Author name code: matsumoto ADS astronomy entries on 2022-09-14 =author:"Matsumoto, Takuma" ------------------------------------------------------------------------ Title: Physical properties of the inner solar corona derived from radio scintillation observations with the Akatsuki spacecraft Authors: Chiba, Shota; Yamazaki, Atsushi; Murata, Yasuhiro; Murakami, Go; Asmar, Sami; Paetzold, Martin; Miyoshi, Yoshizumi; Iwai, Kazumasa; Ando, Hiroki; Häusler, Bernd; Tokumaru, Munetoshi; Imamura, Takeshi; Matsumoto, Takuma; Takeuchi, Hiroshi Bibcode: 2022cosp...44.1345C Altcode: The acceleration of the solar wind mainly occurs in the outer corona at heliocentric distances of about 5-20 $R_{S}$ (= solar radii), where the coronal heating by magnetohydrodynamic waves and the wave-induced magnetic pressure are thought to play major roles in the acceleration. The mechanisms have not been fully confirmed by observations because the acceleration region is too close to the Sun to be observed by in-situ probes. Recently, however, the inner heliosphere observation network is getting ready, such as NASA's Parker Solar Probe and ESA's Solar orbiter. The radio occultation observation covers the acceleration region fully and can obtain the large-scale process of the plasma complementary to in-situ observation. The JAXA's Venus orbiter Akatsuki conducted the radio occultation observations on either side of the superior conjunction. The observations covered various solar cycle periods from solar maximum to solar minimum. Key physical processes in the acceleration region can be observed with radio occultation. Coronal plasma traversing the ray path disturbs radio wave's amplitudes and frequency, from which we can derive physical parameters such as the flow speed and wave's amplitudes. In this research, we analyze data taken by radio occultation observations carried out using Akatsuki's signals during the superior conjunction periods in 2011, 2016, 2018, and 2021. The radial velocity and the turbulence characteristics (power-law exponent, axial ratio and inner scale) were retrieved from the intensity scintillation time series taken in 2016 by fitting a theoretical spectrum to the observed power spectra. In the radial distribution of the derived solar wind velocity, fast winds originating from regions near a coronal hole and slow winds from other regions were identified. We also found that the inner scale increases with the heliocentric distance and that the fast solar wind has larger inner scales than the slow solar wind. We also applied wavelet analysis to the frequency time series taken in 2011 to detect quasi-periodic fluctuations (QPC), that are thought to represent acoustic waves, and quantify the amplitude, the period, and the coherence time of each wave event. The density amplitude and the wave energy flux were estimated following the method of Miyamoto et al. (2014). We confirmed that the fractional density amplitude increases with distance up to $\sim$6 $R_{S}$. The amplitude reaches tens of percent, suggesting a possibility of wave breaking. The energy fluxes increase with distance up to $\sim$6 $R_{S}$, suggesting local generation of waves. It is probable that these radial distributions indicate that the Alfvén waves propagating from the photosphere generate acoustic waves in the outer corona, and the generated acoustic waves dissipate to heat the corona, as suggested by numerical models. The wave energy fluxes in the fast solar wind were larger than those in the slow wind. The results suggest that the fast solar wind originating from the coronal hole is powered by a larger injection of wave energy than the slow wind originating from other regions. In this presentation, we will also report results from the data taken by Akatsuki. Title: Observation of the Solar Corona Using Radio Scintillation with the Akatsuki Spacecraft: Difference Between Fast and Slow Wind Authors: Chiba, Shota; Imamura, Takeshi; Tokumaru, Munetoshi; Shiota, Daikou; Matsumoto, Takuma; Ando, Hiroki; Takeuchi, Hiroshi; Murata, Yasuhiro; Yamazaki, Atsushi; Häusler, Bernd; Pätzold, Martin Bibcode: 2022SoPh..297...34C Altcode: The