Author name code: hara ADS astronomy entries on 2022-09-14 author:"Hara, Hirohisa" ------------------------------------------------------------------------ Title: Quiet Sun Center to Limb Variation of the Linear Polarization Observed by CLASP2 Across the Mg II h and k Lines Authors: Rachmeler, L. A.; Bueno, J. Trujillo; McKenzie, D. E.; Ishikawa, R.; Auchère, F.; Kobayashi, K.; Kano, R.; Okamoto, T. J.; Bethge, C. W.; Song, D.; Ballester, E. Alsina; Belluzzi, L.; Pino Alemán, T. del; Ramos, A. Asensio; Yoshida, M.; Shimizu, T.; Winebarger, A.; Kobelski, A. R.; Vigil, G. D.; Pontieu, B. De; Narukage, N.; Kubo, M.; Sakao, T.; Hara, H.; Suematsu, Y.; Štěpán, J.; Carlsson, M.; Leenaarts, J. Bibcode: 2022ApJ...936...67R Altcode: 2022arXiv220701788R The CLASP2 (Chromospheric LAyer Spectro-Polarimeter 2) sounding rocket mission was launched on 2019 April 11. CLASP2 measured the four Stokes parameters of the Mg II h and k spectral region around 2800 Å along a 200″ slit at three locations on the solar disk, achieving the first spatially and spectrally resolved observations of the solar polarization in this near-ultraviolet region. The focus of the work presented here is the center-to-limb variation of the linear polarization across these resonance lines, which is produced by the scattering of anisotropic radiation in the solar atmosphere. The linear polarization signals of the Mg II h and k lines are sensitive to the magnetic field from the low to the upper chromosphere through the Hanle and magneto-optical effects. We compare the observations to theoretical predictions from radiative transfer calculations in unmagnetized semiempirical models, arguing that magnetic fields and horizontal inhomogeneities are needed to explain the observed polarization signals and spatial variations. This comparison is an important step in both validating and refining our understanding of the physical origin of these polarization signatures, and also in paving the way toward future space telescopes for probing the magnetic fields of the solar upper atmosphere via ultraviolet spectropolarimetry. Title: Development of Fast and Precise Scan Mirror Mechanism for an Airborne Solar Telescope Authors: Oba, Takayoshi; Shimizu, Toshifumi; Katsukawa, Yukio; Kubo, Masahito; Kawabata, Yusuke; Hara, Hirohisa; Uraguchi, Fumihiro; Tsuzuki, Toshihiro; Tamura, Tomonori; Shinoda, Kazuya; Kodeki, Kazuhide; Fukushima, Kazuhiko; Morales Fernández, José Miguel; Sánchez Gómez, Antonio; Balaguer Jimenéz, María; Hernández Expósito, David; Gandorfer, Achim Bibcode: 2022arXiv220713864O Altcode: We developed a scan mirror mechanism (SMM) that enable a slit-based spectrometer or spectropolarimeter to precisely and quickly map an astronomical object. The SMM, designed to be installed in the optical path preceding the entrance slit, tilts a folding mirror and then moves the reflected image laterally on the slit plane, thereby feeding a different one-dimensional image to be dispersed by the spectroscopic equipment. In general, the SMM is required to scan quickly and broadly while precisely placing the slit position across the field-of-view (FOV). These performances are highly in demand for near-future observations, such as studies on the magnetohydrodynamics of the photosphere and the chromosphere. Our SMM implements a closed-loop control system by installing electromagnetic actuators and gap-based capacitance sensors. Our optical test measurements confirmed that the SMM fulfils the following performance criteria: i) supreme scan-step uniformity (linearity of 0.08%) across the wide scan range (${\pm}$1005 arcsec), ii) high stability (3${\sigma}$ = 0.1 arcsec), where the angles are expressed in mechanical angle, and iii) fast stepping speed (26 ms). The excellent capability of the SMM will be demonstrated soon in actual use by installing the mechanism for a near-infrared spectropolarimeter onboard the balloon-borne solar observatory for the third launch, Sunrise III. Title: A spectral solar irradiance monitor (SoSpIM) on the JAXA Solar-C (EUVST) space mission Authors: Harra, Louise K.; Watanabe, Kyoko; Haberreiter, Margit; Hori, Tomoaki; Hara, Hirohisa; Kretzschmar, Matthieu; Woods, Thomas; Shimizu, Toshifumi; Krucker, Samuel; Berghmans, David; Jin, Hidekatsu; Dominique, Marie; Eparvier, Francis G.; Gissot, Samuel; Leng Yeo, Kok; Pfiffner, Dany; Milligan, Ryan; Thiemann, Edward; Miyoshi, Yoshizumi; Imada, Shinsuke; Kawate, Tomoko; Chamberlin, Phillip; Rozanov, Eugene; Silvio Koller, -.; Barczynski, Krzysztof; Nozomu; Nishitani; Ieda, Akimasa; Langer, Patrick; Meier, Leandro; Tye, Daniel; Alberti, Andrea Bibcode: 2022cosp...44..834H Altcode: The JAXA Solar-C (EUVST) mission (Shimizu et al., 2020) is designed to comprehensively understand how mass and energy are transferred throughout the solar atmosphere. The EUV High-Throughput Spectroscopic Telescope (EUVST) onboard does this by observing all the temperature regimes of the atmosphere from the chromosphere to the corona simultaneously. To enhance the EUVST scientific capabilities, there will be a Solar Spectral Irradiance Monitor (SoSpIM). SoSpIM will work hand-in-hand scientifically with EUVST, by providing the full Sun irradiance at sub-second time cadence combined with the spatially resolved spectroscopy from EUVST. The SoSPIM instrument will specifically address two aspects. These are: · Understand how the solar atmosphere becomes unstable, releasing the energy that drives solar flares - achieved through probing fast time cadence solar flare variations. · Measuring solar irradiance that impacts the Earth's thermosphere and the mesosphere, linking to spatially resolved measurements of the solar atmosphere with EUVST. SoSpIM will provide high time resolution measurements in 2 channels (a) in the corona through channel 1 (EUV) and (b) in the lower atmosphere through channel 2 (Lyman alpha). Each channel impacts different layers of the Earth's atmosphere. Title: How Can Solar-C/SOSPIM Contribute to the Understanding of Quasi-Periodic Pulsations in Solar Flares? Authors: Dominique, Marie; Harra, Louise K.; Watanabe, Kyoko; Hara, Hirohisa; Zhukov, Andrei; Shimizu, Toshifumi; Berghmans, David; Dolla, Laurent; Gissot, Samuel; Pfiffner, Dany; Imada, Shinsuke; Silvio Koller, -.; Meier, Leandro; Tye, Daniel; Alberti, Andrea Bibcode: 2022cosp...44.2524D Altcode: Quasi-periodic pulsations (QPPs) refer to nearly-periodic oscillations that are often observed in irradiance time series during solar flares and have also been reported in several stellar flares. In the last years, several statistical studies based on Soft X-ray measurements have reached the conclusion that QPPs are present in most solar flares of class M and above. Still, as of today, we are still unsure of what causes QPPs. Several models could explain the presence of QPPs with periods matching the ones observed. More detailed analysis of the observational signatures of QPPs might help determine which of those models are actually