基本情報
- 所属
- 国立研究開発法人宇宙航空研究開発機構 宇宙科学研究所 太陽系科学研究系 准教授
- 学位
- 博士(理学)
- J-GLOBAL ID
- 200901058783588460
- researchmap会員ID
- 1000292024
研究分野
1経歴
2-
2019年6月 - 現在
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1999年4月
学歴
2-
1995年4月 - 1997年3月
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1991年4月 - 1995年3月
委員歴
3-
2022年4月 - 現在
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2019年4月 - 2025年3月
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2020年4月 - 2022年3月
論文
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JOURNAL OF THE AMERICAN SOCIETY FOR MASS SPECTROMETRY 36(3) 553-564 2025年2月10日In some types of mass spectrometers, such as time-of-flight mass spectrometers (TOF-MSs), it is necessary to control pulsed beams of ions. This can be easily accomplished by applying a pulsed voltage to the pusher electrode while the ionizer is continuously flowing ions. This method is preferred for its simplicity, although the ion utilization efficiency is not optimized. Here we employed another pulse-control method with a higher ion utilization rate, which is to bunch ions and kick them out instead of letting them stream. The benefit of this method is that higher sensitivity can be achieved; since the start of new ions cannot be allowed during TOF separation, it is highly advantageous to bunch ions that would otherwise be unusable. In this study, we used analytical and numerical methods to design a new bunching ionizer with reduced resources, adopting the principle of the electrostatic ion beam trap. The test model experimentally demonstrated the bunching performance with respect to the sample gas density and ion bunching time using gas samples and electron impact ionization. We also conducted an experiment connecting the newly developed bunching ionizer with a miniature TOF-MS. As a result, the sensitivity was improved by an order of magnitude compared to the case using a nonbunching ionizer. Since the device is capable of bunching ions with low voltage and power consumption, it will be possible to find applications in portable mass spectrometers with reduced resources.
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Geophysical Research Letters 52(3) 2025年2月10日 査読有りAbstract We report a statistical result of electrons inside the loss cone with energies of 67 eV–88 keV using electron measurements obtained in situ by the Arase satellite in the inner magnetosphere around the magnetic equator for 60 months. Loss cone electrons are found with a high occurrence probability from the nightside to the dawnside at approximately L = 6. For 641 eV–88 keV electrons, the high‐occurrence region shifts toward later magnetic local times (MLTs) with increasing loss cone electron energy. The spatial distribution of the occurrence probability around MLT = 22–3 at L = 5–6 is consistent with the calculated average resonance energy distribution of whistler mode chorus waves near the magnetic equator. These results suggest that pitch angle scattering driven by chorus waves plays the main role in electron precipitation in this region.
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Journal of Geophysical Research: Space Physics 130(2) 2025年2月6日 査読有りAbstract Strong Thermal Emission Velocity Enhancement (STEVE) is a latitudinally narrow, purple‐band emission observed at subauroral latitudes. Stable Auroral Red (SAR) arcs characterized by major red emission, and red/green arcs with both red and green emissions also occur at subauroral latitudes. Characteristics of magnetospheric source plasma and electromagnetic fields of these three types of arcs have not been fully understood because of the limited conjugate observations between magnetosphere and the ground. In this study, we report 11 conjugate observations (2 STEVEs, 7 SAR arcs, and 2 red/green arcs), using all‐sky images obtained at seven ground stations over more than four years from January 2017 to April 2021 and magnetospheric satellites (Arase and Van Allen Probes). We found that, in the inner magnetosphere, the source region of STEVEs and red/green arcs were located outside the plasmasphere, and that of the SAR arc was in the region of spatial overlap between the plasmasphere and ring current region. Electromagnetic waves at frequencies below 1 Hz were observed for STEVEs and red/green arcs. SuperDARN radar data showed a strong westward plasma flow in the ionosphere, especially during STEVE events, whereas the plasma flows associated with SAR arcs and red/green arcs were generally weaker and variable. The STEVE and SAR arc can appear simultaneously at slightly different latitudes and STEVEs and red/green arcs can transform into SAR arcs. These first comprehensive ground‐satellite measurements of three types of subauroral‐latitude auroras increase our understanding on similarlity, differences, and coupling of these auroras in the ionosphere and the magnetosphere.
