Author name code: otsuji ADS astronomy entries on 2022-09-14 author:"Otsuji, Kenichi" ------------------------------------------------------------------------ Title: Universal Correlation between the Ejected Mass and Total Flare Energy for Solar and Stellar Cold Plasma Ejection Authors: Kotani, Yuji; Otsuji, Kenichi; Shibata, Kazunari; Asai, Ayumi; Ichimoto, Kiyoshi; Ishii, Takako; Yamasaki, Daiki Bibcode: 2022cosp...44.2450K Altcode: We often find spectral signatures of chromospheric plasma ejections accompanied by flares in various spatial scales in the solar and stellar atmospheres. Similar spectral signatures are found regardless of their wide range of scale. However, no physical quantities such as mass and energy have been estimated for flare energies covering over 10 orders of magnitude until now. In this study, we analyzed the spectra of cold plasma ejections associated with flares by performing H$\alpha$ imaging spectroscopy of the solar full-disk with SMART/SDDI. We determined the ejected mass by cloud model fitting to the H$\alpha$ spectrum. We estimated flare energy by DEM analysis using SDO/AIA for small-scale flares and by estimating the bolometric energy for large-scale flares. In addition, we constructed a scaling law for the total flare energy and the ejected mass and compared it with our observation. The results are in good agreement with the scaling law for small mass ejections with small flares in the quiet region for a coronal field strength of 5 G and filament eruptions with flares for that of 5 - 50 G. We also compared it with the observations interpreted as stellar filament eruptions, and found that they were roughly consistent with the scaling law. These results suggest that cold plasma ejections with flares taking place on the sun and stars in a wide range of the energy scale are caused by a common mechanism. Title: Development of CHARMS (charging and radiation monitors for space weather) instruments for follow-on Japanese geostationary meteorological satellite Authors: Sakaguchi, Kaori; Nagatsuma, Tsutomu; Takashima, Takeshi; Otsuji, Kenichi; Tsugawa, Takuya; Ishii, Mamoru; Mitani, Takefumi; Saito, Shinji; Kubo, Yuki; Hozumi, Yuta; Miyake, Hiroaki; Enoki, Kaisei Bibcode: 2022cosp...44.3548S Altcode: CHARMS (charging and radiation monitors for space weather) is a suite of sensors measuring energetic electrons (50 keV - 5 MeV) and protons (10 MeV - 1 GeV), and spacecraft internal charging. It started to be developed as a hosted payload of follow-on geostationary meteorological satellite of Japan as know Himawari. CHARMS aims to monitor the outer radiation belt electrons, solar and galactic protons, that are hazard to spacecraft operation and radiation exposure of astronauts and aircrews. To mitigate these risks from space environment hazard, the space weather forecast service group of the National Institute of Information and Communications Technology (NICT) plans to utilize the CHARMS product issuing forecasts and prompt warnings for space weather users as well as general public. The necessity of operational space weather monitoring in space is increasingly with the expansion of space utilization, including social infrastructure, such as navigation, communication, and broadcasting. CHARMS will be responsible for operational space-based in-situ observations in geostationary orbit over Japan after launch scheduled in 2028. Current status of CHARMS instruments development is introduced in our presentation. Title: Relationship between three-dimensional velocity of filament eruptions and CME association Authors: Seki, Daikichi; Otsuji, Kenichi; Ishii, Takako T.; Asai, Ayumi; Ichimoto, Kiyoshi Bibcode: 2021EP&S...73...58S Altcode: 2021arXiv210204578S It is widely recognised that filament disappearances or eruptions are frequently associated with Coronal Mass Ejections (CMEs). Since CMEs are a major source of disturbances of the space environment surrounding the Earth, it is important to investigate these associations in detail for the better prediction of CME occurrence. However, the proportion of filament disappearances associated with CMEs is under debate. The estimates range from ∼ 10 to ∼ 90% and could be affected by the manners to select the events. In this study, we aim to reveal what parameters control the association between filament eruptions and CMEs. We analysed the relationships between CME associations and the physical parameters of filaments including their length, maximum ascending velocity, and direction of eruptions using 28 events of filament eruptions observed in Hα . We found that the product of the maximum radial velocity and the filament length is well correlated with the CME occurrence. If the product is larger than 8.0 ×106 km2s-1, the filament will become a CME with a probability of 93%, and if the product is smaller than this value, it will not become a CME with a probability of 100%. We suggest a kinetic-energy threshold above which filament eruptions are associated with CMEs. Our findings also suggest the importance of measuring the velocity vector of filament eruption in three-dimensional space for the better prediction of CME occurrence. Title: Small-scale Turbulent Motion of the Plasma in a Solar Filament as the Precursor of Eruption Authors: Seki, Daikichi; Otsuji, Kenichi; Isobe, Hiroaki; Del Zanna, Giulio; Ishii, Takako T.; Sakaue, Takahito; Ichimoto, Kiyoshi; Shibata, Kazunari Bibcode: 2021ApJ...918...38S Altcode: 2021arXiv210611875S A filament, a dense cool plasma supported by the magnetic fields in the solar corona, often becomes unstable and erupts. It is empirically known that the filament often demonstrates some activations such as a turbulent motion prior to eruption. In our previous study, we analyzed the Doppler velocity of an Hα filament and found that the standard deviation of the line-of-sight velocity distribution in a filament, which indicates the increasing amplitude of the small-scale motions, increased prior to the onset of the eruption. Here, we present a further analysis on this filament eruption, which initiated approximately at 03:40 UT on 2016 November 5 in the vicinity of NOAA Active Region 12605. It includes a coronal line observation and the extrapolation of the surrounding magnetic fields. We found that both the spatially averaged microturbulence inside the filament and the nearby coronal line emission increased 6 and 10 hr prior to eruption, respectively. In this event, we did not find any significant changes in the global potential field configuration preceding the eruption for the past 2 days, which indicates that there is a case in which it is difficult to predict the eruption only by tracking the extrapolated global magnetic fields. In terms of space weather prediction, our result on the turbulent motions in a filament could be used as the useful precursor of a filament eruption. Title: A three-dimensional velocity of an erupting prominence prior to a coronal mass ejection Authors: Gutierrez, Maria V.; Otsuji, Kenichi; Asai, Ayumi; Terrazas, Raul; Ishitsuka, Mutsumi; Ishitsuka, Jose; Nakamura, Naoki; Yoshinaga, Yusuke; Morita, Satoshi; Ishii, Takako T.; Ueno, Satoru; Kitai, Reizaburo; Shibata, Kazunari Bibcode: 2021PASJ...73..394G Altcode: 2021arXiv210108575G; 2021PASJ..tmp...23G We present a detailed three-dimensional (3D) view of a prominence eruption, coronal loop expansion, and coronal mass ejections (CMEs) associated with an M4.4 flare that occurred on 2011 March 8 in the active region NOAA 11165. Full-disk Hα images of the flare and filament ejection were successfully obtained by the Flare Monitoring Telescope (FMT) following its relocation to Ica University, Peru. Multiwavelength observation around the Hα line enabled us to derive the 3D velocity field of the Hα prominence eruption. Features in extreme ultraviolet were also obtained by the Atmospheric Imager Assembly onboard the Solar Dynamic Observatory and the Extreme Ultraviolet Imager on board the Solar