playing a role in the generation of QPPs. However, as QPPs is a small timescale process (the period of QPPs is often reported to be less than a minute), such an analysis requires instruments with a good signal-to-noise and high sampling rate. In this context, the spectral solar irradiance monitor SOSPIM, that will be part of the JAXA SOLAR C mission and that will complement the EUVST spectrograph measurements, could be a valuable asset. SOSPIM will observe the solar chromosphere and corona in the Lyman-alpha and EUV spectral ranges at high cadence. In this presentation, we review the current knowledge of QPPs and describe what could be the contribution of SOSPIM to push their understanding one step forward. Title: Probing Upflowing Regions in the Quiet Sun and Coronal Holes Authors: Schwanitz, Conrad; Harra, Louise; Raouafi, Nour E.; Sterling, Alphonse C.; Moreno Vacas, Alejandro; del Toro Iniesta, Jose Carlos; Orozco Suárez, David; Hara, Hirohisa Bibcode: 2021SoPh..296..175S Altcode: 2021arXiv211012753S Recent observations from Parker Solar Probe have revealed that the solar wind has a highly variable structure. How this complex behaviour is formed in the solar corona is not yet known, since it requires omnipresent fluctuations, which constantly emit material to feed the wind. In this article we analyse 14 upflow regions in the solar corona to find potential sources for plasma flow. The upflow regions are derived from spectroscopic data from the EUV Imaging Spectrometer (EIS) on board Hinode determining their Doppler velocity and defining regions which have blueshifts stronger than −6 kms−1. To identify the sources of these blueshift data from the Atmospheric Imaging Assembly (AIA) and the Helioseismic and Magnetic Imager (HMI), on board the Solar Dynamics Observatory (SDO), and the X-ray Telescope (XRT), on board Hinode, are used. The analysis reveals that only 5 out of 14 upflows are associated with frequent transients, like obvious jets or bright points. In contrast to that, seven events are associated with small-scale features, which show a large variety of dynamics. Some resemble small bright points, while others show an eruptive nature, all of which are faint and only live for a few minutes; we cannot rule out that several of these sources may be fainter and, hence, less obvious jets. Since the complex structure of the solar wind is known, this suggests that new sources have to be considered or better methods used to analyse the known sources. This work shows that small and frequent features, which were previously neglected, can cause strong upflows in the solar corona. These results emphasise the importance of the first observations from the Extreme-Ultraviolet Imager (EUI) on board Solar Orbiter, which revealed complex small-scale coronal structures. Title: How Can Solar-C/SOSPIM Contribute to the Understanding of Quasi-Periodic Pulsations in Solar Flares? Authors: Dominique, Marie; Dolla, Laurent; Zhukov, Andrei; Alberti, Andrea; Berghmans, David; Gissot, Samuel; Hara, Hirohisa; Harra, Louise; Imada, Shinsuke; Koller, Silvio; Meier, Leandro; Pfiffner, Daniel; Shimizu, Toshifumi; Tye, Daniel; Watanabe, Kyoko Bibcode: 2021AGUFMSH25E2124D Altcode: Quasi-periodic pulsations (QPPs) refer to nearly-periodic oscillations that are often observed in irradiance time series during solar flares and have also been reported in several stellar flares. In the last years, several statistical studies based on Soft X-ray measurements have reached the conclusion that QPPs are present in most solar flares of class M and above. Still, the mechanism at the origin of QPPs is under debate. Are they caused by waves or periodic fluctuations of the magnetic reconnection driving the flare? Analyzing the characteristics of QPPs and their evolution during the flare could help identifying their origin. However, QPPs sometimes exhibit very different periodicities, and do not always happen during the same phase of the flare. All this could point to the coexistence of QPPs with different origin mechanism, and indicates the need for more observations. In this context, the spectral solar irradiance monitor SOSPIM, that will be part of the JAXA SOLAR C mission and that will complement the EUVST spectrograph measurements, could be a valuable asset. SOSPIM will observe the solar chromosphere and corona in the Lyman-alpha and EUV spectral ranges at high cadence. In this presentation, we review the current knowledge of QPPs and describe what could be the contribution of SOSPIM to push their understanding one step forward. Title: Electron Density Dependence of Extreme Ultraviolet Line Intensity Ratios in Ar XIV Authors: Nakamura, Nobuyuki; Numadate, Naoki; Kono, Yasutaka; Murakami, Izumi; Kato, Daiji; Sakaue, Hiroyuki A.; Hara, Hirohisa Bibcode: 2021ApJ...921..115N Altcode: We report the electron density dependence of extreme ultraviolet line intensity ratios in Ar XIV studied using a well-defined electron beam ion trap plasma. The purpose of this study is to examine the potential of the Ar XIV lines in diagnosing the electron density of solar corona active regions with a temperature higher than 3 MK. The experimentally obtained dependence is in good agreement with collisional-radiative model calculations, which ensures the usability of the Ar XIV lines. Title: Mapping of Solar Magnetic Fields from the Photosphere to the Top of the Chromosphere with CLASP2 Authors: McKenzie, D.; Ishikawa, R.; Trujillo Bueno, J.; Auchere, F.; del Pino Aleman, T.; Okamoto, T.; Kano, R.; Song, D.; Yoshida, M.; Rachmeler, L.; Kobayashi, K.; Narukage, N.; Kubo, M.; Ishikawa, S.; Hara, H.; Suematsu, Y.; Sakao, T.; Bethge, C.; De Pontieu, B.; Vigil, G.; Winebarger, A.; Alsina Ballester, E.; Belluzzi, L.; Stepan, J.; Asensio Ramos, A.; Carlsson, M.; Leenaarts, J. Bibcode: 2021AAS...23810603M Altcode: Coronal heating, chromospheric heating, and the heating & acceleration of the solar wind, are well-known problems in solar physics. Additionally, knowledge of the magnetic energy that powers solar flares and coronal mass ejections, important drivers of space weather, is handicapped by imperfect determination of the magnetic field in the sun's atmosphere. Extrapolation of photospheric magnetic measurements into the corona is fraught with difficulties and uncertainties, partly due to the vastly different plasma beta between the photosphere and the corona. Better results in understanding the coronal magnetic field should be derived from measurements of the magnetic field in the chromosphere. To that end, we are pursuing quantitative determination of the magnetic field in the chromosphere, where plasma beta transitions from greater than unity to less than unity, via ultraviolet spectropolarimetry. The CLASP2 mission, flown on a sounding rocket in April 2019, succeeded in measuring all four Stokes polarization parameters in UV spectral lines formed by singly ionized Magnesium and neutral Manganese. Because these ions produce spectral lines