研究者詳細 - 岩井　一正

論文 - 岩井　一正

分割表示 >> ／全件表示 43 件中 1 - 43 件目

Automatic Detection of Type II Solar Radio Burst by Using 1-D Convolution Neutral Network 査読有り

56 巻 ( 2 ) 頁： 213 - 224 2023年12月

East–West Asymmetry in Interplanetary-Scintillation-Level Variation Associated with Solar-Wind Disturbances 査読有り

298 巻 ( 11 ) 2023年11月

Forecasting Heliospheric CME Solar-Wind Parameters Using the UCSD Time-Dependent Tomography and ISEE Interplanetary Scintillation Data: The 10 March 2022 CME 査読有り

Bernard V. Jackson, Munetoshi Tokumaru, Kazumasa Iwai, Matthew T. Bracamontes, Andrew Buffington, Ken’ichi Fujiki, Go Murakami, Daniel Heyner, Beatriz Sanchez-Cano, Mathias Rojo, Sae Aizawa, Nicolas Andre, Alain Barthe, Emmanuel Penou, Andrei Fedorov, Jean-Andre Sauvaud, Shoichiro Yokota, Yoshifumi Saito

Solar Physics 298 巻 ( 5 ) 2023年5月

掲載種別：研究論文（学術雑誌）出版者・発行元：Springer Science and Business Media LLC

Abstract

Remotely sensed interplanetary scintillation (IPS) data from the Institute for Space-Earth Environmental Research (ISEE), Japan, allows a determination of solar-wind parameters throughout the inner heliosphere. We show the 3D analysis technique developed for these data sets that forecast plasma velocity, density, and component magnetic fields at Earth, as well at the other inner heliospheric planets and spacecraft. One excellent coronal mass ejection (CME) example that occurred on the 10 March 2022 was viewed not only in the ISEE IPS analyses, but also by the spacecraft near Earth that measured the CME arrival at one AU. Solar Orbiter, that was nearly aligned along the Earth radial at 0.45 AU, also measured the CME in plasma density, velocity, and magnetic field. BepiColombo at 0.42 AU was also aligned with the STEREO A spacecraft, and viewed this CME. The instruments used here from BepiColombo include: 1) the European-Space-Agency Mercury-Planetary-Orbiter magnetic field measurements; 2) the Japan Aerospace Exploration Agency Mio spacecraft Solar Particle Monitor that viewed the CME Forbush decrease, and the Mercury Plasma Experiment/Mercury Electron Analyzer instruments that measured particles and solar-wind density from below the spacecraft protective sunshield covering. This article summarizes the analysis using ISEE, Japan real-time data for these forecasts: it provides a synopsis of the results and confirmation of the CME event morphology after its arrival, and discusses how future IPS analyses can augment these results.

DOI： 10.1007/s11207-023-02169-8

その他リンク： https://link.springer.com/article/10.1007/s11207-023-02169-8/fulltext.html

Interplanetary Scintillation Observations of Solar-Wind Disturbances During Cycles 23 and 24 査読有り

Munetoshi Tokumaru, Ken'ichi Fujiki, Kazumasa Iwai

SOLAR PHYSICS 298 巻 ( 2 ) 2023年2月

記述言語：英語掲載種別：研究論文（学術雑誌）出版者・発行元：SPRINGER

Interplanetary scintillation (IPS) analysis is an effective technique for remotely sensing solar-wind disturbances, such as stream-interaction regions (SIRs) and coronal mass ejections (CMEs), which are the main drivers of space weather. Here, we employed 327-MHz IPS observations conducted at the Institute of Space-Earth Environmental Research, Nagoya University for the period of 1997 - 2019 to determine IPS indices that represent the density-fluctuation level of the inner heliosphere. We then compared these indices with the solar-wind density and speed measured near the Earth. Consequently, we found weak but significant positive correlations between the IPS indices and both the solar-wind density and speed gradient at a time lag of 0 days. This suggests that an increase in IPS indices corresponds to the arrival of the compression region associated with SIR or CME at the Earth, which is consistent with model calculations. Significant negative correlations were observed between the IPS and disturbance storm time (Dst) indices at a time lag of a few days; however, the correlations were too weak to enable reliable predictions of space weather. Possible reasons for these weak correlations are also discussed. Using the IPS indices, we determined the solar-cycle variation in the occurrence rate of solar-wind disturbances for the analysis period. The occurrence rates exhibited two maxima corresponding to the solar maximum and minimum, which are generally consistent with the combined effects of CME and SIR. The lower occurrence rates in Cycle 24 than in Cycle 23 reflect a weaker solar activity. These results suggest that the proposed IPS indices are useful for studying the long-term characteristics of solar-wind disturbances.

DOI： 10.1007/s11207-023-02116-7

Solar observing with the Atacama large millimeter-submillimeter array 査読有り

T. S. Bastian, M. Shimojo, M. Bárta, S. M. White, K. Iwai

Frontiers in Astronomy and Space Sciences 9 巻 2022年10月

掲載種別：研究論文（学術雑誌）出版者・発行元：Frontiers Media SA

The Atacama Large Millimeter-submillimeter Array (ALMA), sited on the high desert plains of Chajnantor in Chile, has opened a new window onto solar physics in 2016 by providing continuum observations at millimeter and sub-millimeter wavelengths with an angular resolution comparable to that available at optical (O), ultraviolet (UV), extreme ultraviolet (EUV), and X-ray wavelengths, and with superior time resolution. In the intervening years, progress has been made testing and commissioning new observing modes and capabilities, in developing data calibration strategies, and in data imaging and restoration techniques. Here we review ALMA current solar observing capabilities, the process by which a user may propose to use the instrument, and summarize the observing process and work flow. We then discuss some of the challenges users may encounter in imaging and analyzing their data. We conclude with a discussion of additional solar observing capabilities and modes under consideration that are intended to further exploit the unique spectral coverage provided by ALMA.