Terrestrial Relations Observatory - Ahead satellite. We found that, following collision of the erupted filament with the coronal magnetic field, some coronal loops began to expand, leading to the growth of a clear CME. We also discuss the succeeding activities of CME driven by multiple interactions between the expanding loops and the surrounding coronal magnetic field. Title: Development of new tunable filter for solar observation in Hida observatory Authors: Otsuji, Kenichi; Kimura, Gouichi; Nakatani, Yoshi-kazu; Kaneda, Naoki; Ishii, Takako T.; Hagino, Masaoki; Ichimoto, Kiyoshi Bibcode: 2020SPIE11447E..A5O Altcode: Solar Magnetic Activity Research Telescope (SMART) at Hida observatory is in operational to monitor the solar activity. As a new solar Hα observing instrument for SMART, we developed "Solar Dynamics Doppler Imager (SDDI)", which can measure the three-dimensional motion of solar eruptive phenomena. These eruptive events could be affective to the earth magnetism and cause serious damage to our society. The purpose of SMART/SDDI is monitoring and forecasting the geo-affective solar eruptions. In this paper, we present the development of the tunable filter "F40", the key component of SDDI. The features of TF40 are, (1) fast tuning of observation wavelength, (2) narrow transmission width and large free spectral range (FSR), (3) large field-of-view that covers the entire solar disk with a 20 cm objective lens. TF40 has 7 stages of optical blocks. Each stage consists of a linear polarizer, calcites, a quartz as half waveplate and a Liquid Crystal Variable Retarder (LCVR), and has the periodic transmission profile with 0.05, 0.1, 0.2, 0.4, 0.8, 1.6 and 3.2 nm period at Hα line (656.2808 nm), respectively. Combining the 7 stages, the 0.025 nm transmission width and 3.2 nm FSR are achieved. Retardation of each LCVR and its dependence on applied voltage and temperature were measured for modeling its characteristics, with which we calculate the voltage for desired retardation. Best-shaped transmission profile is obtained by further adjustment of voltages of individual LCVRs using the real solar light. We report the performance and current observing status of the TF40. Title: Synoptic solar observations of the Solar Flare Telescope focusing on space weather Authors: Hanaoka, Yoichiro; Sakurai, Takashi; Otsuji, Ken'ichi; Suzuki, Isao; Morita, Satoshi Bibcode: 2020JSWSC..10...41H Altcode: 2020arXiv200714054H The solar group at the National Astronomical Observatory of Japan is conducting synoptic solar observation with the Solar Flare Telescope. While it is a part of a long-term solar monitoring, contributing to the study of solar dynamo governing solar activity cycles, it is also an attempt at contributing to space weather research. The observations include imaging with filters for Hα, Ca K, G-band, and continuum, and spectropolarimetry at the wavelength bands including the He I 1083.0 nm/Si I 1082.7 nm and the Fe I 1564.8 nm lines. Data for the brightness, Doppler signal, and magnetic field information of the photosphere and the chromosphere are obtained. In addition to monitoring dynamic phenomena like flares and filament eruptions, we can track the evolution of the magnetic fields that drive them on the basis of these data. Furthermore, the magnetic field in solar filaments, which develops into a part of the interplanetary magnetic cloud after their eruption and occasionally hits the Earth, can be inferred in its pre-eruption configuration. Such observations beyond mere classical monitoring of the Sun will hereafter become crucially important from the viewpoint of the prediction of space weather phenomena. The current synoptic observations with the Solar Flare Telescope is considered to be a pioneering one for future synoptic observations of the Sun with advanced instruments. Title: SMART/SDDI Filament Disappearance Catalogue Authors: Seki, Daikichi; Otsuji, Kenichi; Ishii, Takako T.; Hirose, Kumi; Iju, Tomoya; UeNo, Satoru; Cabezas, Denis P.; Asai, Ayumi; Isobe, Hiroaki; Ichimoto, Kiyoshi; Shibata, Kazunari Bibcode: 2020arXiv200303454S Altcode: This paper describes a new SMART/SDDI Filament Disappearance Catalogue, in which we listed almost all the filament disappearance events that the Solar Dynamics Doppler Imager (SDDI) has observed since its installation on the Solar Magnetic Activity Research Telescope (SMART) in May 2016. Our aim is to build a database that can help predict the occurrence and severity of coronal mass ejections (CMEs). The catalogue contains miscellaneous information associated with filament disappearance such as flare, CME, active region, three-dimensional trajectory of erupting filaments, detection in Interplanetary Scintillation (IPS), occurrence of interplanetary CME (ICME) and Dst index. We also provide statistical information on the catalogue data. The catalogue is available from the following website: https://www.kwasan.kyoto-u.ac.jp/observation/event/sddi-catalogue/. Title: SMART/SDDI Filament Disappearance Catalogue Authors: Seki, D.; Otsuji, K.; Ishii, T.; Hirose, K.; Iju, T.; UeNo, S.; Cabezas, D.; Asai, A.; Isobe, H.; Ichimoto, K.; Shibata, K. Bibcode: 2019SunGe..14...95S Altcode: This paper describes a new "SMART/SDDI Filament Disappearance Catalogue," in which we listed almost all the filament disappearance events that the Solar Dynamics Doppler Imager (SDDI) has observed since its installation on the Solar Magnetic Activity Research Telescope (SMART) in May 2016. Our aim is to build a database that can help predict the occurrence and severity of coronal mass ejections (CMEs). The catalogue contains miscellaneous information associated with filament disappearance such as flare, CME, active region, three-dimensional trajectory of erupting filaments, detection in Interplanetary Scintillation (IPS), occurrence of interplanetary CME (ICME) and Dst index. We also provide statistical information on the catalogue data. The catalogue is available from the following website: https://www.kwasan.kyoto-u.ac.jp/observation/event/sddi-catalogue/. Title: Small-scale motions in solar filaments as the precursors of eruptions Authors: Seki, Daikichi; Otsuji, Kenichi; Isobe, Hiroaki; Ishii, Takako T.; Ichimoto, Kiyoshi; Shibata, Kazunari Bibcode: 2019PASJ...71...56S Altcode: 2019arXiv190208718S; 2019PASJ..tmp...48S Filaments, the dense cooler plasma floating in the solar corona supported by magnetic fields, generally exhibit certain activations before they erupt. In our previous study (Seki et al. 2017, ApJ, 843, L24), we observed that the standard deviation of the line-of-sight (LOS) velocities of the small-scale motions in a filament increased prior to its eruption. However, because that study only analyzed one event, it is unclear whether such an increase in the standard deviation of LOS velocities is common in filament eruptions. In this study, 12 filaments that vanished in Hα line center images were analyzed in a manner similar to the one in our previous work; these included two quiescent filaments, four active region filaments, and six intermediate filaments. We verified that in all the 12 events, the standard deviation of the LOS velocities increased before the filaments vanished. Moreover, we observed that the quiescent filaments had approximately 10 times longer duration of an increase in the standard deviation than the other types of filaments. We concluded that the standard deviation of the LOS velocities of the small-scale motions in a filament can potentially be used as a precursor of a filament eruption. Title: Revisiting Kunitomo's Sunspot Drawings During 1835 - 1836 in Japan Authors: Fujiyama, Masashi; Hayakawa, Hisashi; Iju, Tomoya; Kawai, Toshiki; Toriumi, Shin; Otsuji, Kenichi; Kondo, Katsuya; Watanabe, Yusaku; Nozawa, Satoshi; Imada, Shinsuke Bibcode: 2019SoPh..294...43F Altcode: 2019arXiv190303092F We revisit the sunspot drawings made by the Japanese astronomer Kunitomo Toubei during 1835 - 1836 and recount the