under different conditions, CLASP2 thus was able to quantify the magnetic field properties at multiple heights in the chromosphere simultaneously, as shown in the recent paper by Ishikawa et al. In this presentation we will report the findings of CLASP2, demonstrating the variation of magnetic fields along a track on the solar surface and as a function of height in the chromosphere; and we will illustrate what is next for the CLASP missions and the demonstration of UV spectropolarimetry in the solar chromosphere. Title: Instrumental design of the Solar Observing Satellite: solar-C_EUVST Authors: Suematsu, Yoshinori; Shimizu, Toshifumi; Hara, Hirohisa; Kawate, Tomoko; Katsukawa, Yukio; Ichimoto, Kiyoshi; Imada, Shinsuke Bibcode: 2021SPIE11852E..3KS Altcode: The EUV High-Throughput Spectroscopic Telescope (EUVST) of Solar-C mission is a revolutionary spectrometer that is designed to provide high-quality and high cadence spectroscopic data covering a wide temperature range of the chromosphere to flaring corona to investigate the energetics and dynamics of the solar atmosphere. The EUVST consists of only two imaging optical components; a 28-cm clear aperture off-axis parabolic primary mirror and a two-split ellipsoidal grating without a blocking filter for visible light before the primary mirror to achieve unprecedented high spatial and temporal resolution in EUV-UV imaging spectroscopic observations. For this reason, about 53 W of sunlight is absorbed by the multilayer coating on the mirror. We present an instrumental design of the telescope, particularly, primary mirror assembly which enables slit-scan observations for imaging spectroscopy, an image stabilizing tip-tilt control, and a focus adjustment on orbit, together with an optomechanical design of the primary mirror and its supporting system which gives optically tolerant wavefront error against a large temperature increase due to an absorption of visible and IR lights. Title: GRB 210308A: MITSuME Okayama optical upper limits Authors: Ogata, S.; Hosokawa, R.; Murata, K. L.; Adachi, R.; Niwano, M.; Ogawa, F.; Nakamura, N.; Ito, N.; Takamatsu, H.; Hara, H.; Yatsu, Y.; Kawai, N.; MITSuME Collaboration Bibcode: 2021GCN.29621....1O Altcode: We observed the field of GRB 210308A (D'Elia et al.,GCN Circular #29619) with the optical three color (g', Rc, and Ic) CCD cameras attached to the MITSuME 50 cm telescope of Okayama Astrophysical Observatory, Okayama, Japan. The observation with a series of 60 sec exposures started at 2021-03-08 11:03:59 UT.(4.5 hours after Swift BAT trigger) We stacked the images with good conditions. We did not detect the optical afterglow reported previously (D'Elia et al.,GCN Circular #29619) in all three bands. We obtained the 5-sigma limits of the stacked images as follows. T0+[hour] MID-UT T-EXP[sec] 5-sigma limits ------------------------------------------------------------------------------------------------ 4.5 11:51:53 4440 g'>17.6, Rc>17.8, Ic>17.8 ------------------------------------------------------------------------------------------------ T0+ : Elapsed time after the burst T-EXP: Total Exposure time We used the PS1 catalog for flux calibration. The magnitudes are expressed in the AB system. The images were processed in real-time through the MITSuME GPU reduction pipeline (Niwano et al. 2021, PASJ, Vol.73, Issue 1, Pages 4-24; https://github.com/MNiwano/Eclaire). Title: GRB 210306A: MITSuME Akeno optical observation Authors: Hosokawa, R.; Adachi, R.; Murata, K. L.; Niwano, M.; Ogawa, F.; Nakamura, N.; Ito, N.; Ogata, S.; Takamatsu, H.; Hara, H.; Yatsu, Y.; Kawai, N.; MITSuME Collaboration Bibcode: 2021GCN.29608....1H Altcode: We observed the field of GRB 210306A (D'Elia et al. GCN #29597, Watson et al. GCN 29598, Romanov GCN #29599, Strausbaugh et al. GCN #29600, Ohno et al. GCN #29602, Hentunen et al. GCN #29603, Stecklum et al. GCN #29604, Veres et al. GCN #29605, Lipunov et al. GCN #29606, Zhu et al. GCN #29607) with the optical three color (g', Rc, and Ic) CCD cameras attached to the MITSuME 50 cm telescope of Akeno Observatory, Yamanashi, Japan. The observation with a series of 60 sec exposures started at 2021-03-06 09:12:03 UT (5.3 hours after Swift BAT trigger). We stacked the images with good conditions. We marginally detected the point source at the position consistent with the afterglow detected previously(D'Elia et al. GCN #29597, Watson et al. GCN 29598, Romanov GCN #29599, Strausbaugh et al. GCN #29600, Hentunen et al. GCN #29603, Stecklum et al. GCN #29604, Zhu et al. GCN #29607). We measured the magnitudes as follows. T0+[hour] MID-UT T-EXP[sec] measured magnitudes ------------------------------------------------------------------------------------------------ 5.3 11:38:10 8160 g'=20.0+/-0.4, Rc=20.2+/-0.4, Ic=19.0+/-0.3 ------------------------------------------------------------------------------------------------ T0+ : Elapsed time after the burst T-EXP: Total Exposure time We used PS1 catalog for flux calibration. The magnitudes are expressed in the AB system. The images were processed in real-time through the MITSuME GPU reduction pipeline (Niwano et al. 2021, PASJ, Vol.73, Issue 1, Pages 4-24; https://github.com/MNiwano/Eclaire). Title: GRB 210318B: MITSuME Okayama optical upper limits Authors: Hosokawa, R.; Murata, K. L.; Adachi, R.; Niwano, M.; Ogawa, F.; Nakamura, N.; Ito, N.; Ogata, S.; Takamatsu, H.; Hara, H.; Yatsu, Y.; Kawai, N.; MITSuME Collaboration Bibcode: 2021GCN.29675....1H Altcode: We observed the field of GRB 210318B (Troja et al. GCN Circular #29663, Svinkin et al. GCN Circular #29664, Stamatikos et al. GCN Circular #29666, Lipunov et al. GCN Circular #29667, Malacaria et al. GCN Circular #29668) with the optical three color (g', Rc, and Ic) CCD cameras attached to the MITSuME 50 cm telescope of Okayama Astrophysical Observatory, Okayama, Japan. The observation with a series of 60 sec exposures started at 2021-03-19 19:11:03 UT.