DOI： 10.3389/fspas.2022.977368

Magnetohydrodynamic simulation of coronal mass ejections using interplanetary scintillation data observed from radio sites ISEE and LOFAR 査読有り

Kazumasa Iwai, Richard A. Fallows, Mario M. Bisi, Daikou Shiota, Bernard V. Jackson, Munetoshi Tokumaru, Ken'ichi Fujiki

Advances in Space Research 2022年9月

Application of novel interplanetary scintillation visualisations using LOFAR: A case study of merged CMEs from September 2017 査読有り

R.A. Fallows, K. Iwai, B.V. Jackson, P. Zhang, M.M. Bisi, P. Zucca

Advances in Space Research 2022年9月

Over seven decades of solar microwave data obtained with Toyokawa and Nobeyama Radio Polarimeters 査読有り

Masumi Shimojo, Kazumasa Iwai

Geoscience Data Journal 2022年6月

Testing the Alfvén-wave Model of the Solar Wind with Interplanetary Scintillation 査読有り

Munehito Shoda, Kazumasa Iwai, Daikou Shiota

The Astrophysical Journal 928 巻 ( 2 ) 頁： 130 - 130 2022年4月

掲載種別：研究論文（学術雑誌）出版者・発行元：American Astronomical Society

Abstract

Understanding the mechanism(s) of solar wind acceleration is important in astrophysics and geophysics. A promising model of solar wind acceleration is known as the wave/turbulence-driven (WTD) model, in which Alfvén waves feed energy to the solar wind. In this study, we tested the WTD model with global measurements of wind speed from interplanetary scintillation (IPS) observations. For Carrington rotations in minimal and maximal activity phases, we selected field lines calculated by the potential-field source-surface method in high and midlatitudes and compared the simulated and observed wind velocities. The simulation was performed in a self-consistent manner by solving the magnetohydrodynamic equations from the photosphere to the solar wind. In high-latitude regions, the simulated solar wind velocity agrees better with the IPS observation than with the classical Wang–Sheeley empirical estimation, both in maximal and minimal activity phases. In midlatitude regions, the agreement worsens, possibly because of the inaccuracy of the WTD model and/or the magnetic-field extrapolation. Our results indicate that the high-latitude solar wind is likely to be driven by waves and turbulence and that the physics-based prediction of the solar wind velocity is highly feasible with an improved magnetic-field extrapolation.

DOI： 10.3847/1538-4357/ac581e

その他リンク： https://iopscience.iop.org/article/10.3847/1538-4357/ac581e/pdf

Global Distribution of the Solar Wind Speed Reconstructed from Improved Tomographic Analysis of Interplanetary Scintillation Observations between 1985 and 2019 査読有り

Munetoshi Tokumaru, Ken'ichi Fujiki, Masayoshi Kojima, Kazumasa Iwai

ASTROPHYSICAL JOURNAL 922 巻 ( 1 ) 2021年11月

記述言語：英語掲載種別：研究論文（学術雑誌）出版者・発行元：IOP Publishing Ltd

Computer-assisted tomography (CAT) for interplanetary scintillation (IPS) observations enables the determination of the global distribution of solar wind speed. We compared solar wind speeds derived from the CAT analysis of IPS observations between 1985 and 2019 with in situ observations conducted by the near-Earth and Ulysses spacecraft. From this comparison, we found that solar wind speeds from the IPS observations for 2009-2019 were systematically higher than the in situ observations, whereas those for the period until 2008 were in good agreement with the in situ observations. Further, we found that the discrepancy between IPS and the in situ observations is improved by changing the power index of the empirical relation between the solar wind speed and density fluctuations. The CAT analysis using an optimal value for the power index determined from the comparison between IPS and in situ observations revealed long-term variations in the solar wind speed distribution over three cycles, leading to a better understanding of the time-varying global heliosphere. We found that polar solar winds become highly anisotropic at the Cycle 24/25 minimum, which is a peculiar aspect of this minimum. The IPS observations showed general agreement with the Parker Solar Probe observations around the perihelion of Orbit 1; this supports the reliability of the CAT analysis. The results of this study suggest that the physical properties of solar wind microturbulence may vary with a long-term decline in the solar activity, which provides important implication on the solar wind acceleration.

DOI： 10.3847/1538-4357/ac1862

BepiColombo’s Cruise Phase: Unique Opportunity for Synergistic Observations 査読有り

L. Z. Hadid, V. Génot, S. Aizawa, A. Milillo, J. Zender, G. Murakami, J. Benkhoff, I. Zouganelis, T. Alberti, N. André, Z. Bebesi, F. Califano, A. P. Dimmock, M. Dosa, C. P. Escoubet, L. Griton, G. C. Ho, T. S. Horbury, K. Iwai, M. Janvier, E. Kilpua, B. Lavraud, A. Madar, Y. Miyoshi, D. Müller, R. F. Pinto, A. P. Rouillard, J. M. Raines, N. Raouafi, F. Sahraoui, B. Sánchez-Cano, D. Shiota, R. Vainio, A. Walsh

Frontiers in Astronomy and Space Sciences 8 巻 2021年9月

掲載種別：研究論文（学術雑誌）出版者・発行元：Frontiers Media SA

The investigation of multi-spacecraft coordinated observations during the cruise phase of BepiColombo (ESA/JAXA) are reported, with a particular emphasis on the recently launched missions, Solar Orbiter (ESA/NASA) and Parker Solar Probe (NASA). Despite some payload constraints, many instruments onboard BepiColombo are operating during its cruise phase simultaneously covering a wide range of heliocentric distances (0.28 AU–0.5 AU). Hence, the various spacecraft configurations and the combined in-situ and remote sensing measurements from the different spacecraft, offer unique opportunities for BepiColombo to be part of these unprecedented multipoint synergistic observations and for potential scientific studies in the inner heliosphere, even before its orbit insertion around Mercury in December 2025. The main goal of this report is to present the coordinated observation opportunities during the cruise phase of BepiColombo (excluding the planetary flybys). We summarize the identified science topics, the operational instruments, the method we have used to identify the windows of opportunity and discuss the planning of joint observations in the future.