sunspot group number for each image. There are two series of drawings, preliminary (P , containing 17 days with observations) and summary (S , covering 156 days with observations), all made using brush and ink. S is a compilation of drawings for the period from February 1835, to March 1836. Presently, the P drawings are available only for one month, September 1835; those of other periods have presumably been lost. Another drawing (I ) lets us recover the raw group count (RGC) for 25 September 1836, on which the RGC has not been registered in the existing catalogs. We also revise the RGCs from P and S using the Zürich classification and determine that Kunitomo's results tend to yield smaller RGCs than those of other contemporary observers. In addition, we find that Kunitomo's RGCs and spot areas have a correlation (0.71) that is not very different from the contemporary observer Schwabe (0.82). Although Kunitomo's spot areas are much larger than those determined by Schwabe due to skill and instrument limitations, Kunitomo at least captured the growing trend of the spot activity in the early phase of Solar Cycle 8. We also determine the solar rotation axis to estimate the accurate position (latitude and longitude) of the sunspot groups in Kunitomo's drawings. Title: Space Weather Prediction from the Ground: Case of CHAIN Authors: Seki, Daikichi; Ueno, Satoru; Isobe, Hiroaki; Otsuji, Kenichi; Cabezas, Denis P.; Ichimoto, Kiyoshi; Shibata, Kazunari; Chain Team Bibcode: 2018SunGe..13..157S Altcode: In this article, we insist on the importance and the challenges of the prediction of solar eruptive phenomena including flares, coronal mass ejections (CME), and filament eruptions fully based on the ground-based telescopes. It is true that satellites' data are indispensable for the space weather prediction, but they are vulnerable to the space weather effects. Therefore, the ground-based telescopes can be complementary to them from the viewpoint of space weather prediction. From this view point, one possible new flare prediction method that makes use of H-alpha, red wings, and blue wings images obtained by the SDDI/SMART, the ground-based telescope at Hida Observatory, is presented. And in order to show the possibility for the actual operation based on that method, the recent progress of CHAIN project, the international observation network, is mentioned in terms of their outcomes and capacity buildings. Title: Infrared spectro-polarimeter on the Solar Flare Telescope at NAOJ/Mitaka Authors: Sakurai, Takashi; Hanaoka, Yoichiro; Arai, Takehiko; Hagino, Masaoki; Kawate, Tomoko; Kitagawa, Naomasa; Kobiki, Toshihiko; Miyashita, Masakuni; Morita, Satoshi; Otsuji, Ken'ichi; Shinoda, Kazuya; Suzuki, Isao; Yaji, Kentaro; Yamasaki, Takayuki; Fukuda, Takeo; Noguchi, Motokazu; Takeyama, Norihide; Kanai, Yoshikazu; Yamamuro, Tomoyasu Bibcode: 2018PASJ...70...58S Altcode: 2018PASJ..tmp...63S; 2018PASJ..tmp...82S An infrared spectro-polarimeter installed on the Solar Flare Telescope at the Mitaka headquarters of the National Astronomical Observatory of Japan is described. The new spectro-polarimeter observes the full Sun via slit scans performed at two wavelength bands, one near 1565 nm for a Zeeman-sensitive spectral line of Fe I and the other near 1083 nm for He I and Si I lines. The full Stokes profiles are recorded; the Fe I and Si I lines give information on photospheric vector magnetic fields, and the helium line is suitable for deriving chromospheric magnetic fields. The infrared detector we are using is an InGaAs camera with 640 × 512 pixels and a read-out speed of 90 frames s-1. The solar disk is covered by two swaths (the northern and southern hemispheres) of 640 pixels each. The final magnetic maps are made of 1200 × 1200 pixels with a pixel size of 1{^''.}8. We have been carrying out regular observations since 2010 April, and have provided full-disk, full-Stokes maps, at the rate of a few maps per day, on the internet. Title: Space Weather Prediction from the Ground: Case of CHAIN Authors: Seki, Daikichi; Ueno, Satoru; Isobe, Hiroaki; Otsuji, Kenichi; Cabezas, Denis P.; Ichimoto, Kiyoshi; Shibata, Kazunari; CHAIN team Bibcode: 2018arXiv180806295S Altcode: In this article, we insist on the importance and the challenges of the prediction of solar eruptive phenomena including flares, coronal mass ejections (CME), and filament eruptions fully based on the ground-based telescopes. It is true that satellites' data are indispensable for the space weather prediction, but they are vulnerable to the space weather effects. Therefore, the ground-based telescopes can be complementary to them from the viewpoint of space weather prediction. From this view point, one possible new flare prediction method that makes use of H-alpha, red wings, and blue wings images obtained by the SDDI/SMART, the ground-based telescope at Hida Observatory, is presented. And in order to show the possibility for the actual operation based on that method, the recent progress of CHAIN project, the international observation network, is mentioned in terms of their outcomes and capacity buildings. Title: Increase in the Amplitude of Line-of-sight Velocities of the Small-scale Motions in a Solar Filament before Eruption Authors: Seki, Daikichi; Otsuji, Kenichi; Isobe, Hiroaki; Ishii, Takako T.; Sakaue, Takahito; Hirose, Kumi Bibcode: 2017ApJ...843L..24S Altcode: 2017arXiv170509041S We present a study on the evolution of the small-scale velocity field in a solar filament as it approaches the eruption. The observation was carried out by the Solar Dynamics Doppler Imager (SDDI) that was newly installed on the Solar Magnetic Activity Research Telescope at Hida Observatory. The SDDI obtains a narrowband full-disk image of the Sun at 73 channels from Hα - 9.0 Å to Hα + 9.0 Å, allowing us to study the line-of-sight (LOS) velocity of the filament before and during the eruption. The observed filament is a quiescent filament that erupted on 2016 November 5. We derived the LOS velocity at each pixel in the filament using the Becker’s cloud model, and made the histograms of the LOS velocity at each time. The standard deviation of the LOS velocity distribution can be regarded as a measure for the amplitude of the small-scale motion in the filament. We found that the standard deviation on the previous day of the eruption was mostly constant around 2-3 km s-1, and it slightly increased to 3-4 km s-1 on the day of the eruption. It shows a further increase, with a rate of 1.1 m s-2, about three hours before eruption, and another increase, with a rate of 2.8 m s-2, about an hour before eruption. From this result we suggest that the increase in the amplitude of the small-scale motions in a filament can be regarded as a precursor of the eruption. Title: A New Solar Imaging System for Observing High-Speed Eruptions: Solar Dynamics Doppler Imager (SDDI) Authors: Ichimoto, Kiyoshi; Ishii, Takako T.; Otsuji, Kenichi; Kimura, Goichi; Nakatani, Yoshikazu; Kaneda, Naoki; Nagata, Shin'Ichi; UeNo, Satoru; Hirose, Kumi; Cabezas, Denis; Morita, Satoshi Bibcode: 2017SoPh..292...63I Altcode: A new solar imaging system was installed at Hida Observatory to observe the dynamics of flares and filament eruptions. The system (Solar Dynamics Doppler Imager; SDDI) takes full-disk solar images with a field of view of 2520 arcsec×2520 arcsec at multiple wavelengths around the H α line at 6562 Å. Regular operation was started in May 2016, in which images at 73 wavelength positions spanning from H α −9 Å to H α +9 Å are obtained every 15 seconds. The large dynamic range of the line-of-sight velocity measurements (±400 kms−1) allows us to determine the real motions of erupting filaments in 3D space. It is expected that SDDI provides unprecedented datasets to study the relation between the kinematics of filament eruptions and coronal mass ejections (CME), and to contribute to the real-time prediction of the occurrence of CMEs that cause a significant