12 results on '"Asamura, Kazushi"'
Search Results
2. Ion hole formation and nonlinear generation of electromagnetic ion cyclotron waves: THEMIS observations
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Angelopoulos, Vassilis, Shoji, Masafumi, Miyoshi, Yoshizumi, Katoh, Yuto, Keika, Kunihiro, Kasahara, Satoshi, Asamura, Kazushi, Nakamura, Satoko, and Omura, Yoshiharu
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Physics ,010504 meteorology & atmospheric sciences ,Waves in plasmas ,Cyclotron ,Plasma ,Ion acoustic wave ,01 natural sciences ,Charged particle ,law.invention ,Ion ,Geophysics ,Distribution function ,Physics::Plasma Physics ,law ,Electric field ,Physics::Space Physics ,0103 physical sciences ,General Earth and Planetary Sciences ,Atomic physics ,010303 astronomy & astrophysics ,0105 earth and related environmental sciences - Abstract
Accepted: 2017-08-09, 資料番号: SA1170120000
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- 2017
3. High‐speed MCP anodes for high time resolution low‐energy charged particle spectrometers
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Krieger, Amanda, Saito, Yoshifumi, Yokota, Shoichiro, and Asamura, Kazushi
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Resistive touchscreen ,Materials science ,010504 meteorology & atmospheric sciences ,Spectrometer ,business.industry ,Plasma ,Integrated circuit ,01 natural sciences ,Charged particle ,Anode ,law.invention ,Geophysics ,Space and Planetary Science ,law ,visual_art ,0103 physical sciences ,visual_art.visual_art_medium ,Optoelectronics ,Microchannel plate detector ,Ceramic ,business ,010303 astronomy & astrophysics ,0105 earth and related environmental sciences - Abstract
Accepted: 2017-01-25, 資料番号: SA1160337000
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- 2017
4. Density Depletions Associated With Enhancements of Electron Cyclotron Harmonic Emissions: An ERG Observation
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Usui, H., Wang, B. -J., Wang, S. -Y., Tam, S. W. Y., Chang, T. -F., Ho, P. T. P., Shoji, Masafumi, Kazama, Yoichi, Kojima, Hirotsugu, Miyoshi, Yoshizumi, Kasahara, Yoshiya, Asamura, Kazushi, Kumamoto, Atsushi, Tsuchiya, Fuminori, Kasaba, Yasumasa, Matsuda, Shoya, Matsuoka, Ayako, Teramoto, Mariko, Takashima, Takeshi, and Shinohara, Iku
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Physics ,010504 meteorology & atmospheric sciences ,Cyclotron ,Electron ,010502 geochemistry & geophysics ,01 natural sciences ,law.invention ,Geophysics ,law ,Harmonic ,General Earth and Planetary Sciences ,Atomic physics ,Erg ,0105 earth and related environmental sciences - Abstract
著者人数: 20名, Accepted: 2018-09-18, 資料番号: SA1180144000
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- 2018
5. Scattering characteristics and imaging of energetic neutral atoms from the Moon in the terrestrial magnetosheathMagnetosheath-Moon Interaction
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Lue Charles, Futaana Yoshifumi, Barabash Stas, Saito Yoshifumi, Nishino Masaki, Wieser Martin, Asamura Kazushi, Bhardwaj Anil, and Wurz Peter
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Physics::Space Physics ,Astrophysics::Earth and Planetary Astrophysics ,Physics::Geophysics - Abstract
We study hydrogen energetic neutral atom (ENA) emissions from the lunar surface when the Moon is inside the terrestrial magnetosheath. The ENAs are generated by neutralization and backscattering of incident protons of solar wind origin. First we model the effect of the increased ion temperature in the magnetosheath (>10 times larger than that in the undisturbed solar wind) on the ENA scattering characteristics. Then we apply these models to ENA measurements by Chandrayaan 1 and simultaneous ion measurements by Kaguya at the Moon in the magnetosheath. We produce maps of the ENA scattering fraction covering a region at the lunar near side that includes mare and highland surfaces and several lunar magnetic anomalies. We see clear signatures of plasma shielding by the magnetic anomalies. The maps are made at different lunar local times and the results indicate an extended influence and altered morphology of the magnetic anomalies at shallower incidence angles of the magnetosheath protons. The scattering fraction from the unmagnetized regions remains consistent with that in the undisturbed solar wind (10 20). Moreover the observed ENA energy spectra are well reproduced by our temperature dependent model. We conclude that the ENA scattering process is unchanged in the magnetosheath. Similarly to the undisturbed solar wind case it is only magnetic anomalies that provide contrast in the ENA maps not any selenomorphological features such as mare and highland regions.