properties of the coronal plasma at heliocentric distances of 1.5 - 8.9 R⊙ (solar radii) were studied with radio-occultation observations using JAXA's Akatsuki spacecraft in 2016. Physical parameters that characterize the solar wind were retrieved from the intensity-scintillation time series by fitting a theoretical spectrum to the observed power spectra. The derived solar-wind velocity clearly shows a difference between the fast wind and the slow wind, which was identified based on IPS observations. The inner scale, at which fluid motions dissipate and kinetic energy is converted to heat, increases with the heliocentric distance, and the fast wind has larger inner scales than the slow wind. By applying wavelet analysis to the frequency time series, we detected quasi-periodic fluctuations in the electron density. The density oscillations are considered to be manifestations of acoustic waves, which were generated from Alfvén waves originating from the photosphere, and the energy fluxes of those acoustic waves were estimated. The relative density-amplitude peaks around 4 - 6 R⊙ and the wave-energy flux decreases beyond ≈ 6 R⊙, implying that the acoustic waves dissipate to heat the corona. The phase-scintillation spectrum that we obtained cannot be expressed by a single power law. A break is seen around the frequency of 0.5 - 2 Hz beyond ≈ 6 R⊙, suggesting an excess power other than turbulence at lower frequencies. The enhancement of the relative density amplitude around 6 R⊙ found by the wavelet analysis might explain this excess power. The acoustic wave-energy flux in the fast solar wind tends to exceed that in the slow wind, suggesting that the fast wind is powered by a larger injection of Alfvén-wave energy than the slow wind. Title: Probing the Physics of the Solar Atmosphere with the Multi-slit Solar Explorer (MUSE). I. Coronal Heating Authors: De Pontieu, Bart; Testa, Paola; Martínez-Sykora, Juan; Antolin, Patrick; Karampelas, Konstantinos; Hansteen, Viggo; Rempel, Matthias; Cheung, Mark C. M.; Reale, Fabio; Danilovic, Sanja; Pagano, Paolo; Polito, Vanessa; De Moortel, Ineke; Nóbrega-Siverio, Daniel; Van Doorsselaere, Tom; Petralia, Antonino; Asgari-Targhi, Mahboubeh; Boerner, Paul; Carlsson, Mats; Chintzoglou, Georgios; Daw, Adrian; DeLuca, Edward; Golub, Leon; Matsumoto, Takuma; Ugarte-Urra, Ignacio; McIntosh, Scott W.; the MUSE Team Bibcode: 2022ApJ...926...52D Altcode: 2021arXiv210615584D The Multi-slit Solar Explorer (MUSE) is a proposed mission composed of a multislit extreme ultraviolet (EUV) spectrograph (in three spectral bands around 171 Å, 284 Å, and 108 Å) and an EUV context imager (in two passbands around 195 Å and 304 Å). MUSE will provide unprecedented spectral and imaging diagnostics of the solar corona at high spatial (≤0.″5) and temporal resolution (down to ~0.5 s for sit-and-stare observations), thanks to its innovative multislit design. By obtaining spectra in four bright EUV lines (Fe IX 171 Å, Fe XV 284 Å, Fe XIX-Fe XXI 108 Å) covering a wide range of transition regions and coronal temperatures along 37 slits simultaneously, MUSE will, for the first time, "freeze" (at a cadence as short as 10 s) with a spectroscopic raster the evolution of the dynamic coronal plasma over a wide range of scales: from the spatial scales on which energy is released (≤0.″5) to the large-scale (~170″ × 170″) atmospheric response. We use numerical modeling to showcase how MUSE will constrain the properties of the solar atmosphere on spatiotemporal scales (≤0.″5, ≤20 s) and the large field of view on which state-of-the-art models of the physical processes that drive coronal heating, flares, and coronal mass ejections (CMEs) make distinguishing and testable predictions. We describe the synergy between MUSE, the single-slit, high-resolution Solar-C EUVST spectrograph, and ground-based observatories (DKIST and others), and the critical role MUSE plays because of the multiscale nature of the physical processes involved. In this first paper, we focus on coronal heating mechanisms. An accompanying paper focuses on flares and CMEs. Title: Physical properties of the solar corona studied