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Your search keyword '"Morishita, Isao"' showing total 34 results
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34 results on '"Morishita, Isao"'

2. High-resolution two-dimensional map of the solar-time anisotropy obtained by the GRAPES-3 large-area muon telescope

Author

Koi, Tatsumi, primary, Kojima, Hiroshi, additional, Ahmad, Shakeel, additional, Chakraborty, Medha, additional, Chandra, Anuj, additional, Dugad, Shashi, additional, Gupta, Snil K., additional, Hariharan, Balakrishnan, additional, Hayashi, Yoshio, additional, Jagadeesan, Paranjothi, additional, Jain, Atul, additional, Jain, Pankaj, additional, Jhansi, Vuta B., additional, Kawakami, Saburo, additional, Mahapatra, Swapna, additional, Matsuyama, Toshio, additional, Mohanty, Pravata, additional, Morishita, Isao, additional, Morris, Sumuel D., additional, Muraki, Yasushi, additional, Nakamura, Toru, additional, Nayak, Pranaba, additional, Nonaka, Toshiyuki, additional, Ogio, Shoichi, additional, Oshima, Akitoshi, additional, Pattanaik, Diptiranjan, additional, Rakshe, Pankaj S., additional, Ramesh, Kaviti, additional, Rao, Bellam S., additional, Reddy, Lakki V., additional, Shibata, Shoichi, additional, Takamaru, Hisanori, additional, Tanaka, Koichi, additional, Varsi, Fahim, additional, Yamazaki, Katsuya, additional, and Zuberi, Meeran, additional

Published
2021
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3. Correlation between Cosmic Ray Intensity Variations Observed by the Large Acceptance GRAPES-3 Muon Telescope and Interplanetary Magnetic Field.

Author

Shibata, Shoichi, primary, Kojima, Hiroshi, additional, Oshima, Akitoshi, additional, Kawakami, Saburo, additional, Hayashi, Yoshio, additional, Morishita, Isao, additional, Nakamura, Toru, additional, Nonaka, Toshiyuki, additional, Ogio, Shoichi, additional, Takamaru, Hisanori, additional, Tanaka, Koichi, additional, Ito, Nobuo, additional, Matsuyama, Toshio, additional, Yamazaki, Katsuya, additional, Tokumaru, Munetoshi, additional, Gupta, Snil K., additional, R. Dugad, Shashi, additional, Hariharan, Balakrishnan, additional, Jagadeesan, Paranjothi, additional, Jain, Atul, additional, Jhansi, Vuta B., additional, K. Mohanty, Pravata, additional, D. Morris, Samuel, additional, K. Nayak, Pranaba, additional, S. Rakshe, Pankaj, additional, Ramesh, Kaviti, additional, Rao, Bellam S., additional, Reddy, Lakki V., additional, Zuberi, Meeran, additional, Ahmad, Shakeel, additional, Chandra, Anuj, additional, and Subramanian, Prasad, additional

Published
2019
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10. Quiescence of GLE-Producible Solar Proton Eruptions during the Transition Phase of Heliomagnetic Polarity Reversal near the Solar-Activity-Maximum Period.

Author

Nagashima, Kazuo, Sakakibara, Shizuko, 1000040148200, Morishita, Isao, Cosmic-Ray Section, Solar-Terrestrial Environment Laboratory, Nagoya University, Department of Information Management, Asahi University, Nagashima, Kazuo, Sakakibara, Shizuko, 1000040148200, Morishita, Isao, Cosmic-Ray Section, Solar-Terrestrial Environment Laboratory, Nagoya University, and Department of Information Management, Asahi University

Abstract

By using data of the ground-level-enhancement (GLE), of solar cosmic rays observed with the neutron and muon monitors in the period 1942-1990, it is shown that the solar proton eruptions producible GLE are forbidden during the transition phase of the heliomagnetic polarity reversal, near the period of the maximum solar activity. It is suggested that the quiescence of GLE is not due to the suppression effect of the proton eruption from the Sun by the strong solar magnetic field, but is due to the deterioration of the proton acceleration efficiency by the structual change of the field during the transition period., By using data of the ground-level-enhancement (GLE), of solar cosmic rays observed with the neutron and muon monitors in the period 1942-1990, it is shown that the solar proton eruptions producible GLE are forbidden during the transition phase of the heliomagnetic polarity reversal, near the period of the maximum solar activity. It is suggested that the quiescence of GLE is not due to the suppression effect of the proton eruption from the Sun by the strong solar magnetic field, but is due to the deterioration of the proton acceleration efficiency by the structual change of the field during the transition period., identifier:130003558910

Published
2015

11. Interplanetary magnetic field collimated cosmic ray flow across magnetic shock from inside of Forbush decrease, observed as local-time-dependent precursory decrease on the ground