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- 2016
- Full Text
- View/download PDF
6. The ERG Science Center
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Chang, T. F., Miyoshi, Yoshizumi, Hori, Tomoaki, Shoji, Masafumi, Teramoto, Mariko, Segawa, Tomonori, Umemura, Norio, Matsuda, Shoya, Kurita, Satoshi, Keika, Kunihiro, Miyashita, Yukinaga, Seki, Kanako, Tanaka, Yoshimasa, Nishitani, Nozomu, Kasahara, Satoshi, Yokota, Shoichiro, Matsuoka, Ayako, Kasahara, Yoshiya, Asamura, Kazushi, Takashima, Takeshi, and Shinohara, Iku
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lcsh:QB275-343 ,010504 meteorology & atmospheric sciences ,Computer science ,lcsh:Geodesy ,lcsh:QE1-996.5 ,lcsh:Geography. Anthropology. Recreation ,Geology ,Space physics ,01 natural sciences ,lcsh:Geology ,lcsh:G ,Space and Planetary Science ,0103 physical sciences ,Data file ,Analysis software ,Satellite ,Center (algebra and category theory) ,010303 astronomy & astrophysics ,Erg ,0105 earth and related environmental sciences ,Remote sensing - Abstract
著者人数: 21名, Accepted: 2018-05-23, 資料番号: SA1180018000
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- 2018
7. Imaging the South Pole–Aitken basin in backscattered neutral hydrogen atoms
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Vorburger, A., Wurz, P., Barabash, S., Wieser, M., Bhardwaj, A., Futaana, Yoshifumi, and Asamura, Kazushi
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Physics ,Energetic neutral atom ,Hydrogen ,Mineralogy ,Flux ,chemistry.chemical_element ,Astronomy and Astrophysics ,Plasma ,Surface finish ,Geophysics ,South Pole-Aitken basin ,Backscattering ,South Pole–Aitken basin ,Energetic neutralatoms ,Solar wind ,chemistry ,Space and Planetary Science ,Physics::Space Physics ,Moon ,Magnetic anomaly ,Physics::Atmospheric and Oceanic Physics - Abstract
Accepted: 2015-02-11, 資料番号: SA1150127000
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- 2015
8. First Direct Observation of Sputtered Lunar Oxygen
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Vorburger, A., Wurz, P., Barabash, S., Wieser, M., Holmstrom, M., Bhardwaj, A., Futaana, Yoshifumi, and Asamura, Kazushi
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Physics ,530 Physics ,Flux ,chemistry.chemical_element ,Alpha particle ,Atmosphere of Mercury ,Oxygen ,Atmosphere ,Solar wind ,Geophysics ,chemistry ,Space and Planetary Science ,Physics::Space Physics ,Astrophysics::Earth and Planetary Astrophysics ,Atomic physics ,Helium ,Exosphere - Abstract
Accepted: 2014-01-12, 資料番号: SA1140003000
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- 2014
9. Remote energetic neutral atom imaging of electric potential over a lunar magnetic anomaly
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Barabash, S., Wieser, M., Lue, C., Wurz, P., Vorburger, A., Bhardwaj, A., Futaana, Yoshifumi, and Asamura, Kazushi
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010504 meteorology & atmospheric sciences ,530 Physics ,FOS: Physical sciences ,01 natural sciences ,Astrobiology ,Physics - Space Physics ,0103 physical sciences ,Magnetic anomaly ,010303 astronomy & astrophysics ,0105 earth and related environmental sciences ,Earth and Planetary Astrophysics (astro-ph.EP) ,Physics ,Energetic neutral atom ,520 Astronomy ,620 Engineering ,Space Physics (physics.space-ph) ,Physics - Plasma Physics ,Plasma Physics (physics.plasm-ph) ,Geophysics ,13. Climate action ,Physics::Space Physics ,General Earth and Planetary Sciences ,Astrophysics::Earth and Planetary Astrophysics ,Electric potential ,Lunar science ,Astrophysics - Earth and Planetary Astrophysics - Abstract
The formation of electric potential over lunar magnetized regions is essential for understanding fundamental lunar science, for understanding the lunar environment, and for planning human exploration on the Moon. A large positive electric potential was predicted and detected from single point measurements. Here, we demonstrate a remote imaging technique of electric potential mapping at the lunar surface, making use of a new concept involving hydrogen neutral atoms derived from solar wind. We apply the technique to a lunar magnetized region using an existing dataset of the neutral atom energy spectrometer SARA/CENA on Chandrayaan-1. Electrostatic potential larger than +135 V inside the Gerasimovic anomaly is confirmed. This structure is found spreading all over the magnetized region. The widely spread electric potential can influence the local plasma and dust environment near the magnetic anomaly., 19 pages, 3 figures