DOI： 10.3389/fspas.2021.718024

Venus's induced magnetosphere during active solar wind conditions at BepiColombo's Venus 1 flyby 査読有り

Martin Volwerk, Beatriz Sanchez-Cano, Daniel Heyner, Sae Aizawa, Nicolas Andre, Ali Varsani, Johannes Mieth, Stefano Orsini, Wolfgang Baumjohann, David Fischer, Yoshifumi Futaana, Richard Harrison, Harald Jeszenszky, Iwai Kazumasa, Gunter Laky, Herbert Lichtenegger, Anna Milillo, Yoshizumi Miyoshi, Rumi Nakamura, Ferdinand Plaschke, Ingo Richter, Sebastian Rojas Mata, Yoshifumi Saito, Daniel Schmid, Daikou Shiota, Cyril Simon Wedlund

ANNALES GEOPHYSICAE 39 巻 ( 5 ) 頁： 811 - 831 2021年9月

記述言語：英語掲載種別：研究論文（学術雑誌）出版者・発行元：COPERNICUS GESELLSCHAFT MBH

Out of the two Venus flybys that BepiColombo uses as a gravity assist manoeuvre to finally arrive at Mercury, the first took place on 15 October 2020. After passing the bow shock, the spacecraft travelled along the induced magnetotail, crossing it mainly in the Yvso direction. In this paper, the BepiColombo Mercury Planetary Orbiter Magnetometer (MPO-MAG) data are discussed, with support from three other plasma instruments: the Planetary Ion Camera (SERENA-PICAM) of the SERENA suite, the Mercury Electron Analyser (MEA), and the BepiColombo Radiation Monitor (BERM). Behind the bow shock crossing, the magnetic field showed a draping pattern consistent with field lines connected to the interplanetary magnetic field wrapping around the planet. This flyby showed a highly active magnetotail, with e.g. strong flapping motions at a period of similar to 7 min This activity was driven by solar wind conditions. Just before this flyby, Venus's induced magnetosphere was impacted by a stealth coronal mass ejection, of which the trailing side was still interacting with it during the flyby. This flyby is a unique opportunity to study the full length and structure of the induced magnetotail of Venus, indicating that the tail was most likely still present at about 48 Venus radii.

DOI： 10.5194/angeo-39-811-2021

PSTEP: project for solar-terrestrial environment prediction 査読有り

Kanya Kusano, Kiyoshi Ichimoto, Mamoru Ishii, Yoshizumi Miyoshi, Shigeo Yoden, Hideharu Akiyoshi, Ayumi Asai, Yusuke Ebihara, Hitoshi Fujiwara, Tada-Nori Goto, Yoichiro Hanaoka, Hisashi Hayakawa, Keisuke Hosokawa, Hideyuki Hotta, Kornyanat Hozumi, Shinsuke Imada, Kazumasa Iwai, Toshihiko Iyemori, Hidekatsu Jin, Ryuho Kataoka, Yuto Katoh, Takashi Kikuchi, Yuki Kubo, Satoshi Kurita, Haruhisa Matsumoto, Takefumi Mitani, Hiroko Miyahara, Yasunobu Miyoshi, Tsutomu Nagatsuma, Aoi Nakamizo, Satoko Nakamura, Hiroyuki Nakata, Naoto Nishizuka, Yuichi Otsuka, Shinji Saito, Susumu Saito, Takashi Sakurai, Tatsuhiko Sato, Toshifumi Shimizu, Hiroyuki Shinagawa, Kazuo Shiokawa, Daikou Shiota, Takeshi Takashima, Chihiro Tao, Shin Toriumi, Satoru Ueno, Kyoko Watanabe, Shinichi Watari, Seiji Yashiro, Kohei Yoshida, Akimasa Yoshikawa

EARTH PLANETS AND SPACE 73 巻 ( 1 ) 2021年8月

記述言語：英語掲載種別：研究論文（学術雑誌）出版者・発行元：SPRINGER

Although solar activity may significantly impact the global environment and socioeconomic systems, the mechanisms for solar eruptions and the subsequent processes have not yet been fully understood. Thus, modern society supported by advanced information systems is at risk from severe space weather disturbances. Project for solar-terrestrial environment prediction (PSTEP) was launched to improve this situation through synergy between basic science research and operational forecast. The PSTEP is a nationwide research collaboration in Japan and was conducted from April 2015 to March 2020, supported by a Grant-in-Aid for Scientific Research on Innovative Areas from the Ministry of Education, Culture, Sports, Science and Technology of Japan. By this project, we sought to answer the fundamental questions concerning the solar-terrestrial environment and aimed to build a next-generation space weather forecast system to prepare for severe space weather disasters. The PSTEP consists of four research groups and proposal-based research units. It has made a significant progress in space weather research and operational forecasts, publishing over 500 refereed journal papers and organizing four international symposiums, various workshops and seminars, and summer school for graduate students at Rikubetsu in 2017. This paper is a summary report of the PSTEP and describes the major research achievements it produced.

DOI： 10.1186/s40623-021-01486-1

BepiColombo Science Investigations During Cruise and Flybys at the Earth, Venus and Mercury 査読有り

Mangano Valeria, Dosa Melinda, Franz Markus, Milillo Anna, Oliveira Joana S., Lee Yeon Joo, McKenna-Lawlor Susan, Grassi Davide, Heyner Daniel, Kozyrev Alexander S., Peron Roberto, Helbert Joern, Besse Sebastien, de la Fuente Sara, Montagnon Elsa, Zender Joe, Volwerk Martin, Chaufray Jean-Yves, Slavin James A., Krueger Harald, Maturilli Alessandro, Cornet Thomas, Iwai Kazumasa, Miyoshi Yoshizumi, Lucente Marco, Massetti Stefano, Schmidt Carl A., Dong Chuanfei, Quarati Francesco, Hirai Takayuki, Varsani Ali, Belyaev Denis, Zhong Jun, Kilpua Emilia K. J., Jackson Bernard V., Odstrcil Dusan, Plaschke Ferdinand, Vainio Rami, Jarvinen Riku, Ivanovski Stavro Lambrov, Madar Akos, Erdos Geza, Plainaki Christina, Alberti Tommaso, Aizawa Sae, Benkhoff Johannes, Murakami Go, Quemerais Eric, Hiesinger Harald, Mitrofanov Igor G., Iess Luciano, Santoli Francesco, Orsini Stefano, Lichtenegger Herbert, Laky Gunther, Barabash Stas, Moissl Richard, Huovelin Juhani, Kasaba Yasumasa, Saito Yoshifumi, Kobayashi Masanori, Baumjohann Wolfgang