by spacecraft radio scintillation and the difference between fast and slow winds Authors: Chiba, Shota; Imamura, Takeshi; Tokumaru, Munetoshi; Shiota, Daikou; Ando, Hiroki; Matsumoto, Takuma; Takeuchi, Hiroshi; Murata, Yasuhiro; Yamazaki, Atsushi Bibcode: 2021AGUFMSH32B..06C Altcode: The solar wind is a supersonic plasma flow streamed from the solar corona. The solar wind is classified into the fast wind (typically ~750 km/s) and the slow wind (~300 km/s). The acceleration of the solar wind mainly occurs in the outer corona at heliocentric distances of <10 RS (= solar radii), where the coronal heating by magnetohydrodynamic waves and the wave-induced magnetic pressure are thought to play major roles in the acceleration. The mechanisms have not been fully confirmed by observations because the acceleration region is too close to the Sun to be observed by in-situ probes. Key physical processes in the acceleration region can be observed with radio occultation. Coronal plasma traversing the ray path disturbs radio waves amplitudes and frequency, from which we can derive physical parameters such as the flow speed and waves amplitudes. In this research, we analyze data taken by radio occultation observations carried out using JAXAs Venus orbiter Akatsuki's during the superior conjunction periods from May 30 to June 15, 2016. Solar offset distances of about 1.49.0 RS were probed intermittently by 11 observations. Physical parameters were retrieved from the intensity scintillation time series by fitting a theoretical spectrum to the observed power spectra. The derived solar wind velocity clearly shows a difference between the fast wind and the slow wind, which were identified based on IPS observations. The inner scale, at which kinetic energy is converted to heat, increases with the heliocentric distance, and the fast wind has larger inner scales than the slow wind. By applying wavelet analysis to the frequency time series, we detected quasi-periodic fluctuations in the electron density. The density oscillations are considered as manifestations of acoustic waves, which were generated from Alfven waves originating from the photosphere, and the energy fluxes of those acoustic waves were estimated. The fractional density amplitude peaks around 46 RS and the wave energy flux decreases beyond ~6 RS , implying that the acoustic waves dissipate to heat the corona. The acoustic wave energy fluxes in the fast solar wind tend to exceed those in the slow wind, suggesting that the fast wind is powered by a larger injection of Alfven wave energy than the slow wind. Title: Three-body description of 9C: Role of low-lying resonances in breakup reactions Authors: Singh, Jagjit; Matsumoto, Takuma; Fukui, Tokuro; Ogata, Kazuyuki Bibcode: 2021PhRvC.104c4612S Altcode: 2021arXiv210309511S Background: The 9C nucleus and related capture reaction, 8B (p ,γ ) 9C , have been intensively studied with an astrophysical interest. Due to the weakly bound nature of 9C, its structure is likely to be described as the three-body (7Be +p +p ). Its continuum structure is also important to describe reaction processes of 9C, with which the reaction rate of the 8B (p ,γ ) 9C process have been extracted indirectly.

Purpose: We preform three-body calculations on 9C and discuss properties of its ground and low-lying states via breakup reactions.

Methods: We employ the three-body model of 9C using the Gaussian-expansion method combined with the complex-scaling method. This model is implemented in the four-body version of the continuum-discretized coupled-channels method, by which breakup reactions of 9C are studied. The intrinsic spin of 7Be is disregarded.

Results: By tuning a three-body interaction in the Hamiltonian of 9C, we obtain the low-lying 2+ state with the resonant energy 0.781 MeV and the decay width 0.137 MeV, which is consistent with the available experimental information and a relatively high-lying second 2+ wider resonant state. Our calculation predicts also sole 0+ and three 1− resonant states. We discuss the role of these resonances in the elastic breakup cross section of 9C on 208Pb at 65 and 160 MeV/nucleon.