impact on the space environment of the Earth. Title: “Dandelion” Filament Eruption and Coronal Waves Associated with a Solar Flare on 2011 February 16 Authors: Cabezas, Denis P.; Martínez, Lurdes M.; Buleje, Yovanny J.; Ishitsuka, Mutsumi; Ishitsuka, José K.; Morita, Satoshi; Asai, Ayumi; UeNo, Satoru; Ishii, Takako T.; Kitai, Reizaburo; Takasao, Shinsuke; Yoshinaga, Yusuke; Otsuji, Kenichi; Shibata, Kazunari Bibcode: 2017ApJ...836...33C Altcode: 2017arXiv170100308C Coronal disturbances associated with solar flares, such as Hα Moreton waves, X-ray waves, and extreme ultraviolet (EUV) coronal waves, are discussed herein in relation to magnetohydrodynamic fast-mode waves or shocks in the corona. To understand the mechanism of coronal disturbances, full-disk solar observations with high spatial and temporal resolution over multiple wavelengths are of crucial importance. We observed a filament eruption, whose shape is like a “dandelion,” associated with the M1.6 flare that occurred on 2011 February 16 in Hα images taken by the Flare Monitoring Telescope at Ica University, Peru. We derive the three-dimensional velocity field of the erupting filament. We also identify winking filaments that are located far from the flare site in the Hα images, whereas no Moreton wave is observed. By comparing the temporal evolution of the winking filaments with those of the coronal wave seen in the EUV images data taken by the Atmospheric Imaging Assembly on board the Solar Dynamics Observatory and by the Extreme Ultraviolet Imager on board the Solar Terrestrial Relations Observatory-Ahead, we confirm that the winking filaments were activated by the EUV coronal wave. Title: Development of the Universal Tunable Filter and High-resolution Imaging Observation with the Fuxian Solar Observatory Authors: Hagino, M.; Ichimoto, K.; Ueno, S.; Kimura, G.; Otsuji, K.; Kitai, R.; Zhong, L.; Xu, Z.; Shinoda, K.; Hara, H.; Suematsu, Y.; Shimizu, T. Bibcode: 2016ASPC..504..103H Altcode: We have developed a new narrow-band universal tunable filter to perform imaging spectroscopy of the solar chromosphere. The development stage of the filter has been almost finished and we shifted to the scientific observation phase by using large grand-based telescopes. Using the filter, a series of high-resolution images were obtained with the 1m vacuum solar telescope at the Fuxian Solar Observatory. We succeeded in observing several flares and fine structures of the chromospheric layer. Title: A Real Source of a Stealth CME - Energetics of a Filament Eruption and Giant Arcade Formation Authors: Asai, Ayumi; Ishii, Takako T.; Otsuji, Kenichi; Ichimoto, Kiyoshi; Shibata, Kazunari Bibcode: 2015IAUGA..2255125A Altcode: Various active phenomena occurring on the solar surface are sources of disturbances in the solar-terrestrial environment. It is, however, sometimes said that solar flares, the most energetic explosions in the active phenome on the sun, are not crucially important for space weather researches, but coronal mass ejections (CMEs) are more significant. This is because not all flares are associated with CMEs, and therefore, not geo-effective, and because geo-effective CMEs sometimes occur without any notable active phenomena (such as flares) on the sun. The latter is sometimes called as a “stealth CME” event. However, for even such cases, we often see filament eruptions in H-alpha observations and formations of giant arcade in X-ray and/or extreme ultraviolet (EUV) observations.The geomagnetic storm with the Dst index of -105 nT that occurred on October 8, 2012 was such a stealth event. We, on the other hand, recognize formation of an X-ray giant arcade and activation of an H-alpha filament on October 5, 2012. We examined the velocity field of the filament by using the H-alpha wing data obtained with SMART telescope at Hida Observatory, Kyoto University. We also derived the temperature and the volume emission measure by using the X-ray and EUV data obtained by Hinode/XRT and SDO/AIA. We discuss the energetics of this event on the solar surface Title: A statistical analysis of current helicity and twist in solar active regions over the phases of the solar cycle using the spectro-polarimeter data of Hinode Authors: Otsuji, Kenichi; Sakurai, Takashi; Kuzanyan, Kirill Bibcode: 2015PASJ...67....6O Altcode: 2014arXiv1410.7532O; 2014PASJ..tmp..137O Current helicity and twist of solar magnetic fields are important in characterizing the dynamo mechanism working in the convection zone of the Sun. We have carried out a statistical study on the current helicity of solar active regions observed with the spectro-polarimeter (SP) of the Hinode Solar Optical Telescope (SOT). We used SOT-SP data of 558 vector magnetograms of a total of 80 active regions obtained during the period from 2006 to 2012. We have applied spatial smoothing and division of data points into weak and strong field ranges to compare the contributions from different scales and field strengths. We found that the current helicity follows the "hemispheric sign rule" when weak magnetic fields (absolute field strength < 300 gauss) are considered and no smoothing is applied. On the other hand, the pattern of current helicity fluctuates and violates the hemispheric sign rule when stronger magnetic fields are considered and smoothing of 2{^''.}0 (modeled on ground-based observations) is applied. Furthermore, we found a tendency that weak and inclined fields conform to the hemispheric sign rule and strong and vertical fields violate it. These different properties of helicity through the strong and weak magnetic field components give important clues in understanding the solar dynamo as well as the mechanism of formation and evolution of solar active regions. Title: Formation and Decay of Rudimentary Penumbra around a Pore Authors: Watanabe, Hiroko; Kitai, Reizaburo; Otsuji, Kenichi Bibcode: 2014ApJ...796...77W Altcode: We analyze the evolution of a pore in the active region NOAA 10940 using the data obtained by the Hinode satellite on 2007 February 3. The pore we analyzed showed the formation of a rudimentary penumbra structure, succeeded by an abrupt disappearance after about 5 hr. The pore had an approximate radius of 3.5 Mm and a total magnetic flux of 3.0 × 1019 Mx, which is a little smaller than the necessary magnetic flux for penumbral formation supposed by Rucklidge et al. (1-1.5 × 1020 Mx). Our observation describes a rare phenomenon which was in the unstable phase between a pore and a sunspot. The area of the dark umbra gradually decreased when the rudimentary penumbral filaments formed the penumbral structure, meaning that the penumbra develops at the expense of the umbral magnetic flux. This statement was confirmed by a rough estimation of the magnetic flux variation observed by the Hinode Fe I magnetogram. Five hours after the formation phase, the decay phase began. In this decaying phase, multiple opposite polarity patches are found to appear in the exterior of the pore (a different location from the penumbra formation site). We interpret these opposite polarities as signatures of the horizontal magnetic field, which preferably appears in the course of the unstable reconfiguration of the magnetic field structure. During the course of the disappearance of the penumbra, the horizontal penumbral field seems to become vertical because of the dark umbral area that recovered by about 10%. Title: Morphological study of penumbral formation Authors: Kitai, Reizaburo; Watanabe, Hiroko; Otsuji, Ken'ichi Bibcode: 2014PASJ...66S..11K Altcode: 2014PASJ..tmp...96K; 2014arXiv1407.4573K Penumbrae are known to be areas of mainly horizontal magnetic field surrounding umbrae of relatively large and mature sunspots. In this paper, we observationally studied the formation of penumbrae in NOAA 10978, where several penumbral formations were observed in G-band images of the Solar Optical Telescope on board Hinode. Thanks to the continuous observation by Hinode, we