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- 2013
10. Studying the Lunar—Solar Wind Interaction with the SARA Experiment aboard the Indian Lunar Mission Chandrayaan-1
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Anil Bhardwaj, Stas Barabash, M. B. Dhanya, Martin Wieser, Futaana Yoshifumi, Mats Holmström, R. Sridharan, Peter Wurz, Audrey Schaufelberger, Asamura Kazushi, M. Maksimovic, K. Issautier, N. Meyer-Vernet, M. Moncuquet, and F. Pantellini
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Earth and Planetary Astrophysics (astro-ph.EP) ,Physics ,Spectrum analyzer ,Range (particle radiation) ,Solar System ,Energetic neutral atom ,520 Astronomy ,FOS: Physical sciences ,620 Engineering ,Space Physics (physics.space-ph) ,Ion ,Computational physics ,Solar wind ,Magnetosheath ,Physics - Space Physics ,Physics::Space Physics ,Atom ,Astrophysics::Solar and Stellar Astrophysics ,Astrophysics::Earth and Planetary Astrophysics ,Astrophysics - Instrumentation and Methods for Astrophysics ,Instrumentation and Methods for Astrophysics (astro-ph.IM) ,Astrophysics - Earth and Planetary Astrophysics - Abstract
The first Indian lunar mission Chandrayaan-1 was launched on 22 October 2008. The Sub-keV Atom Reflecting Analyzer (SARA) instrument onboard Chandrayaan-1 consists of an energetic neutral atom (ENA) imaging mass analyzer called CENA (Chandrayaan-1 Energetic Neutrals Analyzer), and an ion-mass analyzer called SWIM (Solar wind Monitor). CENA performed the first ever experiment to study the solar wind-planetary surface interaction via detection of sputtered neutral atoms and neutralized backscattered solar wind protons in the energy range ~0.01-3.0 keV. SWIM measures solar wind ions, magnetosheath and magnetotail ions, as well as ions scattered from lunar surface in the ~0.01-15 keV energy range. The neutral atom sensor uses conversion of the incoming neutrals to positive ions, which are then analyzed via surface interaction technique. The ion mass analyzer is based on similar principle. This paper presents the SARA instrument and the first results obtained by the SWIM and CENA sensors. SARA observations suggest that about 20% of the incident solar wind protons are backscattered as neutral hydrogen and ~1% as protons from the lunar surface. These findings have important implications for other airless bodies in the solar system., Comment: 4 pages, 6 figures
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- 2010
11. The SUB-KEV atom reflecting analyzer (SARA) experiment aboard Chandrayaan-1 Mission: instrument and observations
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Stas Barabash, Futaana Yoshifumi, Asamura Kazushi, Peter Wurz, Anil Bhardwaj, R. Sridharan, Mats Holmström, M. B. Dhanya, Audrey Schaufelberger, and Martin Wieser
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Physics ,Spectrum analyzer ,Solar System ,Energetic neutral atom ,Spacecraft ,business.industry ,520 Astronomy ,Analyser ,Astronomy ,620 Engineering ,Solar wind ,Atom ,Absorption (electromagnetic radiation) ,business - Abstract
SARA experiment aboard the first Indian lunar mission Chandrayaan-1 had the objective to explore the solar wind-lunar interaction using energetic neutral atoms (ENA) from the lunar surface as diagnostic tool. SARA consisted of an ENA imaging mass analyzer CENA (Chandrayaan-1 Energetic Neutral Analyzer) and an ion mass analyser SWIM (Solar Wind Monitor), along with a digital processing unit (DPU) which commands and controls the sensors and provides the interface to the spacecraft. Both sensors have provided excellent observational data. CENA has observed ENAs from the lunar surface and found that ~20% of the incident solar wind ions get backscattered as ENAs from the lunar surface. This is contrary to the previous assumptions of almost complete absorption of solar wind by the lunar surface. The observation is relevant for other airless bodies in the solar system.