(40.4 hours after Swift BAT trigger) We stacked the images with good conditions. We did not find any new point sources within the Swift XRT circle (Troja et al. GCN Circular #29663) in all three bands. We obtained the 5-sigma limits of the stacked images as follows. T0+[hour] MID-UT T-EXP[sec] 5-sigma limits ------------------------------------------------------------------------------------------------ 40.4 19:50:32 2040 g'>14.3, Rc>14.2, Ic>13.4 ------------------------------------------------------------------------------------------------ T0+ : Elapsed time after the burst T-EXP: Total Exposure time We used the UCAC4 catalog for flux calibration. The magnitudes are expressed in the AB system. The images were processed in real-time through the MITSuME GPU reduction pipeline (Niwano et al. 2021, PASJ, Vol.73, Issue 1, Pages 4-24; https://github.com/MNiwano/Eclaire). Title: GRB 210212A: MITSuME Akeno optical upper limits Authors: Murata, K. L.; Adachi, R.; Hosokawa, R.; Niwano, M.; Ogawa, F.; Nakamura, N.; Ito, N.; Ogata, S.; Takamatsu, H.; Hara, H.; Yatsu, Y.; Kawai, N.; MITSuME Collaboration Bibcode: 2021GCN.29496....1M Altcode: We observed the field of GRB 210212A (Troja et al. GCN #29487, Beardmore et al. GCN #29489, Palmer et al. GCN #29491, Kuin et al. GCN #29492, Hu et al. GCN #29494, Tohuvavohu et al. GCN #29495) with the optical three color (g', Rc, and Ic) CCD cameras attached to the MITSuME 50 cm telescope of Akeno Observatory, Yamanashi, Japan. The observation with a series of 60 sec exposures started at 2021-02-12 08:51:45 UT(4.43 hours after the Swift BAT trigger). We stacked the images with good conditions. We did not find any new point sources within the enhanced Swift XRT circle (Beardmore et al. GCN #29489) in all three bands. We obtained the 5-sigma limits of the stacked images as follows. T0+[hour] MID-UT T-EXP[sec] 5-sigma limits ------------------------------------------------------------------------------------------------ 8.6 13:05:08 5400 g'>18.6, Rc>18.5, Ic>17.8 ------------------------------------------------------------------------------------------------ T0+ : Elapsed time after the burst T-EXP: Total Exposure time We used the PS1 catalog for flux calibration. The magnitudes are expressed in the AB system. The images were processed in real-time through the MITSuME GPU reduction pipeline (Niwano et al. 2021, PASJ, Vol.73, Issue 1, Pages 4-24; https://github.com/MNiwano/Eclaire). Title: GRB 210222B: MITSuME Akeno optical upper limits Authors: Hosokawa, R.; Murata, K. L.; Adachi, R.; Niwano, M.; Ogawa, F.; Nakamura, N.; Ito, N.; Ogata, S.; Takamatsu, H.; Hara, H.; Yatsu, Y.; Kawai, N.; MITSuME Collaboration Bibcode: 2021GCN.29565....1H Altcode: We observed the field of GRB 210222B (Lipunov et al. GCN #29544, Gropp et al. GCN #29545, Hu et al. GCN #29546, Strausbaugh et al. GCN #29547, Mong et al. GCN #29548, Perley et al. GCN #29549, Mong et al. GCN #29550, Zhu et al. GCN #29551, Fernandez et al. GCN #29552, Lipunov et al. GCN #29554, Jelinek et al. GCN #29557, Zheng et al. GCN #29558, Siegel et al. GCN #29559, Page et al. GCN #29560, Ukwatta et al. GCN #29561, Gokuldass et al. GCN #29562, Belkin et al. GCN #29563) with the optical three color (g', Rc, and Ic) CCD cameras attached to the MITSuME 50 cm telescope of Akeno Observatory, Yamanashi, Japan. The observation with a series of 60 sec exposures started at 2021-02-23 11:00:13 UT(12.4hours after the Swift BAT trigger). We stacked the images with good conditions. We did not detect the optical afterglow reported previously (Gropp et al. GCN #29545, Hu et al. GCN #29546, Strausbaugh et al. GCN #29547, Mong et al. GCN #29548, Perley et al. GCN #29549, Mong et al. GCN #29550, Zhu et al. GCN #29551, Fernandez et al. GCN #29552, Lipunov et al. GCN #29554, Jelinek et al. GCN #29557, Siegel et al. GCN #29559, Gokuldass et al. GCN #29562, Belkin et al. GCN #29563) in all three bands. We obtained the 5-sigma limits of the stacked images as follows. T0+[hour] MID-UT T-EXP[sec] 5-sigma limits ------------------------------------------------------------------------------------------------ 12.4 15:18:25 14100 g'>19.6, Rc>19.9, Ic>19.2 ------------------------------------------------------------------------------------------------ T0+ : Elapsed time after the burst T-EXP: Total Exposure time We used the PS1 catalog for flux calibration. The magnitudes are expressed in the AB system. The images were processed in real-time through the MITSuME GPU reduction pipeline (Niwano et al. 2021, PASJ, Vol.73, Issue 1, Pages 4-24; https://github.com/MNiwano/Eclaire). Title: GRB 210209A: MITSuME Akeno optical upper limits Authors: Hosokawa, R.; Adachi, R.; Murata, K. L.; Niwano, M.; Ogawa, F.; Nakamura, N.; Ito, N.; Ogata, S.; Takamatsu, H.; Hara, H.; Yatsu, Y.; Kawai, N.; MITSuME Collaboration Bibcode: 2021GCN.29455....1H Altcode: We observed the field of GRB 210209A (Laha et al. GCN #29442, Evans et al. GCN #29443, Perri et al. GCN #29449, Breeveld et al. GCN #29453) with the optical three color (g', Rc, and Ic) CCD cameras attached to the MITSuME 50 cm telescope of Akeno Observatory, Yamanashi, Japan. The observation with a series of 60 sec exposures started at 2021-02-10 08:49:41 UT(11.2 hour after the Swift BAT trigger). Since the first 17 images were taken under high airmass conditions, we stacked the images with good conditions. We did not find any new point sources within the enhanced Swift XRT circle (Evans et al. GCN #29443) in all three bands. We obtained the 5-sigma limits of the stacked images as follows. T0+[hour] MID-UT T-EXP[sec] 5-sigma limits ------------------------------------------------------------------------------------------------ 11.2 09:14:41 600 g'>17.2, Rc>17.6, Ic>17.1 ------------------------------------------------------------------------------------------------ T0+ : Elapsed time after the burst T-EXP: Total Exposure time We used the PS1 catalog for flux calibration. The magnitudes are expressed in the AB system. The images were processed in real-time through the MITSuME GPU reduction pipeline (Niwano et al. 2021, PASJ, Vol.73, Issue 1, Pages 4-24; https://github.com/MNiwano/Eclaire). Title: GRB 210218A: MITSuME Akeno optical upper limits Authors: Ogawa, F.; Hosokawa, R.; Murata, K. L.; Adachi, R.; Niwano, M.; Nakamura, N.; Ito, N.; Ogata, S.; Takamatsu, H.; Hara, H.; Yatsu, Y.; Kawai, N.; MITSuME Collaboration Bibcode: 2021GCN.29532....1O Altcode: We observed the field of GRB 210218A (Sbarufatti et al. GCN #29529, Zhu et al. GCN #29530, Xin et al. GCN #29531) with the optical three color (g', Rc, and Ic) CCD cameras attached to the MITSuME 50 cm telescope of Akeno Observatory, Yamanashi, Japan. The observation with a series of 10 sec exposures started at 2021-02-18 13:36:05 UT(46 seconds after the Swift BAT trigger). We stacked the images with good conditions. We did not find any new point sources within the Swift BAT circle (Sbarufatti et al. GCN #29529) in all three bands. We obtained the 5-sigma limits of the stacked images as follows. T0+[sec] MID-UT T-EXP[sec] 5-sigma limits ------------------------------------------------------------------------------------------------ 46 14:03:01 1220 g'>17.3, Rc>17.5, Ic>16.7 ------------------------------------------------------------------------------------------------ T0+ : Elapsed time after the burst T-EXP: Total Exposure time We used the UCAC4 catalog for flux calibration. The magnitudes are expressed in the AB system. The images were processed in real-time through the MITSuME GPU reduction pipeline (Niwano et al. 2021, PASJ, Vol.73, Issue 1, Pages 4-24; https://github.com/MNiwano/Eclaire). Title: Mapping solar magnetic fields from the photosphere to the base of the corona Authors: Ishikawa, Ryohko; Bueno, Javier Trujillo; del Pino Alemán, Tanausú; Okamoto, Takenori J.; McKenzie, David E.; Auchère, Frédéric; Kano, Ryouhei; Song, Donguk; Yoshida, Masaki; Rachmeler, Laurel A.; Kobayashi, Ken; Hara, Hirohisa; Kubo, Masahito; Narukage, Noriyuki; Sakao, Taro; Shimizu, Toshifumi; Suematsu, Yoshinori; Bethge, Christian; De