could morphologically follow the evolution of sunspots and found that there are several paths to the penumbral formation: (1) active accumulation of magnetic flux, (2) rapid emergence of magnetic field, and (3) appearance of twisted or rotating magnetic tubes. In all of these cases, magnetic fields are expected to sustain high inclination at the edges of flux tube concentration longer than the characteristic growth time of downward magnetic pumping. Title: Within the International Collaboration CHAIN: a Summary of Events Observed with Flare Monitoring Telescope (FMT) in Peru Authors: Ishitsuka, J.; Asai, A.; Morita, S.; Terrazas, R.; Cabezas, D.; Gutierrez, V.; Martinez, L.; Buleje, Y.; Loayza, R.; Nakamura, N.; Takasao, S.; Yoshinaga, Y.; Hillier, A.; Otsuji, K.; Shibata, K.; Ishitsuka, M.; Ueno, S.; Kitai, R.; Ishii, T.; Ichimoto, K.; Nagata, S.; Narukage, N. Bibcode: 2014SunGe...9...85I Altcode: In 2008 we inaugurated the new Solar Observatory in collaboration with Faculty of Sciences of San Luis Gonzaga de Ica National University, 300 km south of Lima. In March of 2010 a Flare Monitoring Telescope of Hida Observatory of Kyoto University arrived to Ica, part of CHAIN Project (Continuous H-alpha Imaging Network). In October of the same year we hosted the First FMT Workshop in Ica, then in July of 2011 the Second FMT Workshop was opened. Since that we are focused on two events registered by FMT in Peru to publish results. FMT is a good tool to introduce young people from universities into scientific knowledge; it is good also for education in Solar Physics and outreach. Details of this successful collaboration will be explained in this presentation. Title: Chromospheric Anemone Jets Observed with Hinode/SOT and Hida Ca II Spectroheliograph Authors: Morita, S.; Shibata, K.; Ueno, S.; Ichimoto, K.; Kitai, R.; Otsuji, K. Bibcode: 2012ASPC..454...95M Altcode: We present the first simultaneous observations of chromospheric “anemone” jets in active regions with the Ca II H broadband filetergram on the Hinode/SOT and with the Ca II K spetroheliogram on the Domeless Solar Telescope (DST) at the Hida Observatory. During coordinated observation period, 9 chromospheric anemone jets were simultaneously observed with the two instruments. These observations revealed: (1) the jets are generated in the low chromosphere because these cannot be seen in Ca II K3, (2) these jets are associated with mixed polarity regions which are either small emerging flux regions or moving magnetic features, (3) the Ca II K line often show red or blue asymmetry in K2/K1 component; the footpoint of the jets associated with emerging flux regions often show red asymmetry (2-16 km s-1), while the one with moving magnetic features show blue asymmetry (∼5 km s-1). The magnetic cancellations were observed at the footpoint of the jets. The canceling rates are of order of 1016 Mx s-1, and the resulting magnetic energy release rate (1.1-10)×1024 erg s-1, with the total energy release (1-13)×1026 erg for the duration of the magnetic cancellations, ∼130 s. These are comparable to the estimated total energy, ∼1026 erg, in a single chromospheric anemone jet. Title: Statistical Study on the Nature of Solar-Flux Emergence Authors: Otsuji, Kenichi; Kitai, Reizaburo; Ichimoto, Kiyoshi; Shibata, Kazunari Bibcode: 2011PASJ...63.1047O Altcode: 2011arXiv1106.1955O We studied 101 flux emergence events ranging from small ephemeral regions to large emerging flux regions that were observed with the Hinode Solar Optical Telescope filtergram. We investigated how the total magnetic flux of the emergence event controls the nature of emergence. To determine the modes of emergences, horizontal velocity fields of the global motion of the magnetic patches in the flux emerging sites were measured by local correlation tracking. Between two main polarities of the large emerging flux regions with more than around 2 × 1019 Mx, there were converging flows of anti-polarity magnetic patches. On the other hand, small ephemeral regions showed no converging flow, but a simple diverging pattern. When we looked into the detailed features in the emerging sites, irrespective of the total flux and the spatial size, all of the emergence events were observed to consist of single or multiple elementary emergence unit(s). The typical size of unitary emergence is 4 Mm, and consistent with simulation results. From a statistical study of the flux emergence events, the maximum spatial distance between two main polarities, the magnetic flux growth rate and the mean separation speed were found to follow the power-law functions of the total magnetic flux with indices of 0.27, 0.57, and -0.16, respectively. From a discussion on the observed power-law relations, we obtained a physical view of solar flux emergence, in which the emerging magnetic fields float and evolve while balancing to the surrounding turbulent atmosphere. Title: Observations of Chromospheric Anemone Jets with Hinode Ca II Broadband Filtergraph and Hida Ca II Spectroheliograph Authors: Morita, Satoshi; Shibata, Kazunari; UeNo, Satoru; Ichimoto, Kiyoshi; Kitai, Reizaburo; Otsuji, Ken-ichi Bibcode: 2010PASJ...62..901M Altcode: 2010arXiv1002.2143M We present the first simultaneous observations of chromospheric "anemone" jets in solar active regions with Hinode SOT Ca II H broadband filetergram and Ca II K spetroheliogram on the Domeless Solar Telescope (DST) at Hida Observatory. During the coordinated observation, 9 chromospheric anemone jets were simultaneously observed with the two instruments. These observations revealed three important features, i.e.: (1) the jets are generated in the lower chromosphere, (2) the length and lifetime of the jets are 0.4-5 Mm and 40-320 sec, (3) the apparent velocity of the jets with Hinode SOT are 3-24 km/s, while Ca II K3 component at the jets show blueshifts (in 5 events) in the range of 2- 6 km/s. The chromospheric anemone jets are associated with mixed polarity regions which are either small emerging flux regions or moving magnetic features. It is found that the Ca II K line often show red or blue asymmetry in K2/K1 component: the footpoint of the jets associated with emerging flux regions often show redshift (2-16 km/s), while the one with moving magnetic features show blueshift (around 5 km/s). Detailed analysis of magnetic evolution of the jet foaming regions revealed that the reconnection rate (or canceling rate) of the total magnetic flux at the footpoint of the jets are of order of 10^{16} Mx/s, and the resulting magnetic energy release rate (1.1-10) x 10^{24} erg/s, with the total energy release (1-13) x 10^{26} erg for the duration of the magnetic cancellations, 130s. These are comparable to the estimated total energy, 10^{26} erg, in a single chromospheric anemone jet. An observation-based physical model of the jet is presented. The relation between chromospheric anemone jets and Ellerman bombs is discussed. Title: Internal Fine Structure of Ellerman Bombs Authors: Hashimoto, Yuki; Kitai, Reizaburo; Ichimoto, Kiyoshi; Ueno, Satoru; Nagata, Shin'ichi; Ishii, Takako T.; Hagino, Masaoki; Komori, Hiroyuki; Nishida, Keisuke; Matsumoto, Takuma; Otsuji, Kenichi; Nakamura, Tahei; Kawate, Tomoko; Watanabe, Hiroko; Shibata, Kazunari Bibcode: 2010PASJ...62..879H Altcode: We conducted coordinated observations of Ellerman bombs (EBs) between Hinode Satellite and Hida Observatory (HOP12). CaII H broad-band filter images of NOAA 10966 on 2007 August 9 and 10 were obtained with the Solar Optical Telescope (SOT) aboard the Hinode Satellite, and many bright points were observed. We identified a total of 4 bright points as EBs, and studied the temporal variation of their morphological fine structures and spectroscopic characteristics. With high-resolution CaII H images of SOT, we found that the EBs, thus far thought of as single bright features, are composed of a few of fine subcomponents. Also, by using Stokes I/V filtergrams with Hinode/SOT, and CaII