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Vacuum 114132-114132 2025年2月 査読有り
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Journal of Geophysical Research: Space Physics 129(11) 2024年11月12日 査読有りAbstract We estimated the altitude of aurora by combining data from all‐sky cameras at multiple places which were obtained during the LAMP sounding rocket experiment in Alaska on 5 March 2022. During the launch window of the rocket, three high‐speed all‐sky cameras were operative at three stations immediately below the trajectory of the rocket: Poker Flat, Venetie and Fort Yukon. The all‐sky cameras captured all‐sky images with a temporal resolution of 100 Hz (80 Hz for the Fort Yukon case). The method of altitude determination is based on analyses of time‐series of the optical intensity obtained from the all‐sky cameras in Venetie and Poker Flat covering the downrange area of the rocket trajectory. The estimated altitude of pulsating aurora during the rocket experiment was found to be consistent with that derived from the in‐situ observation of precipitating electrons with a model of optical emission, which confirms the feasibility of deriving the emission altitude through correlation analyses using time‐series. The estimated altitude of aurora decreased after the expansion onset of the substorm and stayed slightly below 100 km during the interval of pulsating aurora in the recovery phase. In particular, prompt and brief lowering of the auroral emission, well down to around 90 km, was detected during a transition of auroral form from discrete to diffuse which occurred ∼10 min after the onset. This result implies an existence of a process causing harder electron precipitation operative soon after the start of the expansion phase of auroral substorm.
MISC
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地球電磁気・地球惑星圏学会総会及び講演会予稿集(CD-ROM) 124th 2008年
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地球電磁気・地球惑星圏学会総会及び講演会予稿集(CD-ROM) 124th ROMBUNNO.B006-18 2008年
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電子情報通信学会技術研究報告. SANE, 宇宙・航行エレクトロニクス 107(2) 43-48 2007年4月9日This paper describes the on-orbit results and lessons learned of the small scientific satellite "INDEX" (REIMEI) for aurora observation and demonstration of advanced satellite technologies. REIMEI is a small satellite with 72kg mass, and is provided with three-axis attitude controlled capabilities for aurora observation. REIMEI was launched into a nearly sun synchronous polar orbit on Aug. 23^<rd>, 2005 (UT) from Baikonur, Kazakhstan by Dnepr rocket. REIMEI satellite functions satisfactorily on the orbit. Three axis control is achieved with accuracy of 0.05 deg. Multi-spectrum images of aurora are taken with 8Hz rate and 2 km spatial resolution to investigate the aurora physics. REIMEI is a small scientific satellite for aurora observation and advanced satellite technologies, and was launched into a nearly sun synchronous polar orbit on Aug. 23^<rd>, 2005 (UTC) from Baikonur, Kazakhstan by Dnepr rocket. REIMEI satellite functions satisfactorily on the orbit. The three-axis attitude control is achieved with accuracy of 0.05deg. REIMEI is performing the simultaneous observation of aurora images as well as particle measurements. REIMEI indicates that even a small satellite launched as a piggy-back can successfully perform the unique scientific mission purposes.
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ICARUS 187(2) 623-625 2007年4月
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地球電磁気・地球惑星圏学会総会及び講演会予稿集(CD-ROM) 122nd ROMBUNNO.B006-40 2007年
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SPACE SCIENCE REVIEWS 126(1-4) 333-354 2006年10月Aurora is caused by the precipitation of energetic particles into a planetary atmosphere, the light intensity being roughly proportional to the precipitating particle energy flux. From auroral research in the terrestrial magnetosphere it is known that bright auroral displays, discrete aurora, result from an enhanced energy deposition caused by downward accelerated electrons. The process is commonly referred to as the auroral acceleration process. Discrete aurora is the visual manifestation of the structuring inherent in a highly magnetized plasma. A strong magnetic field limits the transverse (to the magnetic field) mobility of charged particles, effectively guiding the particle energy flux along magnetic field lines. The typical, slanted arc structure of the Earth's discrete aurora not only visualizes the inclination of the Earth's magnetic field, but also illustrates the confinement of the auroral acceleration process. The terrestrial magnetic field guides and confines the acceleration processes such that the preferred acceleration of particles is frequently along the magnetic field lines. Field-aligned plasma acceleration is therefore also the signature of strongly magnetized plasma. This paper discusses plasma acceleration characteristics in the night-side cavity of Mars. The acceleration is typical for strongly magnetized plasmas - field-aligned acceleration of ions and electrons. The observations map to regions at Mars of what appears to be sufficient magnetization to support magnetic field-aligned plasma acceleration - the localized crustal magnetizations at Mars (Acuna et al., 1999). Our findings are based on data from the ASPERA-3 experiment on ESA's Mars Express, covering 57 orbits traversing the night-side/eclipse of Mars. There are indeed strong similarities between Mars and the Earth regarding the accelerated electron and ion distributions. Specifically acceleration above Mars near local midnight and acceleration above discrete aurora at the Earth - characterized by nearly monoenergetic downgoing electrons in conjunction with nearly monoenergetic upgoing ions. We describe a number of characteristic features in the accelerated plasma: The "inverted V" energy-time distribution, beam vs temperature distribution, altitude distribution, local time distribution and connection with magnetic anomalies. We also compute the electron energy flux and find that the energy flux is sufficient to cause weak to medium strong (up to several tens of kR 557.7 nm emissions) aurora at Mars. Monoenergetic counterstreaming accelerated ions and electrons is the signature of field-aligned electric currents and electric field acceleration. The topic is reasonably well understood in terrestrial magnetospheric physics, although some controversy still remains on details and the cause-effect relationships. We present a potential cause-effect relationship leading to auroral plasma acceleration in the nightside cavity of Mars - the downward acceleration of electrons supposedly manifesting itself as discrete aurora above Mars.