Pontieu, Bart; Dalda, Alberto Sainz; Vigil, Genevieve D.; Winebarger, Amy; Ballester, Ernest Alsina; Belluzzi, Luca; Štěpán, Jiří; Ramos, Andrés Asensio; Carlsson, Mats; Leenaarts, Jorrit Bibcode: 2021SciA....7.8406I Altcode: 2021arXiv210301583I Routine ultraviolet imaging of the Sun's upper atmosphere shows the spectacular manifestation of solar activity; yet we remain blind to its main driver, the magnetic field. Here we report unprecedented spectropolarimetric observations of an active region plage and its surrounding enhanced network, showing circular polarization in ultraviolet (Mg II $h$ & $k$ and Mn I) and visible (Fe I) lines. We infer the longitudinal magnetic field from the photosphere to the very upper chromosphere. At the top of the plage chromosphere the field strengths reach more than 300 gauss, strongly correlated with the Mg II $k$ line core intensity and the electron pressure. This unique mapping shows how the magnetic field couples the different atmospheric layers and reveals the magnetic origin of the heating in the plage chromosphere. Title: GRB 210104A: MITSuME Akeno optical observation Authors: Hosokawa, R.; Adachi, R.; Niwano, M.; Murata, K. L.; Ogawa, F.; Nakamura, N.; Ito, N.; Ogata, S.; Takamatsu, H.; Hara, H.; Yatsu, Y.; Kawai, N.; MITSuME Collaboration Bibcode: 2021GCN.29237....1H Altcode: We observed the field of GRB 210104A (The Fermi GBM team , GCN 29232, E. Troja et al., GCN 29233, B. Biltzinger et al., GCN 29234) with the optical three color (g', Rc, and Ic) CCD cameras attached to the MITSuME 50 cm telescope of Akeno Observatory, Yamanashi, Japan. The observation started at 2021-01-04 11:27:54 UT (55s after Swift BAT trigger). We detected the point source at the position consistent with the afterglow detected previously(E. Troja et al., GCN 29233, L. P. Xin et al., GCN 29235, Y.-D. Hu et al., GCN 29236). We measured the magnitudes as follows. T0+[sec] MID-UT T-EXP[sec] measured magnitudes ------------------------------------------------------------------------------------------------ 55 11:28:24 60 g'=14.6+/-0.1, Rc=14.2+/-0.1, Ic=13.8+/-0.1 ------------------------------------------------------------------------------------------------ T0+ : Elapsed time after the burst T-EXP: Total Exposure time We used PS1 catalog for flux calibration. The magnitudes are expressed in the AB system. The images were processed in real-time through the MITSuME GPU reduction pipeline (Niwano et al., https://doi.org/10.1093/pasj/psaa091, https://arxiv.org/abs/2008.11486; https://github.com/MNiwano/Eclaire). Title: Multicolor-optical observations of the flat-spectrum radio quasar Ton 599 and quasar 3C279 Authors: Hosokawa, R.; Murata, K. L.; Niwano, M.; Wang, S.; Adachi, R.; Ogawa, F.; Nakamura, N.; Ito, N.; Ogata, S.; Takamatsu, H.; Hara, H.; Yatsu, Y.; Kawai, N. Bibcode: 2021ATel14353....1H Altcode: We monitor the flat-spectrum radio quasar Ton 599 with three optical bands (g', Rc, and Ic) using the MITSuME 50 cm Telescopes at Akeno Observatory and Okayama Astrophysical Observatory in Japan. Title: Multicolor-optical observation of the flaring blazar BL Lacertae Authors: Hosokawa, R.; Murata, K. L.; Niwano, M.; Wang, S.; Adachi, R.; Ogawa, F.; Nakamura, N.; Ito, N.; Ogata, S.; Takamatsu, H.; Hara, H.; Yatsu, Y.; Kawai, N. Bibcode: 2021ATel14334....1H Altcode: The flaring blazar BL Lacertae was in the bright state in optical, X-ray and gamma-ray around August 2020 (ATel #13930, #13933, #13956, #13958, #13963, #13964) and in another bright state around October 2020 (ATel #14065, #14069, #14072, #14081, #14096). Title: Sunrise Chromospheric Infrared spectroPolarimeter (SCIP) for SUNRISE III: optical design and performance Authors: Tsuzuki, Toshihiro; Katsukawa, Yukio; Uraguchi, Fumihiro; Hara, Hirohisa; Kubo, Masahito; Nodomi, Yoshifumi; Suematsu, Yoshinori; Kawabata, Yusuke; Shimizu, Toshifumi; Gandorfer, Achim; Feller, Alex; Grauf, Bianca; Solanki, Sami; Carlos del Toro Iniesta, Jose Bibcode: 2020SPIE11447E..AJT Altcode: The Sunrise Chromospheric Infrared spectroPolarimeter (SCIP) is a near-IR spectro-polarimeter instrument newly designed for Sunrise III, which is a balloon-borne solar observatory equipped with a 1 m optical telescope. To acquire high-quality 3D magnetic and velocity fields, SCIP selects the two wavelength bands centered at 850 nm and 770 nm, which contain many spectrum lines that are highly sensitive to magnetic fields permeating the photosphere and chromosphere. To achieve high spatial and spectral resolution (0.21 arcsec and 2 × 105), SCIP optics adopt a quasi-Littrow configuration based on an echelle grating and two high-order aspheric mirrors. Using different diffraction orders of the echelle grating, dichroic beam splitter, and polarizing beam-splitters, SCIP can obtain s- and p-polarization signals in the two wavelength bands simultaneously within a relatively small space. We established the wavefront error budget based on tolerance analysis, surface figure errors, alignment errors, and environmental changes. In addition, we performed stray light analysis, and designed light traps and baffles needed to suppress unwanted reflections and diffraction by the grating. In this paper, we present the details of this optical system and its performance. Title: GRB 201203A: MITSuME Okayama optical upper limits Authors: Niwano, M.; Hosokawa, R.; Murata, K. L.; Adachi, R.; Ogawa, F.; Nakamura, N.; Ito, N.; Ogata, S.; Takamatsu, H.; Hara, H.; Yatsu, Y.; Kawai, N.; MITSuME Collaboration Bibcode: 2020GCN.28992....1N Altcode: We observed the field of GRB 201203A (S. Dichiara et al., GCN Circular #28985) with the optical three color (g', Rc, and Ic) CCD cameras attached to the MITSuME 50 cm telescope of Okayama Astrophysical Observatory, Okayama, Japan. The observation started at 12:02:06 UT. We did not find any new point sources within the Swift-XRT circle ( V. D'Elia et al., GCN Circular #28990) in all three bands. We obtained the 5-sigma limits as follows. T0+[hour] MID-UT T-EXP[sec] 5-sigma limits ------------------------------------------------------------------------------------------------ 6.9 13:45:28.19 9000 g'>17.9, Rc>18.6, Ic>17.7 ------------------------------------------------------------------------------------------------ T0+ : Elapsed time after the burst T-EXP: Total Exposure time We used the PS1 catalog for flux calibration. The magnitudes are expressed in the AB system. The images were processed in real-time through the MITSuME GPU reduction pipeline (Niwano et al., 10.1093/pasj/psaa091, arXiv:2008.11486; https://github.com/MNiwano/Eclaire). Title: Sunrise Chromospheric Infrared spectroPolarimeter (SCIP) for SUNRISE III: opto-mechanical analysis and design Authors: Uraguchi, Fumihiro; Tsuzuki, Toshihiro; Katsukawa, Yukio; Hara, Hirohisa; Iwamura, Satoru; Kubo, Masahito; Nodomi, Yoshifumi; Suematsu, Yoshinori; Kawabata, Yusuke; Shimizu, Toshifumi; Gandorfer, Achim; del Toro Iniesta, Jose