, T. C., Hornstrup, A., Hundertmark, M., Jessen-Hansen, J., Jørgensen, U. G., Kains, N., Kerins, E., Liebig, C., Lund, M., Lunkkvist, M., Mancini, L., Mathiasen, M., Penny, M. T., Rahvar, S., Ricci, D., Scarpetta, G., Skottfelt, J., Southworth, J., Surdej, J., Tregloan-Reed, J., Wambsganss, J., Wertz, O., Almeida, L. A., Batista, V., Christie, G., DePoy, D. L., Dong, Subo, Gaudi, B. S., Henderson, C., Jablonski, F., Lee, C. -U., McCormick, J., McGregor, D., Moorhouse, D., Natusch, T., Ngan, H., Park, S. -Y., Pogge, R. W., Tan, T. -G., Thornley, G., Yee, J. C., Albrow, M. D., Bachelet, E., Beaulieu, J. -P., Brillant, S., Cassan, A., Cole, A. A., Corrales, E., Coutures, C., Dieters, S., Prester, D. Dominis, Donatowicz, J., Greenhill, J., Kubas, D., Marquette, J. -B., Menzies, J. W., Sahu, K. C., Zub, M.
High-magnification microlensing events provide an important channel to detect planets. Perturbations near the peak of a high-magnification event can be produced either by a planet or a binary companion. It is known that central perturbations induced
Externí odkaz:
http://arxiv.org/abs/1204.4789
Autor:
Shin, I. -G., Han, C., Choi, J. -Y., Udalski, A., Sumi, T., Gould, A., Bozza, V., Dominik, M., Fouqué, P., Horne, K., Szymański, K., Kubiak, M., Soszyński, I., Pietrzyński, G., Poleski, R., Ulaczyk, K., Pietrukowicz, P., Kozłowski, S., Skowron, J., Wyrzykowski, Ł., Abe, F., Bennett, D. P., Bond, I. A., Botzler, C. S., Chote, P., Freeman, M., Fukui, A., Furusawa, K., Itow, Y., Kobara, S., Ling, C. H., Masuda, K., Matsubara, Y., Miyake, N., Muraki, Y., Ohmori, K., Ohnishi, K., Rattenbury, N. J., Saito, To., Sullivan, D. J., Suzuki, D., Suzuki, K., Sweatman, W. L., Takino, S., Tristram, P. J., Wada, K., Yock, P. C. M., Bramich, D. M., Snodgrass, C., Steele, I. A., Street, R. A., Tsapras, Y., Alsubai, K. A., Browne, P., Burgdorf, M. J., Novati, S. Calchi, Dodds, P., Dreizler, S., Fang, X. -S., Grundahl, F., Gu, C. -H., Hardis, S., Harpsøe, K., Hinse, T. C., Hornstrup, A., Hundertmark, M., Jessen-Hansen, J., Jørgensen, U. G., Kains, N., Kerins, E., Liebig, C., Lund, M., Lunkkvist, M., Mancini, L., Mathiasen, M., Penny, M. T., Rahvar, S., Ricci, D., Scarpetta, G., Skottfelt, J., Southworth, J., Surdej, J., Tregloan-Reed, J., Wambsganss, J., Wertz, O., Almeida, L. A., Batista, V., Christie, G., DePoy, D. L., Dong, Subo, Gaudi, B. S., Henderson, C., Jablonski, F., Lee, C. -U., McCormick, J., McGregor, D., Moorhouse, D., Natusch, T., Ngan, H., Park, S. -Y., Pogge, R. W., Tan, T. -G., Thornley, G., Yee, J. C., Albrow, M. D., Bachelet, E., Beaulieu, J. -P., Brillant, S., Cassan, A., Cole, A. A., Corrales, E., Coutures, C., Dieters, S., Prester, D. Dominis, Donatowicz, J., Greenhill, J., Kubas, D., Marquette, J. -B., Menzies, J. W., Sahu, K. C., Zub, M.
Despite astrophysical importance of binary star systems, detections are limited to those located in small ranges of separations, distances, and masses and thus it is necessary to use a variety of observational techniques for a complete view of stella
Externí odkaz:
http://arxiv.org/abs/1204.2869
Autor:
Bensby, T., Adén, D., Meléndez, J., Gould, A., Feltzing, S., Asplund, M., Johnson, J. A., Lucatello, S., Yee, J. C., Ramírez, I., Cohen, J. G., Thompson, I., Bond, I. A., Gal-Yam, A., Han, C., Sumi, T., Suzuki, D., Wada, K., Miyake, N., Furusawa, K., Ohmori, K., Saito, To., Tristram, P., Bennett, D.
[ABRIDGED] Based on high-resolution (R~42000 to 48000) and high signal-to-noise (S/N~50 to 150) spectra obtained with UVES/VLT, we present detailed elemental abundances (O, Na, Mg, Al, Si, Ca, Ti, Cr, Fe, Ni, Zn, Y, and Ba) and stellar ages for 26 mi
Externí odkaz:
http://arxiv.org/abs/1107.5606