Conclusions: The low-lying 2+ state is probed as a sharp peak of the breakup cross section, while the 1− states enhance the cross section around 3 MeV. Our calculations will further support the future and ongoing experimental campaigns for extracting astrophysical information and evaluating the two-proton removal cross sections. Title: Full compressible 3D MHD simulation of solar wind Authors: Matsumoto, Takuma Bibcode: 2021MNRAS.500.4779M Altcode: 2020arXiv200903770M; 2020MNRAS.tmp.3336M Identifying the heating mechanisms of the solar corona and the driving mechanisms of solar wind are key challenges in understanding solar physics. A full three-dimensional compressible magnetohydrodynamic (MHD) simulation was conducted to distinguish between the heating mechanisms in the fast solar wind above the open field region. Our simulation describes the evolution of the Alfvénic waves, which includes the compressible effects from the photosphere to the heliospheric distance s of 27 solar radii (R⊙). The hot corona and fast solar wind were reproduced simultaneously due to the dissipation of the Alfvén waves. The inclusion of the transition region and lower atmosphere enabled us to derive the solar mass-loss rate for the first time by performing a full three-dimensional compressible MHD simulation. The Alfvén turbulence was determined to be the dominant heating mechanism in the solar wind acceleration region (s > 1.3 R⊙), as suggested by previous solar wind models. In addition, shock formation and phase mixing are important below the lower transition region (s < 1.03 R⊙) as well. Title: Thermal responses in a coronal loop maintained by wave heating mechanisms Authors: Matsumoto, Takuma Bibcode: 2018MNRAS.476.3328M Altcode: 2018MNRAS.tmp..477M; 2017arXiv171207377M A full 3-dimensional compressible magnetohydrodynamic (MHD) simulation is conducted to investigate the thermal responses of a coronal loop to the dynamic dissipation processes of MHD waves. When the foot points of the loop are randomly and continuously forced, the MHD waves become excited and propagate upward. Then, 1-MK temperature corona is produced naturally as the wave energy dissipates. The excited wave packets become non-linear just above the magnetic canopy, and the wave energy cascades into smaller spatial scales. Moreover, collisions between counter-propagating Alfvén wave packets increase the heating rate, resulting in impulsive temperature increases. Our model demonstrates that the heating events in the wave-heated loops can be nanoflare-like in the sense that they are spatially localized and temporally intermittent. Title: Importance of MHD Waves Observed with Hinode Authors: Matsumoto, Takuma Bibcode: 2018ASSL..449...79M Altcode: No abstract at ADS Title: Competition between shock and turbulent heating in coronal loop system Authors: Matsumoto, Takuma Bibcode: 2016MNRAS.463..502M Altcode: 2016MNRAS.tmp.1154M; 2016arXiv160606019M 2.5-dimensional magnetohydrodynamic (MHD) simulations are performed with high spatial resolution in order to distinguish between competing models of the coronal heating problem. A single coronal loop powered by Alfvén waves excited in the photosphere is the target of this study. The coronal structure is reproduced in our simulations as a natural consequence of the transportation and dissipation of Alfvén waves. Further, the coronal structure is maintained as the spatial resolution is changed from 25 to 3 km, although the temperature at the loop top increases with the spatial resolution. The heating mechanisms change gradually across the magnetic canopy at a height of 4 Mm. Below the magnetic canopy, both the shock and the MHD turbulence are dominant heating processes. Above the magnetic canopy, the shock heating rate reduces to less than 10 per cent of the total heating rate while the MHD turbulence provides significant energy to balance the radiative cooling and thermal conduction loss or gain. The importance of compressibility shown in this study would significantly impact on the prospects of successful MHD turbulence theory in the solar chromosphere. Title: Magnetohydrodynamic Shocks in and above Post-flare Loops: Two-dimensional Simulation and a Simplified Model Authors: Takasao, Shinsuke; Matsumoto, Takuma; Nakamura, Naoki; Shibata, Kazunari Bibcode: 2015ApJ...805..135T Altcode: 2015arXiv150405700T Solar flares are an explosive phenomenon where super-sonic flows and shocks are expected in and above the post-flare loops. To understand the dynamics of post-flare loops, a two-dimensional magnetohydrodynamic (2D MHD) simulation of a solar flare has been carried out. We found new shock structures in and above the post-flare loops, which were not resolved in the previous work by Yokoyama & Shibata. To study the dynamics of flows along the