Carlos Bibcode: 2020SPIE11447E..ABU Altcode: The Sunrise Chromospheric Infrared spectroPolarimeter (SCIP) is a near-IR spectro-polarimeter instrument newly designed for Sunrise III, a balloon-borne solar observatory with a 1-m diameter telescope. In order to achieve the strict requirements the SCIP wavefront error, it is necessary to quantify the errors due to environmen- tal effects such as gravity and temperature variation under the observation conditions. We therefore conducted an integrated opto-mechanical analysis incorporating mechanical and thermal disturbances into a finite element model of the entire SCIP structure to acquire the nodal displacements of each optical element, then fed them back to the optical analysis software in the form of rigid body motion and surface deformation fitted by polynomials. This method allowed us to determine the error factors having a significant influence on optical performance. For example, no significant wavefront degradation was associated with the structural mountings because the optical element mounts were well designed based on quasi-kinematic constraints. In contrast, we found that the main factor affecting wavefront degradation was the rigid body motions of the optical elements, which must be mini- mized within the allowable level. Based on these results, we constructed the optical bench using a sandwich panel as the optical bench consisting of an aluminum-honeycomb core and carbon fiber reinforced plastic skins with a high stiffness and low coefficient of thermal expansion. We then confirmed that the new opto-mechanical model achieved the wavefront error requirement. In this paper, we report the details of this integrated opto-mechanical analysis, including the wavefront error budgeting and the design of the opto-mechanics. Title: GRB 201223A: MITSuME Akeno optical observation Authors: Hosokawa, R.; Murata, K. L.; Adachi, R.; Niwano, M.; Ogawa, F.; Nakamura, N.; Ito, N.; Ogata, S.; Takamatsu, H.; Hara, H.; Yatsu, Y.; Kawai, N.; MITSuME Collaboration Bibcode: 2020GCN.29164....1H Altcode: We observed the field of GRB 201223A (J.D. Gropp et al., GCN #29158, J. Wood et al., GCN #29161) with the optical three color (g', Rc, and Ic) CCD cameras attached to the MITSuME 50 cm telescope of Akeno Observatory, Yamanashi, Japan. The observation started at 2020-12-23 17:59:18 UT (52s after Swift BAT trigger). We detected the point source at the position consistent with the afterglow detected previously (Lipunov et al. GCN #29157, Gropp et al., GCN #29158, Z.P. Zhu et al. GCN #29159, Y.-D. Hu et al. GCN #29160). We measured the magnitudes as follows. T0+[sec] MID-UT T-EXP[sec] measured magnitudes ------------------------------------------------------------------------------------------------ 52 17:59:48 60 g'=15.45+/-0.05, Rc=15.04+/-0.03, Ic=14.77+/-0.04 ------------------------------------------------------------------------------------------------ T0+ : Elapsed time after the burst T-EXP: Total Exposure time We used PS1 catalog for flux calibration. The magnitudes are expressed in the AB system. The images were processed in real-time through the MITSuME GPU reduction pipeline (Niwano et al., https://doi.org/10.1093/pasj/psaa091, https://arxiv.org/abs/2008.11486; https://github.com/MNiwano/Eclaire). Title: The Solar-C (EUVST) mission: the latest status Authors: Shimizu, Toshifumi; Imada, Shinsuke; Kawate, Tomoko; Suematsu, Yoshinori; Hara, Hirohisa; Tsuzuki, Toshihiro; Katsukawa, Yukio; Kubo, Masahito; Ishikawa, Ryoko; Watanabe, Tetsuya; Toriumi, Shin; Ichimoto, Kiyoshi; Nagata, Shin'ichi; Hasegawa, Takahiro; Yokoyama, Takaaki; Watanabe, Kyoko; Tsuno, Katsuhiko; Korendyke, Clarence M.; Warren, Harry; De Pontieu, Bart; Boerner, Paul; Solanki, Sami K.; Teriaca, Luca; Schuehle, Udo; Matthews, Sarah; Long, David; Thomas, William; Hancock, Barry; Reid, Hamish; Fludra, Andrzej; Auchère, Frederic; Andretta, Vincenzo; Naletto, Giampiero; Poletto, Luca; Harra, Louise Bibcode: 2020SPIE11444E..0NS Altcode: Solar-C (EUVST) is the next Japanese solar physics mission to be developed with significant contributions from US and European countries. The mission carries an EUV imaging spectrometer with slit-jaw imaging system called EUVST (EUV High-Throughput Spectroscopic Telescope) as the mission payload, to take a fundamental step towards answering how the plasma universe is created and evolves and how the Sun influences the Earth and other planets in our solar system. In April 2020, ISAS (Institute of Space and Astronautical Science) of JAXA (Japan Aerospace Exploration Agency) has made the final down-selection for this mission as the 4th in the series of competitively chosen M-class mission to be launched with an Epsilon launch vehicle in mid 2020s. NASA (National Aeronautics and Space Administration) has selected this mission concept for Phase A concept study in September 2019 and is in the process leading to final selection. For European countries, the team has (or is in the process of confirming) confirmed endorsement for hardware contributions to the EUVST from the national agencies. A recent update to the mission instrumentation is to add a UV spectral irradiance monitor capability for EUVST calibration and scientific purpose. This presentation provides the latest status of the mission with an overall description of the mission concept emphasizing on key roles of the mission in heliophysics research from mid 2020s. Title: Sunrise Chromospheric Infrared SpectroPolarimeter (SCIP) for sunrise III: system design and capability Authors: Katsukawa, Y.; del Toro Iniesta, J. C.; Solanki, S. K.; Kubo, M.; Hara, H.; Shimizu, T.; Oba, T.; Kawabata, Y.; Tsuzuki, T.; Uraguchi, F.; Nodomi, Y.; Shinoda, K.; Tamura, T.; Suematsu, Y.; Ishikawa, R.; Kano, R.; Matsumoto, T.; Ichimoto, K.; Nagata, S.; Quintero Noda, C.; Anan, T.; Orozco Suárez, D.; Balaguer Jiménez, M.; López Jiménez, A. C.; Cobos Carrascosa, J. P.; Feller, A.; Riethmueller, T.; Gandorfer, A.; Lagg, A. Bibcode: 2020SPIE11447E..0YK Altcode: The Sunrise balloon-borne solar observatory carries a 1 m aperture optical telescope and provides us a unique platform to conduct continuous seeing-free observations at UV-visible-IR wavelengths from an altitude of higher than 35 km. For the next flight planned for 2022, the post-focus instrumentation is upgraded with new spectro- polarimeters for the near UV (SUSI) and the near-IR (SCIP), whereas the imaging spectro-polarimeter Tunable Magnetograph (TuMag) is capable of observing multiple spectral lines within the visible wavelength. A new spectro-polarimeter called the Sunrise Chromospheric Infrared spectroPolarimeter (SCIP) is under development for observing near-IR wavelength ranges of around 770 nm and 850 nm. These wavelength ranges contain many spectral lines sensitive to solar magnetic fields and SCIP will be able to obtain magnetic and velocity structures in the solar atmosphere with a sufficient height resolution by combining spectro-polarimetric data of