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SPACE SCIENCE REVIEWS 126(1-4) 239-266 2006年10月Although the Mars Express (MEX) does not carry a magnetometer, it is in principle possible to derive the interplanetary magnetic field (IMF) orientation from the three dimensional velocity distribution of pick-up ions measured by the Ion Mass Analyser (IMA) on board MEX because pick-up ions' orbits, in velocity phase space, are expected to gyrate around the IMF when the IMF is relatively uniform on a scale larger than the proton gyroradius. During bow shock outbound crossings, MEX often observed cycloid distributions (two dimensional partial ring distributions in velocity phase space) of protons in a narrow channel of the IMA detector (only one azimuth for many polar angles). We show two such examples. Three different methods are used to derive the IMF orientation from the observed cycloid distributions. One method is intuitive (intuitive method), while the others derive the minimum variance direction of the velocity vectors for the observed ring ions. These velocity vectors are selected either manually (manual method) or automatically using simple filters (automatic method). While the intuitive method and the manual method provide similar IMF orientations by which the observed cycloid distribution is well arranged into a partial circle (representing gyration) and constant parallel velocity, the automatic method failed to arrange the data to the degree of the manual method, yielding about a 30 degrees offset in the estimated IMF direction. The uncertainty of the derived IMF orientation is strongly affected by the instrument resolution. The source population for these ring distributions is most likely newly ionized hydrogen atoms, which are picked up by the solar wind.
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SPACE SCIENCE REVIEWS 126(1-4) 113-164 2006年10月The general scientific objective of the ASPERA-3 experiment is to study the solar wind atmosphere interaction and to characterize the plasma and neutral gas environment within the space near Mars through the use of energetic neutral atom (ENA) imaging and measuring local ion and electron plasma. The ASPERA-3 instrument comprises four sensors: two ENA sensors, one electron spectrometer, and one ion spectrometer. The Neutral Particle Imager (NPI) provides measurements of the integral ENA flux (0.1 - 60 keV) with no mass and energy resolution, but high angular resolution. The measurement principle is based on registering products ( secondary ions, sputtered neutrals, reflected neutrals) of the ENA interaction with a graphite-coated surface. The Neutral Particle Detector (NPD) provides measurements of the ENA flux, resolving velocity ( the hydrogen energy range is 0.1 10 keV) and mass ( H and O) with a coarse angular resolution. The measurement principle is based on the surface reflection technique. The Electron Spectrometer (ELS) is a standard top-hat electrostatic analyzer in a very compact design which covers the energy range 0.01 - 20 keV. These three sensors are located on a scanning platform which provides scanning through 180 degrees of rotation. The instrument also contains an ion mass analyzer (IMA). Mechanically IMA is a separate unit connected by a cable to the ASPERA-3 main unit. IMA provides ion measurements in the energy range 0.01 - 36 keV/charge for the main ion components H+, He++, He+, O+, and the group of molecular ions 20 - 80 amu/q. ASPERA-3 also was its own DC/DC converters and digital processing unit (DPU).
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電子情報通信学会技術研究報告. SANE, 宇宙・航行エレクトロニクス 105(438) 29-34 2005年11月25日小型科学衛星INDEX(れいめい)の打上げと初期成果
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European Space Agency, (Special Publication) ESA SP (1240) 121-139 2004年8月The ASPERA-3 (Analyser of Space Plasma and Energetic Atoms) instrument of Mars Express is designed to study the solar wind-Mars atmosphere interaction and to characterise the plasma and neutral gas environment in near-Mars space through energetic neutral atom (ENA) imaging and local charged-particle measurements. The studies address the fundamental question: how strongly do the interplanetary plasma and electromagnetic fields affect the martian atmosphere? This question is directly related to the problem of martian dehydration. The instrument comprises four sensors two ENA sensors, and electron and ion spectrometers. The Neutral Particle Imager (NPI) measures the integral ENA flux (0.1-60 keV) with no mass and energy resolution but with high angular resolution. The Neutral Particle Detector (NPD) measures the ENA flux, resolving energy (0.1-10 keV) and mass (H and O) with a coarse angular resolution. The electron spectrometer (ELS) is a standard top-hat electrostatic analyser of a very compact design. These three sensors are mounted on a scanning platform providing 4π coverage. The instrument includes an ion mass composition sensor, IMA (Ion Mass Analyser). Mechanically, IMA is a separate unit connected by a cable to the ASPERA-3 main unit. IMA provides ion measurements in the energy range 0.01-40 keV/q for the main ion components H+, He 2+, He+O+ with 20-80 amu/g.