SPACE SCIENCE REVIEWS 217 巻 ( 1 ) 2021年2月

Validation of coronal mass ejection arrival-time forecasts by magnetohydrodynamic simulations based on interplanetary scintillation observations 査読有り

Iwai Kazumasa, Shiota Daikou, Tokumaru Munetoshi, Fujiki Ken'ichi, Den Mitsue, Kubo Yuki

EARTH PLANETS AND SPACE 73 巻 ( 1 ) 2021年1月

Estimating the Temperature and Density of a Spicule from 100 GHz Data Obtained with ALMA 査読有り

Shimojo Masumi, Kawate Tomoko, Okamoto Takenori J., Yokoyama Takaaki, Narukagel Noriyuki, Sakao Taro, Iwai Kazumasa, Fleishman Gregory D., Shibatas Gazunari

ASTROPHYSICAL JOURNAL LETTERS 888 巻 ( 2 ) 2020年1月

Spectral Structures of Type II Solar Radio Bursts and Solar Energetic Particles 査読有り国際共著国際誌

Iwai Kazumasa, Yashiro Seiji, Nitta Nariaki V, Kubo Yuki

ASTROPHYSICAL JOURNAL 888 巻 ( 1 ) 2020年1月

Coordinated Interplanetary Scintillation Observations in Japan and Russia for Coronal Mass Ejection Events in Early September 2017 査読有り

Tokumaru Munetoshi, Fujiki Ken'ichi, Iwai Kazumasa, Tyul'bashev Sergey, Chashei Igor

SOLAR PHYSICS 294 巻 ( 7 ) 2019年7月

Development of a coronal mass ejection arrival time forecasting system using interplanetary scintillation observations 査読有り

Iwai Kazumasa, Shiota Daikou, Tokumaru Munetoshi, Fujiki Ken'ichi, Den Mitsue, Kubo Yuki

EARTH PLANETS AND SPACE 71 巻 2019年4月

Comparative Study of Microwave Polar Brightening, Coronal Holes, and Solar Wind over the Solar Poles 査読有り

Fujiki Ken'ichi, Shibasaki Kiyoto, Yashiro Seiji, Tokumaru Munetoshi, Iwai Kazumasa, Masuda Satoshi

SOLAR PHYSICS 294 巻 ( 3 ) 2019年3月

Solar Polar Brightening and Radius at 100 and 230GHz Observed by ALMA 査読有り

Selhorst Caius L., Simoes Paulo J. A., Brajsa Roman, Valio Adriana, Gimenez de Castro C. G., Costa Joaquim E. R., Menezes Fabian, Pierre Rozelot Jean, Hales Antonio S., Iwai Kazumasa, White Stephen

ASTROPHYSICAL JOURNAL 871 巻 ( 1 ) 2019年1月

Detection of Propagating Fast Sausage Waves through Detailed Analysis of a Zebra-pattern Fine Structure in a Solar Radio Burst 査読有り

Kaneda K., Misawa H., Iwai K., Masuda S., Tsuchiya F., Katoh Y., Obara T.

ASTROPHYSICAL JOURNAL LETTERS 855 巻 ( 2 ) 2018年3月

Solar ALMA Observations: Constraining the Chromosphere above Sunspots 査読有り

Loukitcheva Maria A., Iwai Kazumasa, Solanki Sami K., White Stephen M., Shimojo Masumi

ASTROPHYSICAL JOURNAL 850 巻 ( 1 ) 2017年11月

Variation of the Solar Microwave Spectrum in the Last Half Century 査読有り

Shimojo Masumi, Iwai Kazumasa, Asai Ayumi, Nozawa Satoshi, Minamidani Tetsuhiro, Saito Masao

ASTROPHYSICAL JOURNAL 848 巻 ( 1 ) 2017年10月

OCTAD-S: digital fast Fourier transform spectrometers by FPGA 査読有り

Iwai Kazumasa, Kubo Yuki, Ishibashi Hiromitsu, Naoi Takahiro, Harada Kenichi, Ema Kenji, Hayashi Yoshinori, Chikahiro Yuichi

EARTH PLANETS AND SPACE 69 巻頁： 95 2017年7月

Observing the Sun with the Atacama Large Millimeter/submillimeter Array (ALMA): Fast-Scan Single-Dish Mapping 査読有り

S. M. White, K. Iwai, N. M. Phillips, R. E. Hills, A. Hirota, P. Yagoubov, G. Siringo, M. Shimojo, T. S. Bastian, A. S. Hales, T. Sawada, S. Asayama, M. Sugimoto, R. G. Marson, W. Kawasaki, E. Muller, T. Nakazato, K. Sugimoto, R. Brajsa, I. Skokic, M. Barta, S. Kim, A. J. Remijan, I. de Gregorio, S. A. Corder, H. S. Hudson, M. Loukitcheva, B. Chen, B. De Pontieu, G. D. Fleishmann, D. E. Gary, A. Kobelski, S. Wedemeyer, Y. Yan