reconnected magnetic field, the kinematics and energetics of the plasma are investigated along selected field lines. It is found that shocks are crucial to determine the thermal and flow structures in the post-flare loops. On the basis of the 2D MHD simulation, we developed a new post-flare loop model, which we defined as the pseudo-2D MHD model. The model is based on the one-dimensional (1D) MHD equations, where all variables depend on one space dimension, and all the three components of the magnetic and velocity fields are considered. Our pseudo-2D model includes many features of the multi-dimensional MHD processes related to magnetic reconnection (particularly MHD shocks), which the previous 1D hydrodynamic models are not able to include. We compared the shock formation and energetics of a specific field line in the 2D calculation with those in our pseudo-2D MHD model, and found that they give similar results. This model will allow us to study the evolution of the post-flare loops in a wide parameter space without expensive computational cost or neglecting important physics associated with magnetic reconnection. Title: Saturation of Stellar Winds from Young Suns Authors: Suzuki, Takeru K.; Imada, Shinsuke; Kataoka, Ryuho; Kato, Yoshiaki; Matsumoto, Takuma; Miyahara, Hiroko; Tsuneta, Saku Bibcode: 2013PASJ...65...98S Altcode: 2012arXiv1212.6713S We investigated mass losses via stellar winds from Sun-like main-sequence stars with a wide range of activity levels. We performed forward-type magnetohydrodynamical numerical experiments for Alfvén wave-driven stellar winds with a wide range of input Poynting flux from the photosphere. Increasing the magnetic field strength and the turbulent velocity at the stellar photosphere from the current solar level, the mass-loss rate rapidly at first increases, owing to suppression of the reflection of the Alfvén waves. The surface materials are lifted up by the magnetic pressure associated with the Alfvén waves, and the cool dense chromosphere is intermittently extended to 10%#8211;20% of the stellar radius. The dense atmospheres enhance the radiative losses, and eventually most of the input Poynting energy from the stellar surface escapes by radiation. As a result, there is no more sufficient energy remaining for the kinetic energy of the wind; the stellar wind saturates in very active stars, as observed in Wood et al. (2002, ApJ, 574, 412; 2005, ApJ, 628, L143). The saturation level is positively correlated with Br,0 f0, where Br,0 and f0 are the magnetic field strength and the filling factor of open flux tubes at the photosphere. If Br,0 f0 is relatively large gtrsim 5 G, the mass-loss rate could be as high as 1000 times. If such a strong mass loss lasts for ∼ 1 billion years, the stellar mass itself would be affected, which could be a solution to the faint young Sun paradox. We derived a Reimers-type scaling relation that estimates the mass-loss rate from an energetics consideration of our simulations. Finally, we derived the evolution of the mass-loss rates, dot;{M} ∝ t-1.23, of our simulations, combining with an observed time evolution of X-ray flux from Sun-like stars, which are shallower than dot;{M} ∝ t-2.33±0.55 in Wood et al. (2005). Title: Connecting the photosphere and the solar wind Authors: Matsumoto, Takuma; Suzuki, Takeru Ken Bibcode: 2013AIPC.1539...38M Altcode: We have performed 2.5 dimensional magnetohydrodynamic simulations for Alfvén wave propagation in the solar atmosphere. The coronal heating and the solar wind acceleration problems are our main target. Our simulation is self-consistent one in terms of the fact that we do not assume any background atmospheric structures. The hot corona and the high speed solar wind appeared in our numerical simulation as a natural consequence of Alfvén wave injection from the photosphere. Significant amount of the Alfvén wave energy is converted into the longitudinal wave around the chromosphere. The longitudinal wave damped rapidly as they propagated upward to the corona, which suggests that the shock heating is efficient in the low corona. Although the turbulent cascade was efficient dissipation mechanism in our simulation, we will concentrate on the shock heating mechanisms in this paper. Title: Connecting the Sun and the Solar Wind: The First 2.5-dimensional Self-consistent MHD Simulation under the Alfvén Wave Scenario Authors: Matsumoto, Takuma; Suzuki, Takeru Ken Bibcode: 2012ApJ...749....8M Altcode: 2011arXiv1109.6707M The solar wind emanates from the hot and tenuous solar corona. Earlier studies using 1.5-dimensional simulations show that Alfvén waves generated in the photosphere play an important role in coronal heating through the process of nonlinear mode conversion. In order to understand the physics of coronal heating and solar