Physics – Fluid Dynamics
Scientist
Physics
Fluid Dynamics
Scientist
Mathematics Department, University of California, Los Angeles, California 90095-1555, USA and Department of Electronics and Mechanical Engineering, Chiba University, Chiba, 263-8522, Japan
College of Science and Technology, Aoyama Gakuin University, Tokyo, 157, Japan
Faculty of Science and Technology, Aoyama Gakuin University, Setagaya, Tokyo, 157-8572, Japan
Waseda University, Tokyo, Japan
Instituto de Fisica Gleb Wataghin, Universidade Estadual de Campinas, Campinas, S.P.N. M.AmatoF. M. OliveiraCastroCentro Brasileiro de Pesquisas Fisicas, Rio de Janeiro, RJR. H. C.MaldonadoInstitute de Fisica, Universidade Federal Fluminence, Niteroi, RJH.AokiY.FujimotoY.FunayamaS.HasegawaH.KumanoH.SembaT.TabukiM.TamadaK.TanakaS.YamashitaScience and Engineering Research Laboratory, Waseda University, Shinjuku, TokyoN.ArataT.ShibataK.YokoiDepartment of Physics, Aoyama Gakuin University, Setagaya, TokyoA.OhsawaInstitute for Cosmic-Ray Research, University of Tikyo, Tanashi, Tokyo
Darmstadt, Technische Hochschule, Darmstadt, Germany
Kernforschungszentrum Karlsruhe GmbH, Institut für Kernphysik, Germany
Kernforschungszentrum Karlsruhe GmbH, Karlsruhe, Germany
Instituto de Fisica Gleb Wataghin-Universidade Estadual de Campinas, Campinas, Sáo Paulo, BrasilN. M.AmatoF. M. OliveiraCastroCentro Brasileiro de Pesquisas Fisicas, Rio de Janeiro, RJ, BrasilH.AokiY.FujimotoS.HasegawaH.Kumanok.SawayanagiH.SembaT.TabukiM.TamadaS.YamashitaScience and Engineering Research Laboratory, Waseda University, Shinjuku, Tokyo, JapanN.ArataT.ShibataK.YokoiDepartment of Physics, Aoyama Gakuin University, Setagaya, Tokyo, JapanA.OhsawaInstitute for Cosmic Ray Research, Tokyo University, Tanashi, Tokyo, Japan
Darmstadt, Technische Hochschule, Darmstadt; Kernforschungszentrum Karlsruhe GmbH, Karlsruhe, Germany
Kernfoschungszentrum Karlsruhe GmbH, Karlsruhe, Germany
Aoyamagakuin Univ., Tokyo, Japan.
Kernforschungszentrum Karlsruhe GmbH, Institut für Kernphyik III, Karlsruhe, Germany
A new type of nuclear interactions in the ΣEγ>~1014 eV region
Accreting white dwarf models of Type I supernovae. III - Carbon deflagration supernovae
Atmospheric Phenomena of High Energy Cosmic Rays at Mt. Chacaltaya. (Abstract)
Carbon deflagration models for type-I supernovae and theoretical optical spectra
Centauro and Mini Centauro
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