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- 2010
- Full Text
- View/download PDF
12. Pre-flight Calibration and Near-Earth Commissioning Results of the Mercury Plasma Particle Experiment (MPPE) Onboard MMO (Mio)
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Saito, Yoshifumi, Delcourt, Dominique, Hirahara, Masafumi, Barabash, Stas, André, Nicolas, Takashima, Takeshi, Asamura, Kazushi, Yokota, Shoichiro, Wieser, Martin, Nishino, Masaki N., Oka, Mitsuo, Futaana, Yoshifumi, Harada, Yuki, Sauvaud, Jean-André, Louarn, Philippe, Lavraud, Benoit, Génot, Vincent, Mazelle, Christian, Dandouras, Iannis, Jacquey, Christian, Aoustin, Claude, Barthe, Alain, Cadu, Alexandre, Fedorov, Andréi, Frezoul, Anne-Marie, Garat, Catherine, Le Comte, Eric, Lee, Qiu-Mei, Médale, Jean-Louis, Moirin, David, Penou, Emmanuel, Petiot, Mathieu, Peyre, Guy, Rouzaud, Jean, Séran, Henry-Claude, Nĕmec̆ek, Zdenĕk, S̆afránková, Jana, Marcucci, Maria Federica, Bruno, Roberto, Consolini, Giuseppe, Miyake, Wataru, Shinohara, Iku, Hasegawa, Hiroshi, Seki, Kanako, Coates, Andrew J., Leblanc, Frédéric, Verdeil, Christophe, Katra, Bruno, Fontaine, Dominique, Illiano, Jean-Marie, Berthelier, Jean-Jacques, Techer, Jean-Denis, Fraenz, Markus, Fischer, Henning, Krupp, Norbert, Woch, Joachim, Bührke, Ulrich, Fiethe, Björn, Michalik, Harald, Matsumoto, Haruhisa, Yanagimachi, Tomoki, Miyoshi, Yoshizumi, Mitani, Takefumi, Shimoyama, Manabu, Zong, Qiugang, Wurz, Peter, Andersson, Herman, Karlsson, Stefan, Holmström, Mats, Kazama, Yoichi, Ip, Wing-Huen, Hoshino, Masahiro, Fujimoto, Masaki, Terada, Naoki, and Keika, Kunihiro
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13. Climate action ,520 Astronomy ,620 Engineering ,7. Clean energy - Abstract
BepiColombo Mio (previously called MMO: Mercury Magnetospheric Orbiter) was successfully launched by Ariane 5 from Kourou, French Guiana on October 20, 2018. The Mercury Plasma/Particle Experiment (MPPE) is a comprehensive instrument package onboard Mio spacecraft used for plasma, high-energy particle and energetic neutral atom measurements. It consists of seven sensors including two Mercury Electron Analyzers (MEA1 and MEA2), Mercury Ion Analyzer (MIA), Mass Spectrum Analyzer (MSA), High Energy Particle instrument for electron (HEP-ele), High Energy Particle instrument for ion (HEP-ion), and Energetic Neutrals Analyzer (ENA). Significant efforts were made pre-flight to calibrate all of the MPPE sensors at the appropriate facilities on the ground. High voltage commissioning of MPPE analyzers was successfully performed between June and August 2019 and in February 2020 following the completion of the low voltage commissioning in November 2018. Although all of the MPPE analyzers are now ready to begin observation, the full service performance has been delayed until Mio’s arrival at Mercury. Most of the fields of view (FOVs) of the MPPE analyzers are blocked by the thermal shield surrounding the Mio spacecraft during the cruising phase. Together with other instruments on Mio including Magnetic Field Investigation (MGF) and Plasma Wave Investigation (PWI) that measure plasma field parameters, MPPE will contribute to the comprehensive understanding of the plasma environment around Mercury when BepiColombo/Mio begins observation after arriving at the planet Mercury in December 2025.
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