these lines. Polarimetric measurements are conducted using a rotating waveplate as a modulator and polarizing beam splitters in front of the cameras. The spatial and spectral resolutions are 0.2" and 2 105, respectively, and a polarimetric sensitivity of 0.03 % (1σ) is achieved within a 10 s integration time. To detect minute polarization signals with good precision, we carefully designed the opto-mechanical system, polarization optics and modulation, and onboard data processing. Title: Current Status of the Solar-C_EUVST Mission Authors: Imada, S.; Shimizu, T.; Kawate, T.; Toriumi, S.; Katsukawa, Y.; Kubo, M.; Hara, H.; Suematsu, Y.; Ichimoto, K.; Watanabe, T.; Watanabe, K.; Yokoyama, T.; Warren, H.; Long, D.; Harra, L. K.; Teriaca, L. Bibcode: 2020AGUFMSH056..05I Altcode: Solar-C_EUVST (EUV High-Throughput Spectroscopic Telescope) is designed to comprehensively understand the energy and mass transfer from the solar surface to the solar corona and interplanetary space, and to investigate the elementary processes that take place universally in cosmic plasmas. As a fundamental step towards answering how the plasma universe is created and evolves, and how the Sun influences the Earth and other planets in our solar system, the proposed mission is designed to comprehensively understand how mass and energy are transferred throughout the solar atmosphere. Understanding the solar atmosphere, which connects to the heliosphere via radiation, the solar wind and coronal mass ejections, and energetic particles is pivotal for establishing the conditions for life and habitability in the solar system.
The two primary science objectives for Solar-C_EUVST are : I) Understand how fundamental processes lead to the formation of the solar atmosphere and the solar wind, II) Understand how the solar atmosphere becomes unstable, releasing the energy that drives solar flares and eruptions. Solar-C_EUVST will, A) seamlessly observe all the temperature regimes of the solar atmosphere from the chromosphere to the corona at the same time, B) resolve elemental structures of the solar atmosphere with high spatial resolution and cadence to track their evolution, and C) obtain spectroscopic information on the dynamics of elementary processes taking place in the solar atmosphere. In this talk, we will first discuss the science target of the Solar-C_EUVST, and then discuss the current status of the Solar-C_EUVST mission. Title: GRB 201214B: MITSuME Akeno optical upper limits Authors: Nakamura, N.; Hosokawa, R.; Murata, K. L.; Adachi, R.; Niwano, M.; Ogawa, F.; Ito, N.; Ogata, S.; Takamatsu, H.; Hara, H.; Yatsu, Y.; Kawai, N.; MITSuME Collaboration Bibcode: 2020GCN.29056....1N Altcode: We observed the field of GRB 201214B (The Fermi GBM team, GCN #29039, P. Evans et al., GCN #29043, V. Lipunov et al., GCN #29044, D. Palmer et al., GCN #29045, B. Sbarufatti et al., GCN #29052 ) with the optical three color (g', Rc, and Ic) CCD cameras attached to the MITSuME 50 cm telescope of Akeno Observatory, Yamanashi, Japan. The observation with a series of 60 sec exposures started at 2020-12-15 18:51:41 UT(28.8 hour after trigger). We did not find any new point sources within the enhanced Swift BAT circle (D. Palmer et al., GCN #29045) in all three bands. We obtained the 5-sigma limits of the stacked images as follows T0+[hour] MID-UT T-EXP[sec] 5-sigma limits ------------------------------------------------------------------------------------------------ 28.8 18:51:41 10380 g'>20.9, Rc>21.0, Ic>20.3 ------------------------------------------------------------------------------------------------ T0+ : Elapsed time after the burst T-EXP: Total Exposure time We used the PS1 catalog for flux calibration. The magnitudes are expressed in the AB system. The images were processed in real-time through the MITSuME GPU reduction pipeline (Niwano et al., https://doi.org/10.1093/pasj/psaa091, https://arxiv.org/abs/2008.11486; https://github.com/MNiwano/Eclaire). Title: Thermal design of the Solar-C (EUVST) telescope Authors: Suematsu, Yoshinori; Shimizu, Toshifumi; Hara, Hirohisa; Kawate, Tomoko; Katsukawa, Yukio; Ichimoto, Kiyoshi; Imada, Shinsuke; Nagae, Kazuhiro; Yamazaki, Atsumu; Hattori, Tomoya Bibcode: 2020SPIE11444E..3KS Altcode: The EUV High-Throughput Spectroscopic Telescope (EUVST) of Solar-C mission consists of only two imaging optical components; a 28-cm clear aperture off-axis parabolic primary mirror and a two-split ellipsoidal grating without a blocking filter for visible light before the primary mirror to achieve unprecedented high spatial and temporal resolution in EUV-UV imaging spectroscopic observations. For this reason, about 60 W of sunlight is absorbed by the multilayer coating on the mirror. We report a thermal design of telescope in which the temperature of the primary mirror bonding part and underlying tip-tilt and slit-scanning mechanisms is well lower than a glass transition temperature of adhesive (about 60°C) and thermal deformation of the primary mirror is small, although it is non-negligibly small. Title: A sensitivity analysis of the updated optical design for EUVST on the Solar-C mission Authors: Kawate, Tomoko; Tsuzuki, Toshihiro; Shimizu, Toshifumi; Imada, Shinsuke; Katsukawa, Yukio; Hara, Hirohisa; Suematsu, Yoshinori; Ichimoto, Kiyoshi; Hattori, Tomoya; Narasaki, Shota; Warren, Harry P.; Teriaca, Luca; Korendyke, Clarence M.; Brown, Charles M.; Auchere, Frederic Bibcode: 2020SPIE11444E..3JK Altcode: The EUV high-throughput spectroscopic telescope (EUVST) onboard the Solar-C mission has the high spatial (0.4'') resolution over a wide wavelength range in the vacuum ultraviolet. To achieve high spatial resolution under a design constraint given by the JAXA Epsilon launch vehicle, we further update the optical design to secure margins needed to realize 0.4'' spatial resolution over a field of view of 100''×100''. To estimate the error budgets of spatial and spectral resolutions due to installation and fabrication errors, we perform a sensitivity analysis for the position and orientation of each optical element and for the grating parameters by ray tracing with the Zemax software. We obtain point spread functions (PSF) for rays from 9 fields and at 9 wavelengths on each detector by changing each parameter slightly. A full width at half maximum (FWHM) of the PSF is derived at each field and wavelength position as a function of the perturbation of each optical parameter. Assuming a mount system of each optical element and an error of each optical parameter, we estimate spatial and spectral resolutions by taking installation and fabrication errors into account. The results of the sensitivity analysis suggest that budgets of the total of optical design and the assembly errors account for 15% and 5.8% of our budgets of the spatial resolution in the long wavelength and short wavelength bands, respectively. On the other hand, the grating fabrication errors give a large degradation of spatial and spectral