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地球電磁気・地球惑星圏学会総会及び講演会予稿集(CD-ROM) 110th (Web) 2001年
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REVIEW OF SCIENTIFIC INSTRUMENTS 71(8) 3024-3030 2000年8月A new-type analyzer for measurement of energetic neutral atoms (ENAs) in an energy range of 4-40 keV is described. Incoming ENAs are ionized by electron stripping at passage of an ultrathin carbon foil. After post-acceleration (by 3 kV), the particles are guided to a time-of-flight (TOF) section over a wide energy-per-charge bandwidth by means of electrostatic deflection without any potential sweeping for electrodes. Then, their velocity is measured by the TOF technique, with which species can also be identified, because the particle energies are limited to a certain range by the electrostatic deflector and acceleration upon entering the TOF section. A unique feature in the present analyzer is in the rejection method of extreme ultraviolet (EUV) contamination. In contrast to conventional usage of serrated electrodes for EUV attenuation, one of the electrostatic deflection plates is machined to be so flat that EUV photons are guided to a photon trap regardless of wavelength. The TOF device can also be used in a coincidence mode for noise suppression. The present instrument was flown on a sounding rocket, and has successfully measured ENAs precipitating into the low-latitude upper atmosphere from the magnetosphere. (C) 2000 American Institute of Physics. [S0034- 6748(00)02008-6].
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GEOPHYSICAL RESEARCH LETTERS 26(1) 33-36 1999年1月Energetic neutral atoms (ENAs) with energies of 4 to 35 keV were measured at altitudes of 170 to 570 km by a new ENA instrument on board a sounding rocket. The instrument measured particles precipitating into the ionosphere from the equatorial region of the magnetosphere at a magnetic local time of similar to 1830. The geomagnetic activity was quiet for a prolonged period before the launch. The measured ENA flux was similar to 10(2) (cm(2) s str keV)(-1) at energies of similar to 10 keV. The energy spectrum is in a good agreement with an expected spectrum of hydrogen atoms originating from the ring current region as reported by Milillo et al. [1996]. The altitude profile is also discussed in terms of collisional interaction of ENAs with upper-atmospheric constituents.
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ISAS Research Note 607 1997年
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JOURNAL OF GEOMAGNETISM AND GEOELECTRICITY 47(10) 973-987 1995年The ionospheric neutral wind is induced by the ion drag forcing under the sufficiently continuous southward IMF conditions in the polar region. If the IMF turns northward sharply after prolonged southward interval, the neutral wind gives its own momentum to the charged particles and makes the ionospheric currents. This phenomenon is one of the forms of ''flywheel'' effect. To ascertain the existence of the flywheel effect and to obtain its global pattern in the polar region we analyzed the ionospheric equivalent current system derived from ground-based geomagnetic observation by superposed epoch method. The results show (1) appearance of dawnward and antisunward currents after IMF northward turning, (2) its attenuation with a time constant of several hours, (3) seasonal dependence in the attenuation time constant, (4) small day-night difference in the current intensity after the turning. The antisunward current is stronger for the case with prolonged southward IMF interval before the northward turning than that for short and weak southward IMF case. These results are consistent with the theoretical expectations of the flywheel effect, though there are some difference with the prediction by computer simulations in the global current pattern such as the dawnward rotation of the current vector.
共同研究・競争的資金等の研究課題
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日本学術振興会 科学研究費助成事業 国際共同研究加速基金(国際共同研究強化(B)) 2022年10月 - 2027年3月
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日本学術振興会 科学研究費助成事業 基盤研究(A) 2021年4月 - 2026年3月
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日本学術振興会 科学研究費助成事業 挑戦的研究(萌芽) 2022年6月 - 2025年3月
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日本学術振興会 科学研究費助成事業 基盤研究(B) 2021年4月 - 2024年3月
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日本学術振興会 科学研究費助成事業 基盤研究(B) 2021年4月 - 2024年3月