SOLAR PHYSICS 292 巻 ( 7 ) 2017年7月

記述言語：英語掲載種別：研究論文（学術雑誌）出版者・発行元：SPRINGER

The Atacama Large Millimeter/submillimeter Array (ALMA) radio telescope has commenced science observations of the Sun starting in late 2016. Since the Sun is much larger than the field of view of individual ALMA dishes, the ALMA interferometer is unable to measure the background level of solar emission when observing the solar disk. The absolute temperature scale is a critical measurement for much of ALMA solar science, including the understanding of energy transfer through the solar atmosphere, the properties of prominences, and the study of shock heating in the chromosphere. In order to provide an absolute temperature scale, ALMA solar observing will take advantage of the remarkable fast-scanning capabilities of the ALMA 12 m dishes to make single-dish maps of the full Sun. This article reports on the results of an extensive commissioning effort to optimize the mapping procedure, and it describes the nature of the resulting data. Amplitude calibration is discussed in detail: a path that uses the two loads in the ALMA calibration system as well as sky measurements is described and applied to commissioning data. Inspection of a large number of single-dish datasets shows significant variation in the resulting temperatures, and based on the temperature distributions, we derive quiet-Sun values at disk center of 7300 K at lambda = 3 mm and 5900 K at lambda = 1.3 mm. These values have statistical uncertainties of about 100 K, but systematic uncertainties in the temperature scale that may be significantly larger. Example images are presented from two periods with very different levels of solar activity. At a resolution of about 25 '', the 1.3 mm wavelength images show temperatures on the disk that vary over about a 2000 K range. Active regions and plages are among the hotter features, while a large sunspot umbra shows up as a depression, and filament channels are relatively cool. Prominences above the solar limb are a common feature of the single-dish images.

DOI： 10.1007/s11207-017-1123-2

ALMA Discovery of Solar Umbral Brightness Enhancement at lambda=3 mm 査読有り国際共著国際誌

Iwai Kazumasa, Loukitcheva Maria, Shimojo Masumi, Solanki Sami K., White Stephen M.

ASTROPHYSICAL JOURNAL LETTERS 841 巻 ( 2 ) 頁： L20 2017年6月

Polarization Characteristics of Zebra Patterns in Type IV Solar Radio Bursts 査読有り

Kaneda K., Misawa H., Iwai K., Tsuchiya F., Obara T., Katoh Y., Masuda S.

ASTROPHYSICAL JOURNAL 842 巻 ( 1 ) 2017年6月

The First ALMA Observation of a Solar Plasmoid Ejection from an X-Ray Bright Point 査読有り国際共著国際誌

Shimojo Masumi, Hudson Hugh S., White Stephen M., Bastian Timothy S., Iwai Kazumasa

ASTROPHYSICAL JOURNAL LETTERS 841 巻 ( 1 ) 2017年5月

The Brightness Temperature of the Quiet Solar Chromosphere at 2.6 mm 査読有り国際共著国際誌

Kazumasa Iwai, Masumi Shimojo, Shinichiro Asayama, Tetsuhiro Minamidani, Stephen White, Timothy Bastian, Masao Saito

SOLAR PHYSICS 292 巻 ( 1 ) 頁： 22 2017年1月

担当区分：筆頭著者,　責任著者記述言語：英語掲載種別：研究論文（学術雑誌）出版者・発行元：SPRINGER

The absolute brightness temperature of the Sun at millimeter wavelengths is an important diagnostic of the solar chromosphere. Because the Sun is so bright, measurement of this property usually involves the operation of telescopes under extreme conditions and requires a rigorous performance assessment of the telescope. In this study, we establish solar observation and calibration techniques at 2.6 mm wavelength for the Nobeyama 45 m telescope and accurately derive the absolute solar brightness temperature. We tune the superconductor-insulator-superconductor (SIS) receiver by inducing different bias voltages onto the SIS mixer to prevent saturation. Then, we examine the linearity of the receiver system by comparing outputs derived from different tuning conditions. Furthermore, we measure the lunar filled beam efficiency of the telescope using the New Moon, and then derive the absolute brightness temperature of the Sun. The derived solar brightness temperature is 7700 +/- 310 K at 115 GHz. The telescope beam pattern is modeled as a summation of three Gaussian functions and derived using the solar limb. The real shape of the Sun is determined via deconvolution of the beam pattern from the observed map. Such well-calibrated single-dish observations are important for high-resolution chromospheric studies because they provide the absolute temperature scale that is lacking from interferometer observations.

DOI： 10.1007/s11207-016-1044-5

Microwave observations of a large-scale coronal wave with the Nobeyama radioheliograph 査読有り

A. Warmuth, K. Shibasaki, K. Iwai, G. Mann

ASTRONOMY & ASTROPHYSICS 593 巻 2016年9月

記述言語：英語掲載種別：研究論文（学術雑誌）出版者・発行元：EDP SCIENCES S A

Context. Large-scale globally propagating waves in the solar corona have been studied extensively, mainly using extreme ultraviolet (EUV) observations. In a few events, corresponding wave signatures have been detected in microwave radioheliograms provided by the Nobeyama radioheliograph (NoRH). Several aspects of these observations seem to contradict the conclusions drawn from EUV observations.
Aims. We investigate whether the microwave observations of global waves are consistent with previous findings.
Methods. We revisited the wave of 1997 Sep. 24, which is still the best-defined event in microwaves. We obtained radioheliograms at 17 and 34 GHz from NoRH and studied the morphology, kinematics, perturbation profile evolution, and emission mechanism of the propagating microwave signatures.
Results. We find that the NoRH wave signatures are morphologically consistent with both the associated coronal wave as observed by SOHO/EIT and the Moreton wave seen in H alpha. The NoRH wave is clearly decelerating, which is typically found for large-amplitude coronal waves associated with Moreton waves, and its kinematical curve is consistent with the EIT wavefronts. The perturbation profile shows a pronounced decrease in amplitude. Based on the derivation of the spectral index of the excess microwave emission, we conclude that the NoRH wave is due to optically thick free-free bremsstrahlung from the chromosphere.
Conclusions. The wavefronts seen in microwave radioheliograms are chromospheric signatures of coronal waves, and their characteristics support the interpretation of coronal waves as large-amplitude fast-mode MHD waves or shocks.