H spectroheliograms with Hida/Domeless Solar Telescope (DST), our observation showed: (1) The mean duration, the mean width, the mean length, and the mean aspect ratio of the subcomponents were 390 s, 170 km, 450 km, and 2.7, respectively. (2) Subcomponents started to appear on the magnetic neutral lines, and extended their lengths from the original locations. (3) When the CaII H line of EBs showed the characteristic blue asymmetry, they are associated with the appearance or re-brightening of subcomponents. Summarizing our results, we obtained an observational view that elementary magnetic reconnections take place one by one successively and intermittently in EBs, and that their manifestation is the fine subcomponents of the EB phenomena. Title: Spicule Dynamics over a Plage Region Authors: Anan, Tetsu; Kitai, Reizaburo; Kawate, Tomoko; Matsumoto, Takuma; Ichimoto, Kiyoshi; Shibata, Kazunari; Hillier, Andrew; Otsuji, Kenichi; Watanabe, Hiroko; Ueno, Satoru; Nagata, Shin'ichi; Ishii, Takako T.; Komori, Hiroyuki; Nishida, Keisuke; Nakamura, Tahei; Isobe, Hiroaki; Hagino, Masaoki Bibcode: 2010PASJ...62..871A Altcode: 2010arXiv1002.2288A We studied spicular jets over a plage area and derived their dynamic characteristics using Hinode Solar Optical Telescope (SOT) high-resolution images. A target plage region was near to the west limb of the solar disk. This location permitted us to study the dynamics of spicular jets without any overlapping effect of spicular structures along the line of sight. In this work, to increase the ease with which we could identify spicules on the disk, we applied the image processing method `MadMax' developed by Koutchmy et al. (1989). It enhances fine, slender structures (like jets), over a diffuse background. We identified 169 spicules over the target plage. This sample permited us to derive statistically reliable results regarding spicular dynamics. The properties of plage spicules can be summarized as follows: (1) In a plage area, we clearly identified spicular jet features. (2) They were shorter in length than the quiet region limb spicules, and followed a ballistic motion under constant deceleration. (3) The majority (80%) of the plage spicules showed a cycle of rise and retreat, while 10% of them faded out without a complete retreat phase. (4) The deceleration of the spicule was proportional to the velocity of ejection (i.e., the initial velocity). Title: CaII K Spectral Study of an Emerging Flux Region using the Domeless Solar Telescope in Hida Observatory Authors: Otsuji, Kenichi; Kitai, Reizaburo; Matsumoto, Takuma; Ichimoto, Kiyoshi; Ueno, Satoru; Nagata, Shin'ichi; Isobe, Hiroaki; Shibata, Kazunari Bibcode: 2010PASJ...62..893O Altcode: 2010arXiv1005.2025O A cooperative observation with Hida Observatory and the Hinode satellite was performed on an emerging flux region. Successive CaII K spectro-heliograms of the emerging flux region were taken by the Domeless Solar Telescope of Hida Observatory. Hinode observed the emerging flux region with CaII H and FeI Stokes IQUV filtergrams. In this study, detailed dynamics and the temporal evolution of the magnetic flux emergence was studied observationally. The event was first detected in the photospheric magnetic field signals; 3 minutes later, a horizontal expansion of the dark area was detected. Then, 7 minutes later than the horizontal expansion, the emerging loops were detected with a maximal rise speed of 2.1 km s-1 at chromospheric heights. The observed dynamics of the emerging magnetic flux from the photosphere to the upper chromosphere was very consistent with the results of previous simulation studies. A gradual rising phase of flux tubes with a weak magnetic strength was confirmed by our observation. Title: Emergence of Helical Flux and the Formation of an Active Region Filament Channel Authors: Lites, B. W.; Kubo, M.; Berger, T.; Frank, Z.; Shine, R.; Tarbell, T.; Title, A.; Okamoto, T. J.; Otsuji, K. Bibcode: 2010ApJ...718..474L Altcode: We present comprehensive observations of the formation and evolution of a filament channel within NOAA Active Region (AR) 10978 from Hinode/Solar Optical Telescope and TRACE. We employ sequences of Hinode spectro-polarimeter maps of the AR, accompanying Hinode Narrowband Filter Instrument magnetograms in the Na I D1 line, Hinode Broadband Filter Instrument filtergrams in the Ca II H line and G-band, Hinode X-ray telescope X-ray images, and TRACE Fe IX 171 Å image sequences. The development of the channel resembles qualitatively that presented by Okamoto et al. in that many indicators point to the emergence of a pre-existing sub-surface magnetic flux rope. The consolidation of the filament channel into a coherent structure takes place rapidly during the course of a few hours, and the filament form then gradually shrinks in width over the following two days. Particular to this filament channel is the observation of a segment along its length of horizontal, weak (500 G) flux that, unlike the rest of the filament channel, is not immediately flanked by strong vertical plage fields of opposite polarity on each side of the filament. Because this isolated horizontal field is observed in photospheric lines, we infer that it is unlikely that the channel formed as a result of reconnection in the corona, but the low values of inferred magnetic fill fraction along the entire length of the filament channel suggest that the bulk of the field resides somewhat above the low photosphere. Correlation tracking of granulation in the G band presents no evidence for either systematic flows toward the channel or systematic shear flows along it. The absence of these flows, along with other indications of these data from multiple sources, reinforces (but does not conclusively demonstrate) the picture of an emerging flux rope as the origin of this AR filament channel. Title: Solar Plages: Observational Study of Their Chromospheric Heating and Spicular Mass Ejections Authors: Kitai, R.; Hashimoto, Y.; Anan, T.; Matsumoto, T.; Kawate, T.; Watanabe, H.; Otsuji, K.; Nakamura, T.; Nishizuka, N.; Nishida, K.; Ueno, S.; Nagata, S.; Shibata, K. Bibcode: 2009ASPC..415...19K Altcode: We investigated the chromospheric dynamics of plage area. From our spectroscopic analysis of the CaII K line, we have found that their periodic variations are due to the propagation of acoustic waves from the lower layers. Another observational work on Hinode CaII H images, gave us a new result that there are numerous spicular jets in plage area, thanks to the stable observing condition of Hinode. The present paper is an extended abstract of our works which will be published fully in our future papers. Title: The tandem Fabry Perot Full-Disk Solar Vector Magnetogram system for the Solar Magnetic Activity Research Telescope (SMART) Authors: Otsuji, K.; Nagata, S.; Ueno, S.; Kitai, R.; Kimura, G.; Nakatani, Y.; Ishii, T.; Morita, S.; Shibata, K. Bibcode: 2009AGUFMSH33B1498O Altcode: For solar and heliospheric physics, energy release mechanism of solar flares and onset of CMEs are one of the most the most important issues. Solar Magnetic Activity Research Telescope (SMART) in Hida observatory Kyoto University aims to investigate the relation between the solar flares and photospheric vector magnetic field. Full disk high resolution H-alpha images as well as and photospheric vector magnetic field using Fe I 6302 line have been taken regularly since 2005. In order to improve the vector magnetic field measurement accuracy, a tandem Fabry Perot Stokes polarimeter is newly constructed for the SMART. The system consist of a tandem FP with FWHM of ~0.01nm, polarization beam splitter and two CCD cameras taking orthogonally polarized images simultaneously. In this poster we present the system design and laboratory test results, and expected observational capabilities. We also present the flux emergence activities observed with SMART and Hinode satellite. Title: The tandem Fabry-Perot filter imaging