Author

Nagashima, K., Fujimoto, K., 1000040148200, Morishita, Isao, Cosmic-Ray Section, Solar-Terrestrial Environment Laboratory, Nagoya University, Department of Information Management, Asahi University, Nagashima, K., Fujimoto, K., 1000040148200, Morishita, Isao, Cosmic-Ray Section, Solar-Terrestrial Environment Laboratory, Nagoya University, and Department of Information Management, Asahi University

Abstract

source:http://sites.agu.org, source:http://publications.agu.org/author-resource-center/copyright-transfer

Published
2015

16. Interplanetary magnetic field collimated cosmic ray flow across magnetic shock from inside of Forbush decrease, observed as local-time-dependent precursory decrease on the ground

Author

Nagashima, K., Fujimoto, K., Morishita, Isao, Cosmic-Ray Section, Solar-Terrestrial Environment Laboratory, Nagoya University, and Department of Information Management, Asahi University

Subjects
Shock wave, Physics, Atmospheric Science, Neutron monitor, Ecology, Astrophysics::High Energy Astrophysical Phenomena, Paleontology, Soil Science, Forestry, Cosmic ray, Astrophysics, Aquatic Science, Oceanography, Collimated light, Solar wind, Geophysics, Space and Planetary Science, Geochemistry and Petrology, Local time, Earth and Planetary Sciences (miscellaneous), Forbush decrease, Interplanetary magnetic field, Earth-Surface Processes, Water Science and Technology
Abstract

In the previous papers (Nagashima et al., 1992, 1993) the authors pointed out the existence of the local-time-dependent precursory decrease of cosmic rays in front of the shock wave of the interplanetary magnetic field (IMF) and interpreted it as being due to the IMF-collimated outward flow of the low-density cosmic rays across the shock from the inside of the Forbush decrease. In those papers, however, the physical properties of the collimated flow such as the direction, the collimation angle, and the rigidity spectrum of the constituent cosmic rays were only estimated qualitatively owing to the lack of the simulation of the precursory decrease produced by the flow. In the present paper these properties are quantitatively obtained by analyzing the hourly data of the precursory decreases observed on January 25 and 26, 1968, at the worldwide neutron monitor stations. The obtained direction and collimation angle of the flow approximately coincide respectively with those expected from the IMF. This fact gives evidence for the reconfirmation of the existence of the IMF-guided collimated flow, responsible for the precursory decrease.

Published
1994

21. Quiescence of GLE-Producible Solar Proton Eruptions during the Transition Phase of Heliomagnetic Polarity Reversal near the Solar-Activity-Maximum Period

Author

Nagashima, Kazuo, Sakakibara, Shizuko, Morishita, Isao, Cosmic-Ray Section, Solar-Terrestrial Environment Laboratory, Nagoya University, and Department of Information Management, Asahi University

Subjects
Astrophysics::High Energy Astrophysical Phenomena, Physics::Space Physics, Physics::Accelerator Physics, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics
Abstract

By using data of the ground-level-enhancement (GLE), of solar cosmic rays observed with the neutron and muon monitors in the period 1942-1990, it is shown that the solar proton eruptions producible GLE are forbidden during the transition phase of the heliomagnetic polarity reversal, near the period of the maximum solar activity. It is suggested that the quiescence of GLE is not due to the suppression effect of the proton eruption from the Sun by the strong solar magnetic field, but is due to the deterioration of the proton acceleration efficiency by the structual change of the field during the transition period.

Published
1991

29. THE PHOTOCHEMICAL BEHAVIOR OF DI-μ-OXO-BINUCLEAR MANGANESE COMPLEXES IN ACIDIC SOLUTION

Author

Otsuji, Yoshio, Sawada, Keizo, Morishita, Isao, Taniguchi, Yukio, and Mizuno, Kazuhiko

Abstract

Di-μ-oxo-dimanganese complex [Mn2IV,IIIO2(bpy)4](Clo4)3, which is stable in the ground state, is reduced by irradiation of 313 nm light in acidic solutions. On the other hand, [Mn2IV,IVO2(phen)4](Clo4)4is reduced in the dark to the MnIV–MnIIIcomplex and then further reduced upon irradiation. The photoreductions of the complexes are accompanied by the one-electron oxidation of water to generate hydroxyl radical.

Published
1977
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34. Total synthesis of hydroxy-α- and hydroxy-β-sanshool using Suzuki-Miyaura coupling.

Author

Igarashi Y, Aoki K, Nishimura H, Morishita I, and Usui K

Subjects
Amides chemistry, Magnetic Resonance Spectroscopy, Spectrometry, Mass, Electrospray Ionization, Spectrophotometry, Infrared, Amides chemical synthesis
Abstract

Here, we describe the first total synthesis of hydroxyl-α- and hydroxyl-β-sanshool, which involves Suzuki-Miyaura coupling (SMC). Hydroxy-α-sanshool (1) was synthesized by SMC of bromoalkyne 4 with boronate 3 followed by (Z)-selective reduction of the triple bond in the coupling product. Hydroxy-β-sanshool (2) was synthesized by regio- and (E)-selective conversion of 4 to iodoalkene 11 followed by SMC with 3.

Published
2012
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