DOI： 10.1051/0004-6361/201628591

CORONAL MAGNETIC FIELDS DERIVED FROM SIMULTANEOUS MICROWAVE AND EUV OBSERVATIONS AND COMPARISON WITH THE POTENTIAL FIELD MODEL 査読有り

Shun Miyawaki, Kazumasa Iwai, Kiyoto Shibasaki, Daikou Shiota, Satoshi Nozawa

ASTROPHYSICAL JOURNAL 818 巻 ( 1 ) 2016年2月

記述言語：英語掲載種別：研究論文（学術雑誌）出版者・発行元：IOP PUBLISHING LTD

We estimated the accuracy of coronal magnetic fields derived from radio observations by comparing them to potential field calculations and the differential emission measure measurements using EUV observations. We derived line-of-sight components of the coronal magnetic field from polarization observations of the thermal bremsstrahlung in the NOAA active region 11150, observed around 3:00 UT on 2011 February 3 using the Nobeyama Radioheliograph at 17 GHz. Because the thermal bremsstrahlung intensity at 17 GHz includes both chromospheric and coronal components, we extracted only the coronal component by measuring the coronal emission measure in EUV observations. In addition, we derived only the radio polarization component of the corona by selecting the region of coronal loops and weak magnetic field strength in the chromosphere along the line of sight. The upper limits of the coronal longitudinal magnetic fields were determined as 100-210 G. We also calculated the coronal longitudinal magnetic fields from the potential field extrapolation using the photospheric magnetic field obtained from the Helioseismic and Magnetic Imager. However, the calculated potential fields were certainly smaller than the observed coronal longitudinal magnetic field. This discrepancy between the potential and the observed magnetic field strengths can be explained consistently by two reasons:. (1) the underestimation of the coronal emission measure resulting from the limitation of the temperature range of the EUV observations, and (2) the underestimation of the coronal magnetic field resulting from the potential field assumption.

DOI： 10.3847/0004-637X/818/1/8

CHROMOSPHERIC SUNSPOTS IN THE MILLIMETER RANGE AS OBSERVED BY THE NOBEYAMA RADIOHELIOGRAPH 査読有り

Kazumasa Iwai, Hideki Koshiishi, Kiyoto Shibasaki, Satoshi Nozawa, Shun Miyawaki, Takuro Yoneya

ASTROPHYSICAL JOURNAL 816 巻 ( 2 ) 頁： 91 2016年1月

記述言語：英語掲載種別：研究論文（学術雑誌）出版者・発行元：IOP PUBLISHING LTD

We investigate the upper chromosphere and the transition region of the sunspot umbra using the radio brightness temperature at 34 GHz (corresponding to 8.8 mm observations) as observed by the Nobeyama Radioheliograph (NoRH). Radio free-free emission in the longer millimeter range is generated around the transition region, and its brightness temperature yields the region's temperature and density distribution. We use the NoRH data at 34 GHz by applying the Steer-CLEAN image synthesis. These data and the analysis method enable us to investigate the chromospheric structures in the longer millimeter range with high spatial resolution and sufficient visibilities. We also perform simultaneous observations of one sunspot using the NoRH and the Nobeyama 45 m telescope operating at 115 GHz. We determine that 115 GHz emission mainly originates from the lower chromosphere while 34 GHz emission mainly originates from the upper chromosphere and transition region. These observational results are consistent with the radio emission characteristics estimated from current atmospheric models of the chromosphere. On the other hand, the observed brightness temperature of the umbral region is almost the same as that of the quiet region. This result is inconsistent with current sunspot models, which predict a considerably higher brightness temperature of the sunspot umbra at 34 GHz. This inconsistency suggests that the temperature of the region at which the 34 GHz radio emission becomes optically thick should be lower than that predicted by the models.

DOI： 10.3847/0004-637X/816/2/91

FREQUENCY DEPENDENCE OF POLARIZATION OF ZEBRA PATTERN IN TYPE-IV SOLAR RADIO BURSTS 査読有り

Kazutaka Kaneda, H. Misawa, K. Iwai, F. Tsuchiya, T. Obara

ASTROPHYSICAL JOURNAL LETTERS 808 巻 ( 2 ) 2015年8月

記述言語：英語掲載種別：研究論文（学術雑誌）出版者・発行元：IOP PUBLISHING LTD

We investigated the polarization characteristics of a zebra pattern (ZP) in a type-IV solar radio burst observed with AMATERAS on 2011 June 21 for the purpose of evaluating the generation processes of ZPs. Analyzing highly resolved spectral and polarization data revealed the frequency dependence of the degree of circular polarization and the delay between two polarized components for the first time. The degree of circular polarization was 50%-70% right-handed and it varied little as a function of frequency. Cross-correlation analysis determined that the left-handed circularly polarized component was delayed by 50-70 ms relative to the right-handed component over the entire frequency range of the ZP and this delay increased with the frequency. We examined the obtained polarization characteristics by using pre-existing ZP models and concluded that the ZP was generated by the double-plasma-resonance process. Our results suggest that the ZP emission was originally generated in a completely polarized state in the O-mode and was partly converted into the X-mode near the source. Subsequently, the difference between the group velocities of the O-mode and X-mode caused the temporal delay.