spectro-polarimeter for the Solar Magnetic Activity Research Telescope (SMART) Authors: Nagata, Shin'ichi; Otsuji, Kenichi; Ishii, Takako T.; Ichimoto, Kiyoshi; Ueno, Satoru; Kitai, Reizaburo; Kimura, Goichi; Shibata, Kazunari; Nakatani, Yoshikazu; Morita, Satoshi Bibcode: 2009SPIE.7438E..0VN Altcode: 2009SPIE.7438E..22N In order to perform precise and high time cadence magnetic field measurement across the solar surface, the Tandem Fabry-Perot filter imaging spectro-polarimeter for the Solar Magnetic Activity Research Telescope (SMART) is revised. By using the CCD with moderate frame rate of 30fps, full Stokes vectors on the field-of-view 320"x240" can be obtained at 4 wavelengths around FeI6302 line within about 15s. The optical performance of the Tandem Fabry-Perof filters is investigated by using the spectrograph at the Domeless Solar Telescope at Hida Observatory. The test results show the full-width-half-maximum (FWHM) of the tandem filters is about 0.017nm over the 60mm clear aperture is achieved. The system is developed to start the regular observations from 2010. Title: Cooperative observation of solar atmospheric heating by Hida observatory and Hinode Authors: Kitai, R.; Hashimoto, Y.; Anan, T.; Watanabe, H.; Ishii, T. T.; Kawate, T.; Matsumoto, T.; Otsuji, K.; Nakamura, T.; Morita, S.; Nishizuka, N.; Nishida, K.; Ueno, S.; Nagata, S.; Ichimoto, K.; Shibata, K. Bibcode: 2008AGUFMSH41B1625K Altcode: At Hida observatory of Kyoto University, we continue to study solar activities and fine structures with Domeless Solar Telescope (DST) and Solar Magnetic Activity Research Telescope (SMART). In this work, we will report some recent cooperative observational results with Hinode on the following topics: (1) Plage heating and waves Analysis of a long time series of CaII K spectrograms at a plage area showed us a clear co-existence of 3- and 5-min oscillation in Doppler velocity. We simulated the response of the VAL model atmosphere to the input of 3-min/5-min acoustic disturbances, in 1-D geometry and found that plage chromosphere is heated unsteadily by acoustic shock waves as was proposed by Carlsson and Stein (1997). (2) Disk spicules in and around plage regions We clearly identified numerous ejecting features in a plage area. Their morphological shapes of thin tapered cylinder and their dynamics strongly suggest that they are spicules in plage area. Plage spicules were observed to move under constant deceleration, which are driven by acoustic shock waves predicted by Shibata and Suematsu (1980) and Hansteen et al. (2007). Our results will be discussed from the view point of Type I, II classification of limb spicules ( de Pontieu et al. 2007). (3) Umbral dots We have confirmed that umbral dots are manifestation of magneto-convection in strong magnetic filed from the analysis of Hinode/SOT/BFI&SP. We will discuss the plausibility of monolithic umbral model from the oscillatory brightening of umbral dots. (4) X-ray brightenings in the supergranular network XRT showed us numerous bright points in solar quiet regions. Possible relation between these XBPs and supergranular network pattern in quiet chromosphere was studied. XBPs were found to be located in the network not in the cell center. Many of network bright XBPs were consisted of magnetically bipolar loops. (5) Ellerman bombs By studying the fine structure of Ellerman bomb, we have found core-halo structure and loop like fine-structures in the chromosphere. Discussions on the origin of bombs will be given from the viewpoint of magnetic reconnection theory. Title: Giant Chromospheric Anemone Jet Observed with Hinode and Comparison with Magnetohydrodynamic Simulations: Evidence of Propagating Alfvén Waves and Magnetic Reconnection Authors: Nishizuka, N.; Shimizu, M.; Nakamura, T.; Otsuji, K.; Okamoto, T. J.; Katsukawa, Y.; Shibata, K. Bibcode: 2008ApJ...683L..83N Altcode: 2008arXiv0810.3384N Hinode discovered a beautiful giant jet with both cool and hot components at the solar limb on 2007 February 9. Simultaneous observations by the Hinode SOT, XRT, and TRACE 195 Å satellites revealed that hot (~5 × 106 K) and cool (~104 K) jets were located side by side and that the hot jet preceded the associated cool jet (~1-2 minutes). A current-sheet-like structure was seen in optical (Ca II H), EUV (195 Å), and soft X-ray emissions, suggesting that magnetic reconnection is occurring in the transition region or upper chromosphere. Alfvén waves were also observed with Hinode SOT. These propagated along the jet at velocities of ~200 km s-1 with amplitudes (transverse velocity) of ~5-15 km s-1 and a period of ~200 s. We performed two-dimensional MHD simulation of the jets on the basis of the emerging flux-reconnection model, by extending Yokoyama and Shibata's model. We extended the model with a more realistic initial condition (~106 K corona) and compared our model with multiwavelength observations. The improvement of the coronal temperature and density in the simulation model allowed for the first time the reproduction of the structure and evolution of both the cool and hot jets quantitatively, supporting the magnetic reconnection model. The generation and the propagation of Alfvén waves are also reproduced self-consistently in the simulation model. Title: Cooperative Observation of Ellerman Bombs between the Solar Optical Telescope aboard Hinode and Hida/Domeless Solar Telescope Authors: Matsumoto, Takuma; Kitai, Reizaburo; Shibata, Kazunari; Nagata, Shin'ichi; Otsuji, Kenichi; Nakamura, Tahei; Watanabe, Hiroko; Tsuneta, Saku; Suematsu, Yoshinori; Ichimoto, Kiyoshi; Shimizu, Toshifumi; Katsukawa, Yukio; Tarbell, Theodore D.; Lites, Bruce W.; Shine, Richard A.; Title, Alan M. Bibcode: 2008PASJ...60..577M Altcode: High-resolution CaIIH broad-band filter images of NOAA10933 on 2007 January 5 were obtained by the Solar Optical Telescope aboard the Hinode satellite. Many small-scale (∼1") bright points were observed outside the sunspot and inside the emerging flux region. We identified some of these bright points with Ellerman bombs (EBs) by using Hα images taken by the Domeless Solar Telescope at Hida observatory. The sub-arcsec structures of two EBs seen in CaIIH were studied in detail. Our observation showed the following two aspects: (1) The CaIIH bright points identified with EBs were associated with the bipolar magnetic field structures, as reported by previous studies. (2)The structure of the CaIIH bright points turned out to consist of the following two parts: a central elongated bright core (0.7" × 0.5") located along the magnetic neutral line and a diffuse halo (1.2"×1.8"). Title: Height Dependence of Gas Flows in an Ellerman Bomb Authors: Matsumoto, Takuma; Kitai, Reizaburo; Shibata, Kazunari; Otsuji, Kenichi; Naruse, Takuya; Shiota, Daikou; Takasaki, Hiroyuki Bibcode: 2008PASJ...60...95M Altcode: We performed spectroscopic observations of Ellerman bombs (EBs) in an active region of NOAA 10705 at Hida Observatory on 2004 November 24. The photospheric velocity fields of EBs have for the first time been investigated spectroscopically. From the Doppler shifts of a TiII absorption line (6559.576Å) and a broad Hα emission line, we derived the photospheric velocity and the lower chromospheric velocity, respectively. The photospheric velocity of EBs was ∼ 0.2kms-1, indicating downward flow, on average. We found that the photospheric velocity variation of EBs has a good temporal correlation with the Hα wing emission variation. On the other hand, the chromospheric velocity showed an upward flow of ∼1-3kms-1 on the average. From the characteristics of the flow field, we conclude that the observed EB occurred at the upper photospheric level. We suggest that it is important to know the motions of EBs in the photosphere because a plausible triggering mechanism of EBs is magnetic reconnection in the low-lying atmosphere. Title: Giant chromospheric jet observed with Hinode and magnetic reconnection model Authors: Nishizuka, Naoto; Shimizu, Masaki; Nakamura, Tahei; Otsuji, Kenichi; Okamoto, Takenori; Shibata, Kazunari; Katsukawa, Yukio Bibcode: 2008cosp...37.2239N Altcode: 2008cosp.meet.2239N Heating of the solar chromosphere and corona is one of the long-standing puzzles in astronomy and also a key to understand the Sun-Earth connection through solar wind and EUV/X-ray radiation. A solar space telescope mission Hinode revealed that solar chromosphere is much more dynamic than had been thought and is full of tiny jets, which may be a key to resolve the puzzle of chromospheric and coronalheating. It has long been observed that H-alpha jets called surges often occur in the chromosphere. They have been believed to be produced by magnetic reconnection, which is an energy conversion mechanism from magnetic energy into thermal and kinetic energies of plasma when anti-parallel magnetic fields encounter and reconnect with each other. Hinode's new chromospheric observations (with Calcium II H broad band filter) revealed that jets are ubiquitous in the chromosphere and some of the jets show evidence of magnetic reconnection. However, there have not been simultaneous observations of the chromospheric jets at X-ray, EUV, and Optical (at Calcium II H line) wavelengths until now. Here we report first multi-wavelength observations of a chromospheric jet with Solar Optical Telescope (SOT) and X-Ray Telescope (XRT) on board Hinode and TRACE 195A filter. With its unprecedented high quality instruments at both optical and X-rays, Hinode discovered a beautiful, giant jet with both cool (104 K) and hot (5x106 K) components at the solar limb. TRACE satellite also observed the same jet with EUV telescope and revealed the existence of both hot (106 K) and cool (unknown temperature) components. These data set are probably the best multi-wavelength observations of solar jets until now. We also performed magnetohydrodynamic simulation of the jet based on the reconnection model and found that it can explain various observational facts very well. It has often been argued that some of solar jets are produced by magnetic reconnection, but previous observations had a limitation on spatial and temporal resolutions and temperature coverage. Using these new data and twodimensional magnetohydrodynamic simulations of the jet, we showed, for the first time, how hot and cool jets are heated and accelerated during the reconnection, including associated generation of Alfvén waves. This jet formation dynamics would show a proto-tyep of reconnection e model of solar jets and can be applied for other small jets discovered by Hinode, which might heat the chromosphere and corona. Title: Chromospheric Anemone Jets as Evidence of Ubiquitous Reconnection Authors: Shibata, Kazunari; Nakamura, Tahei; Matsumoto, Takuma; Otsuji, Kenichi; Okamoto, Takenori J.; Nishizuka, Naoto; Kawate, Tomoko; Watanabe, Hiroko; Nagata, Shin'ichi; UeNo, Satoru; Kitai, Reizaburo; Nozawa, Satoshi; Tsuneta, Saku; Suematsu, Yoshinori; Ichimoto, Kiyoshi; Shimizu, Toshifumi; Katsukawa, Yukio; Tarbell, Theodore D.; Berger, Thomas E.; Lites, Bruce W.; Shine, Richard A.; Title, Alan M. Bibcode: 2007Sci...318.1591S Altcode: 2008arXiv0810.3974S The heating of the solar chromosphere and corona is a long-standing puzzle in solar physics. Hinode observations show the ubiquitous presence of chromospheric anemone jets outside sunspots in active regions. They are typically 3 to 7 arc seconds = 2000 to 5000 kilometers long and 0.2 to 0.4 arc second = 150 to 300 kilometers wide, and their velocity is 10 to 20 kilometers per second. These small jets have an inverted Y-shape, similar to the shape of x-ray anemone jets in the corona. These features imply that magnetic reconnection similar to that in the corona is occurring at a much smaller spatial scale throughout the chromosphere and suggest that the heating of the solar chromosphere and corona may be related to small-scale ubiquitous reconnection. Title: Small-Scale Magnetic-Flux Emergence Observed with Hinode Solar Optical Telescope Authors: Otsuji, Kenichi; Shibata, Kazunari; Kitai, Reizaburo; Ueno, Satoru; Nagata, Shin'ichi; Matsumoto, Takuma; Nakamura, Tahei; Watanabe, Hiroko; Tsuneta, Saku; Suematsu, Yoshinori; Ichimoto, Kiyoshi; Shimizu, Toshifumi; Katsukawa, Yukio; Tarbell, Theodore D.; Lites, Bruce; Shine, Richard A.; Title Alan M. Bibcode: 2007PASJ...59S.649O Altcode: 2007arXiv0709.3207O We observed small-scale magnetic-flux emergence in a sunspot moat region by the Solar Optical Telescope (SOT) aboard the Hinode satellite. We analyzed filtergram images observed at wavelengths of Fe 6302Å, G band, and CaII H. In Stokes I images of Fe 6302Å, emerging magnetic flux was recognized as dark lanes. In the G band, they showed to be their shapes almost the same as in Stokes I images. These magnetic fluxes appeared as dark filaments in CaII H images. Stokes V images of Fe 6302Å showed pairs of opposite polarities at footpoints of each filament. These magnetic concentrations were identified to correspond to bright points in G band/CaII H images. From an analysis of time-sliced diagrams, we derived the following properties of emerging flux, which are consistent with those of previous studies: (1) Two footpoints separate each other at a speed of 4.2kms-1 during the initial phase of evolution, and decrease to about 1kms-1 10minutes later. (2) CaII H filaments appear almost simultaneously with the formation of dark lanes in Stokes I in an observational cadence of 2minutes. (3) The lifetime of the dark lanes in the Stokes I and G band is 8minutes, while that of Ca filament is 12minutes. An interesting phenomena was observed, that an emerging flux tube expanded laterally in the photosphere with a speed of 3.8kms-1. A discussion on the horizontal expansion of the flux tube is given with refernce to previous simulation studies. Title: Umbral Fine Structures in Sunspots Observed with Hinode Solar Optical Telescope Authors: Kitai, Reizaburo; Watanabe, Hiroko; Nakamura, Tahei; Otsuji, Ken-ichi; Matsumoto, Takuma; UeNo, Satoru; Nagata, Shin'ichi; Shibata, Kazunari; Muller, Richard; Ichimoto, Kiyoshi; Tsuneta, Saku; Suematsu, Yoshinori; Katsukawa, Yukio; Shimizu, Toshifumi; Tarbell, Theodore D.; Shine, Richard A.; Title, Alan M.; Lites, Bruce Bibcode: 2007PASJ...59S.585K Altcode: 2007arXiv0711.3266K A high resolution imaging observation of a sunspot umbra was made with the Hinode Solar Optical Telescope. Filtergrams at wavelengths of the blue and green continua were taken during three consecutive days. The umbra consisted of a dark core region, several diffuse components, and numerous umbral dots. We derived basic properties of umbral dots (UDs), especially their temperatures, lifetimes, proper motions, spatial distribution, and morphological evolution. The brightness of UDs is confirmed to depend on the brightness of their surrounding background. Several UDs show fission and fusion. Thanks to the stable condition of the space observation, we could for the first time follow the temporal behavior of these events. The derived properties of the internal structure of the umbra are discussed from the viewpoint of magnetoconvection in a strong magnetic field. Title: Preliminary experimental results of gas recycling subsystems except carbon dioxide concentration Authors: Otsuji, K.; Sawada, T.; Satoh, S.; Kanda, S.; Matsumura, H.; Kondo, S.; Otsubo, K. Bibcode: 1987AdSpR...7d..69O Altcode: 1987AdSpR...7...69O Oxygen concentration and separation is an essential factor for air recycling in a CELSS. Furthermore, if the value of the plant assimilatory quotient is not coincident with that of the animal respiratory quotient, the recovery of O2 from the concentrated CO2 through chemical methods will become necessary to balance the gas contents in a CELSS. Therefore, oxygen concentration and separation equipment using Salcomine and O2 recovery equipment, such as Sabatier and Bosch reactors, were experimentally developed and tested.