wind acceleration together, it is important to consider the regions from photosphere to interplanetary space as a single system. We performed 2.5-dimensional, self-consistent magnetohydrodynamic simulations, covering from the photosphere to the interplanetary space for the first time. We carefully set up the grid points with spherical coordinates to treat the Alfvén waves in the atmosphere with huge density contrast and successfully simulate the solar wind streaming out from the hot solar corona as a result of the surface convective motion. The footpoint motion excites Alfvén waves along an open magnetic flux tube, and these waves traveling upward in the non-uniform medium undergo wave reflection, nonlinear mode conversion from Alfvén mode to slow mode, and turbulent cascade. These processes lead to the dissipation of Alfvén waves and acceleration of the solar wind. It is found that the shock heating by the dissipation of the slow-mode wave plays a fundamental role in the coronal heating process, whereas the turbulent cascade and shock heating drive the solar wind. Title: Propagation of Moreton Waves Authors: Zhang, Yuzong; Kitai, Reizaburo; Narukage, Noriyuki; Matsumoto, Takuma; Ueno, Satoru; Shibata, Kazunari; Wang, Jingxiu Bibcode: 2011PASJ...63..685Z Altcode: With the Flare-Monitoring Telescope (FMT) and Solar Magnetic Activity Research Telescope (SMART) at Hida observatory of Kyoto University, 13 events of Moreton waves were captured at Hα center, Hα ±0.5 Å, and Hα ±0.8 Å wavebands since 1997. With such samples, we have studied the statistical properties of the propagation of Moreton waves. Moreton waves were all restricted in sectorial zones with a mean value of 92°. However, their accompanying EIT waves, observed simultaneously with SOHO/EIT at extreme-ultraviolet wavelength, were very isotropic with a quite extended scope of 193°. The average propagation speeds of the Moreton waves and the corresponding EIT waves were 664 km s-1 and 205 km s-1, respectively. Moreton waves propagated either under large-scale close magnetic flux loops, or firstly in the sectorial region where two sets of magnetic loops separated from each other and diverged, and then stopped before the open magnetic flux region. The location swept by Moreton waves had a relatively weak magnetic field as compared to the magnetic fields at their sidewalls. The ratio of the magnetic flux density between the sidewall and the path falls in the range of 1.4 to 3.7 at a height of 0.01 solar radii. Additionally, we roughly estimated the distribution of the fast magnetosonic speed between the propagating path and sidewalls in an event on 1997 November 3, and found a relatively low-fast magnetosonic speed in the path. We also found that the propagating direction of Moreton waves coincided with the direction of filament eruption in a few well-observed events. This favors an interpretation of the ``Piston'' model, although further studies are necessary for any definitive conclusion. 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: Temporal Power Spectra of the Horizontal Velocity of the Solar Photosphere Authors: Matsumoto, Takuma; Kitai, Reizaburo Bibcode: 2010ApJ...716L..19M Altcode: 2010arXiv1004.5173M We have derived the temporal power spectra of the horizontal velocity of the solar photosphere. The data sets for 14 quiet regions observed with the G-band filter of Hinode/SOT are analyzed to measure the temporal fluctuation of the horizontal velocity by using the local correlation tracking (LCT) method. Among the high resolution (~0farcs2) and seeing-free data sets of Hinode/SOT, we selected the observations whose duration is longer than 70 minutes and cadence is about 30 s. The so-called k-ω diagrams of the photospheric horizontal velocity are derived for the first time to investigate the temporal evolution of convection. The power spectra derived from k-ω diagrams typically have a double power-law shape bent over at a frequency of 4.7 mHz. The power-law index in the high frequency range is -2.4, while the power-law index in the low frequency range is -0.6. The root mean square of the horizontal speed is about 1.1 km s-1 when we use a tracer size of 0farcs4 in the LCT method. Autocorrelation functions of intensity fluctuation, horizontal velocity, and its spatial derivatives are also derived in order to measure the correlation time of the stochastic photospheric motion. Since one of the possible energy sources of the coronal heating is the photospheric convection, the power spectra derived in the present study will be of high value to quantitatively justify various coronal heating models. Title: Nonlinear Propagation of Alfvén Waves Driven by Observed Photospheric Motions: Application to the Coronal Heating and Spicule Formation Authors: Matsumoto, Takuma; Shibata, Kazunari