DOI： 10.1088/2041-8205/808/2/L45

SOLAR MICRO-TYPE III BURST STORMS AND LONG DIPOLAR MAGNETIC FIELD IN THE OUTER CORONA 査読有り

A. Morioka, Y. Miyoshi, K. Iwai, Y. Kasaba, S. Masuda, H. Misawa, T. Obara

ASTROPHYSICAL JOURNAL 808 巻 ( 2 ) 2015年8月

記述言語：英語掲載種別：研究論文（学術雑誌）出版者・発行元：IOP PUBLISHING LTD

Solar micro-type III radio bursts are elements of the so-called type III storms and are characterized by short-lived, continuous, and weak emissions. Their frequency of occurrence with respect to radiation power is quite different from that of ordinary type III bursts, suggesting that the generation process is not flare-related, but due to some recurrent acceleration processes around the active region. We examine the relationship of micro-type III radio bursts with coronal streamers. We also explore the propagation channel of bursts in the outer corona, the acceleration process, and the escape route of electron beams. It is observationally confirmed that micro-type III bursts occur near the edge of coronal streamers. The magnetic field line of the escaping electron beams is tracked on the basis of the frequency drift rate of micro-type III bursts and the electron density distribution model. The results demonstrate that electron beams are trapped along closed dipolar field lines in the outer coronal region, which arise from the interface region between the active region and the coronal hole. A 22 year statistical study reveals that the apex altitude of the magnetic loop ranges from 15 to 50 R-S. The distribution of the apex altitude has a sharp upper limit around 50 RS suggesting that an unknown but universal condition regulates the upper boundary of the streamer dipolar field.

DOI： 10.1088/0004-637X/808/2/191

OBSERVATION OF THE CHROMOSPHERIC SUNSPOT AT MILLIMETER RANGE WITH THE NOBEYAMA 45 m TELESCOPE 査読有り

Kazumasa Iwai, Masumi Shimojo

ASTROPHYSICAL JOURNAL 804 巻 ( 1 ) 頁： 48 2015年5月

記述言語：英語掲載種別：研究論文（学術雑誌）出版者・発行元：IOP PUBLISHING LTD

The brightness temperature of the radio free-free emission at millimeter range is an effective tool for characterizing the vertical structure of the solar chromosphere. In this paper, we report on the first single-dish observation of a sunspot at 85 and 115 GHz with sufficient spatial resolution for resolving the sunspot umbra using the Nobeyama 45 m telescope. We used radio attenuation material, i.e., a solar filter, to prevent the saturation of the receivers. Considering the contamination from the plage by the side lobes, we found that the brightness temperature of the umbra should be lower than that of the quiet region. This result is inconsistent with the preexisting atmospheric models. We also found that the brightness temperature distribution at millimeter range strongly corresponds to the ultraviolet continuum emission at 1700 angstrom, especially at the quiet region.

DOI： 10.1088/0004-637X/804/1/48

Coronal magnetic field and the plasma beta determined from radio and multiple satellite observations 招待有り査読有り

Iwai Kazumasa, Shibasaki, K., Nozawa, S., Takahashi, T., Sawada, S., Kitagawa, J., Miyawaki, S. and Kashiwagi, H.

Earth Planets and Space 66 巻頁： 149 2014年11月

SPECTRAL STRUCTURES AND THEIR GENERATION MECHANISMS FOR SOLAR RADIO TYPE-I BURSTS 査読有り

K. Iwai, Y. Miyoshi, S. Masuda, F. Tsuchiya, A. Morioka, H. Misawa

ASTROPHYSICAL JOURNAL 789 巻 ( 1 ) 頁： 4 2014年7月

記述言語：英語掲載種別：研究論文（学術雑誌）出版者・発行元：IOP PUBLISHING LTD

The fine spectral structures of solar radio type-I bursts were observed by the solar radio telescope AMATERAS. The spectral characteristics, such as the peak flux, duration, and bandwidth, of the individual burst elements were satisfactorily detected by the highly resolved spectral data of AMATERAS with the burst detection algorithm that is improved in this study. The peak flux of the type-I bursts followed a power-law distribution with a spectral index of 2.9-3.3, whereas their duration and bandwidth were distributed more exponentially. There were almost no correlations between the peak flux, duration, and bandwidth. That means there was no similarity in the shapes of the burst spectral structures. We defined the growth rate of a burst as the ratio between its peak flux and duration. There was a strong correlation between the growth rate and peak flux. These results suggest that the free energy of type-I bursts that is originally generated by nonthermal electrons is modulated in the subsequent stages of the generation of nonthermal electrons, such as plasma wave generation, radio wave emissions, and propagation. The variation of the timescale of the growth rate is significantly larger than that of the coronal environments. These results can be explained by the situation wherein the source region may have the inhomogeneity of an ambient plasma environment, such as the boundary of open and closed field lines, and the superposition of entire emitted bursts was observed by the spectrometer.

DOI： 10.1088/0004-637X/789/1/4

GENERATION MECHANISM OF THE SLOWLY DRIFTING NARROWBAND STRUCTURE IN THE TYPE IV SOLAR RADIO BURSTS OBSERVED BY AMATERAS 査読有り

Y. Katoh, K. Iwai, Y. Nishimura, A. Kumamoto, H. Misawa, F. Tsuchiya, T. Ono

ASTROPHYSICAL JOURNAL 787 巻 ( 1 ) 2014年5月

記述言語：英語掲載種別：研究論文（学術雑誌）出版者・発行元：IOP PUBLISHING LTD

We investigate the type IV burst event observed by AMATERAS on 2011 June 7, and reveal that the main component of the burst was emitted from the plasmoid eruption identified in the EUV images of the Solar Dynamics Observatory (SDO)/AIA. We show that a slowly drifting narrowband structure (SDNS) appeared in the burst's spectra. Using statistical analysis, we reveal that the SDNS appeared for a duration of tens to hundreds of milliseconds and had a typical bandwidth of 3 MHz. To explain the mechanism generating the SDNS, we propose wave-wave coupling between Langmuir waves and whistler-mode chorus emissions generated in a post-flare loop, which were inferred from the similarities in the plasma environments of a post-flare loop and the equatorial region of Earth's inner magnetosphere. We assume that a chorus element with a rising tone is generated at the top of a post-flare loop. Using the magnetic field and plasma density models, we quantitatively estimate the expected duration of radio emissions generated from coupling between Langmuir waves and chorus emissions during their propagation in the post-flare loop, and we find that the observed duration and bandwidth properties of the SDNS are consistently explained by the proposed generation mechanism. While observations in the terrestrial magnetosphere show that the chorus emissions are a group of large-amplitude wave elements generated naturally and intermittently, the mechanism proposed in the present study can explain both the intermittency and the frequency drift in the observed spectra.

DOI： 10.1088/0004-637X/787/1/45

Measurements of Coronal and Chromospheric Magnetic Fields Using Polarization Observations by the Nobeyama Radioheliograph 査読有り

Kazumasa Iwai, Kiyoto Shibasaki

PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN 65 巻 ( SP1 ) 頁： S14 2013年12月

記述言語：英語掲載種別：研究論文（学術雑誌）出版者・発行元：OXFORD UNIV PRESS

Coronal and chromospheric magnetic fields are derived from polarization and spectral observations of the thermal free free emission using the Nobeyama Radioheliograph (NoRH). In magnetized plasma, the ordinary and extraordinary modes of free free emission have different optical depths. This creates a circularly polarized component in an atmosphere with a temperature gradient. We observed an active region on 2012 April 13 to derive its coronal and chromospheric magnetic fields. The observed degree of circular polarization was between 0.5% and 1.7%. The radio circular polarization images were compared with ultraviolet images observed by the Atmospheric Imaging Assembly and the photospheric magnetic field observed by the Helioseismic and Magnetic Imager, both on board the Solar Dynamic Observatory. At the edge of the active region, the radio circular polarization was emitted mainly from coronal loops, and the coronal magnetic field was derived to be about 70 G. At the center of the active region, the chromospheric and coronal components cannot be separated. The derived magnetic field is about 20% to 50% of the corresponding photospheric magnetic field, which is an emission-measure-weighted average of the coronal and chromospheric magnetic fields.

DOI： 10.1093/pasj/65.sp1.S14

PEAK FLUX DISTRIBUTIONS OF SOLAR RADIO TYPE-I BURSTS FROM HIGHLY RESOLVED SPECTRAL OBSERVATIONS 査読有り

K. Iwai, S. Masuda, Y. Miyoshi, F. Tsuchiya, A. Morioka, H. Misawa

ASTROPHYSICAL JOURNAL LETTERS 768 巻 ( 1 ) 頁： L2 2013年5月

記述言語：英語掲載種別：研究論文（学術雑誌）出版者・発行元：IOP PUBLISHING LTD

Solar radio type-I bursts were observed on 2011 January 26 by high resolution observations with the radio telescope AMATERAS in order to derive their peak flux distributions. We have developed a two-dimensional auto burst detection algorithm that can distinguish each type-I burst element from complex noise storm spectra that include numerous instances of radio frequency interference (RFI). This algorithm removes RFI from the observed radio spectra by applying a moving median filter along the frequency axis. Burst and continuum components are distinguished by a two-dimensional maximum and minimum search of the radio dynamic spectra. The analysis result shows that each type-I burst element has one peak flux without double counts or missed counts. The peak flux distribution of type-I bursts derived using this algorithm follows a power law with a spectral index between 4 and 5.

DOI： 10.1088/2041-8205/768/1/L2

IPRT/AMATERAS: A New Metric Spectrum Observation System for Solar Radio Bursts 査読有り

K. Iwai, F. Tsuchiya, A. Morioka, H. Misawa

SOLAR PHYSICS 277 巻 ( 2 ) 頁： 447 - 457 2012年4月

記述言語：英語掲載種別：研究論文（学術雑誌）出版者・発行元：SPRINGER

A new radio spectropolarimeter for solar radio observation has been developed at Tohoku University and installed on the Iitate Planetary Radio Telescope (IPRT) at the Iitate observatory in Fukushima prefecture, Japan. This system, named AMATERAS (the Assembly of Metric-band Aperture TElescope and Real-time Analysis System), enables us to observe solar radio bursts in the frequency range between 150 and 500 MHz. The minimum detectable flux in the observation frequency range is less than 0.7 SFU with an integration time of 10 ms and a bandwidth of 61 kHz. Both left and right polarization components are simultaneously observed in this system. These specifications are accomplished by combining the large aperture of IPRT with a high-speed digital receiver. Observational data are calibrated and archived soon after the daily observation. The database is available online. The high-sensitivity observational data with the high time and frequency resolutions from AMATERAS will be used to analyze spectral fine structures of solar radio bursts.

DOI： 10.1007/s11207-011-9919-y

SOLAR RADIO TYPE-I NOISE STORM MODULATED BY CORONAL MASS EJECTIONS 査読有り

K. Iwai, Y. Miyoshi, S. Masuda, M. Shimojo, D. Shiota, S. Inoue, F. Tsuchiya, A. Morioka, H. Misawa

ASTROPHYSICAL JOURNAL 744 巻 ( 2 ) 頁： 167 2012年1月

記述言語：英語掲載種別：研究論文（学術雑誌）出版者・発行元：IOP PUBLISHING LTD

The first coordinated observations of an active region using ground-based radio telescopes and the Solar Terrestrial Relations Observatory (STEREO) satellites from different heliocentric longitudes were performed to study solar radio type-I noise storms. A type-I noise storm was observed between 100 and 300 MHz during a period from 2010 February 6 to 7. During this period the two STEREO satellites were located approximately 65. (ahead) and -70 degrees (behind) from the Sun-Earth line, which is well suited to observe the earthward propagating coronal mass ejections (CMEs). The radio flux of the type-I noise storm was enhanced after the preceding CME and began to decrease before the subsequent CME. This time variation of the type-I noise storm was directly related to the change of the particle acceleration processes around its source region. Potential-field source-surface extrapolation from the Solar and Heliospheric Observatory/ Michelson Doppler Imager (SOHO/ MDI) magnetograms suggested that there was a multipolar magnetic system around the active region from which the CMEs occurred around the magnetic neutral line of the system. From our observational results, we suggest that the type-I noise storm was activated at a side-lobe reconnection region that was formed after eruption of the preceding CME. This magnetic structure was deformed by a loop expansion that led to the subsequent CME, which then suppressed the radio burst emission.

DOI： 10.1088/0004-637X/744/2/167

　前のページ - 次のページ　

1