Bibcode: 2010ApJ...710.1857M Altcode: 2010arXiv1001.4307M We have performed MHD simulations of Alfvén wave propagation along an open flux tube in the solar atmosphere. In our numerical model, Alfvén waves are generated by the photospheric granular motion. As the wave generator, we used a derived temporal spectrum of the photospheric granular motion from G-band movies of Hinode/Solar Optical Telescope. It is shown that the total energy flux at the corona becomes larger and the transition region's height becomes higher in the case when we use the observed spectrum rather than the white/pink noise spectrum as the wave generator. This difference can be explained by the Alfvén wave resonance between the photosphere and the transition region. After performing Fourier analysis on our numerical results, we have found that the region between the photosphere and the transition region becomes an Alfvén wave resonant cavity. We have confirmed that there are at least three resonant frequencies, 1, 3, and 5 mHz, in our numerical model. Alfvén wave resonance is one of the most effective mechanisms to explain the dynamics of the spicules and the sufficient energy flux to heat the corona. Title: Nonlinear Propagation of Alfven Waves Driven by Observed Photospheric Motions: Application to the Coronal Heating and Spicule Formation Authors: Matsumoto, Takuma; Shibata, Kazunari Bibcode: 2010cosp...38.2919M Altcode: 2010cosp.meet.2919M We have performed MHD simulations of Alfven wave propagation along an open ux tube in the solar atmosphere. In our numerical model, Alfven waves are generated by the photospheric granular motion. As the wave generator, we used a derived temporal spectrum of the photo-spheric granular motion from G-band movies of Hinode/SOT. It is shown that the total energy ux at the corona becomes larger and the transition region height becomes higher in the case when we use the observed spectrum rather than white/pink noise spectrum as the wave gener-ator. This difference can be explained by the Alfven wave resonance between the photosphere and the transition region. After performing Fourier analysis on our numerical results, we have found that the region between the photosphere and the transition region becomes an Alfven wave resonant cavity. We have conrmed that there are at least three resonant frequencies, 1, 3 and 5 mHz, in our numerical model. Alfven wave resonance is one of the most effective mechanisms to explain the dynamics of the spicules and the sufficient energy ux to heat the corona. 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: Multi-scale Interlocked Simulation of Solar Eruption Authors: Kusano, Kanya; Sugiyama, Tooru; Inoue, Satoshi; Shiota, Daiko; Asano, Eiji; Matsumoto, Takuma; Kataoka, Ryuho; Shibata, Kazunari Bibcode: 2008cosp...37.1659K Altcode: 2008cosp.meet.1659K The onset process of solar eruption, which arises as solar flares and/or coronal mass ejections (CME), is one of the most important subject in space and astrophysical plasma physics, because it is the typical phenomena of the explosive energy liberation in plasma as well as the primary cause of space weather disturbances. However, not only the onset mechanism but even the physical condition to trigger it are not yet well clarified. In particular, the mutual relationship between large-scale magnetic configuration and small-scale reconnection dynamics in the CME initiation is hardly understood, although it is quite important from the view point both of the multi-scale plasma physics and the space weather forecast. The objective of this paper is to develop a new type of simulation framework to shed a light to this long-standing problem. Our simulation is performed by the incorporation of multiple models, each of which can calculate the different dynamics at different scales. They are constituted of the active region model, the global corona model, the interplanetary space model, and the fluid-particle interlocked model, which is able to handle the calculation of energetic particle acceleration in macro-scale magnetic environment. We have applied the new model to simulate the eruptive event caused by the X-class flare occurred on December 13, 2006, using vector magnetic field data observed by Hinode, Solar Optical Telescope. In this talk, after a brief review of the theories proposed so far for the flare and CME initiation, we show the basic algorithm of our model. Then, we present the result of the first-ever datadriven simulation of the solar eruption. The detail comparison between the simulation and the observation is also reported. Finally, we are discussing about the predictability of solar eruption, based on the numerical experiments with the multi-scale interlocked model. 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.