resolutions, and investigations of compensators are needed to relax the fabrication tolerance of the grating surface parameters. Title: GRB 201104B: MITSuME Akeno optical observation Authors: Hosokawa, R.; Adachi, R.; Murata, K. L.; Niwano, M.; Ogawa, F.; Nakamura, N.; Ito, N.; Ogata, S.; Takamatsu, H.; Hara, H.; Yatsu, Y.; Kawai, N.; MITSuME Collaboration Bibcode: 2020GCN.28870....1H Altcode: We observed the field of GRB 201104B (B. Sbarufatti et al., GCN #28825) with the optical three color (g', Rc, and Ic) CCD cameras attached to the MITSuME 50 cm telescope of Akeno Observatory, Yamanashi, Japan. The observation with a series of 60 sec exposures started at 2020-11-05 08:14:33 UT. The first 29 images were heavily affected by twilight at Akeno Observatory. We marginally detected the point source at the position consistent with the afterglow detected previously (Marshall et al., GCN #28827, Vielfaure et al., GCN #28840, Oates et al., GCN #28851, Belkin et al., GCN #28852, Belkin et al., GCN #28856, and Gupta et al., GCN #28860). We measured the magnitudes as follows. T0+[hour] MID-UT T-EXP[sec] measured magnitudes ------------------------------------------------------------------------------------------------ 15.2 2020-11-05 12:59:59 21360 g'=21.5+/-0.3, Rc=20.7+/-0.2, Ic=20.3+/-0.3 ------------------------------------------------------------------------------------------------ T0+ : Elapsed time after the burst T-EXP: Total Exposure time We used the PS1 catalog for flux calibration. The magnitudes are expressed in the AB system. The images were processed in real-time through the MITSuME GPU reduction pipeline (Niwano et al., https://doi.org/10.1093/pasj/psaa091, https://arxiv.org/abs/2008.11486; https://github.com/MNiwano/Eclaire). Title: GRB 201017A: MITSuME Akeno optical upper limits Authors: Hosokawa, R.; Murata, K. L.; Adachi, R.; Niwano, M.; Ogawa, F.; Nakamura, N.; Ito, N.; Ogata, S.; Takamatsu, H.; Hara, H.; Yatsu, Y.; Kawai, N.; MITSuME Collaboration Bibcode: 2020GCN.28684....1H Altcode: We observed the field of GRB 201017A (The Fermi GBM team, GCN #28665, A. D'Ai et al., GCN #28666, V. Lipunov et al., GCN #28667, L. P. Xin et al., GCN #28672, S. Belkin et al., GCN #28679) with the optical three color (g', Rc, and Ic) CCD cameras attached to the MITSuME 50 cm telescope of Akeno Observatory, Yamanashi, Japan. The observation started at 2020-10-17 12:53:15 UT.(186 min after trigger) Since some images were heavily affected by bad weather, we stacked the images with good conditions. We did not find any new point sources within the enhanced Swift/XRT circle (M. R. Goad et al., GCN #28671) in all three bands. We obtained the 5-sigma limits as follows T0+[min] MID-UT T-EXP[sec] 5-sigma limits ------------------------------------------------------------------------------------------------ 296 17:53:37 9480 g'>20.0,Rc>19.9,Ic>19.2 ------------------------------------------------------------------------------------------------ T0+ : Elapsed time after the burst T-EXP: Total Exposure time We used the PS1 catalog for flux calibration. The magnitudes are expressed in the AB system. The images were processed in real-time through the MITSuME GPU reduction pipeline (Niwano et al., accepted for publication in PASJ, https://arxiv.org/abs/2008.11486; https://github.com/MNiwano/Eclaire). Title: GRB 201020A: MITSuME Akeno optical observation Authors: Adachi, R.; Hosokawa, R.; Murata, K. L.; Niwano, M.; Ogawa, F.; Nakamura, N.; Ito, N.; Ogata, S.; Takamatsu, H.; Hara, H.; Yatsu, Y.; Kawai, N.; MITSuME Collaboration Bibcode: 2020GCN.28697....1A Altcode: We observed the field of GRB 201020A (E. Ambrosi et al.,GCN Circular #28696) with the optical three color (g', Rc, and Ic) CCD cameras attached to the MITSuME 50 cm telescope of Akeno Observatory, Yamanashi, Japan. The observation started at 2020-10-20 08:31:00 UT. The first 28 images were heavily affected by twilight at Akeno Observatory. We detected the point source at the position consistent with the afterglow detected previously (E. Ambrosi et al. GCN #28696). We measured the magnitudes as follows. T0+[min] MID-UT T-EXP[sec] measured magnitudes ------------------------------------------------------------------------------------------------ 196 09:15:39 1260 g'=19.4+/-0.2, Rc=18.4+/-0.1, Ic=18.4+/-0.2 ------------------------------------------------------------------------------------------------ T0+ : Elapsed time after the burst T-EXP: Total Exposure time We used GSC2.3 and PS1 catalog for flux calibration. The magnitudes are expressed in the AB system. The images were processed in real-time through the MITSuME GPU reduction pipeline (Niwano et al., accepted for publication in PASJ, https://arxiv.org/abs/2008.11486; https://github.com/MNiwano/Eclaire). Title: GRB 201024A: MITSuME Akeno optical upper limits Authors: Niwano, M.; Murata, K. L.; Hosokawa, R.; Adachi, R.; Ogawa, F.; Nakamura, N.; Ito, N.; Ogata, S.; Takamatsu, H.; Hara, H.; Yatsu, Y.; Kawai, N.; MITSuME Collaboration Bibcode: 2020GCN.28779....1N Altcode: We observed the field of GRB 201024A (F. E. Marshall et al.,GCN Circular #28761) with the optical three color (g', Rc, and Ic) CCD cameras attached to the MITSuME 50 cm telescope of Akeno Observatory, Yamanashi, Japan. We observed for two nights. The observation with a series of 60 sec exposures started at 2020-10-24 16:04:04UT for the first night and 2020-10-25 15:56:17UT for the second night. We stacked the images with good conditions each night. We did not detect the point source reported by other telescopes (Lipunov et al. GCN Circular #28760, Fernandez-Garcia et al. #28763, de Ugarte Postigo et al. #28764, Martin Jelinek et al. #28766). We obtained the 5-sigma limits of the stacked images as follows. T0+[hour] MID-UT T-EXP[sec] 5-sigma limits ------------------------------------------------------------------------------------------------ 13.78 2020-10-24T18:27:11 11520 g'>20.2, Rc>20.4, Ic>19.7 38.48 2020-10-25T17:17:59 1980 g'>19.4, Rc>19.6, Ic>18.8 ------------------------------------------------------------------------------------------------ T0+: Elapsed time after the burst T-EXP: Total Exposure time We used the PS1 catalog for flux calibration. The magnitudes are expressed in the AB system. The images were processed in real-time through the MITSuME GPU reduction pipeline (Niwano et al., accepted for publication in PASJ, https://arxiv.org/abs/2008.11486; https://github.com/MNiwano/Eclaire). Title: GRB 201027A: MITSuME Akeno optical upper limits Authors: Hosokawa, R.; Hara, H.; Adachi, R.; Niwano, M.; Ogawa, F.; Murata, K. L.; Nakamura, N.; Ito, N.; Ogata, S.; Takamatsu, H.; Yatsu, Y.; Kawai, N.; MITSuME Collaboration Bibcode: 2020GCN.28802....1H Altcode: We observed the field of GRB 201027A (V. Lipunov et al., GCN #28787, S. B. Cenko et al., GCN #28788, Y.-D. Hu et al., GCN #28794 ) with the optical three color (g', Rc, and Ic) CCD cameras attached to the MITSuME 50 cm telescope of Akeno Observatory, Yamanashi, Japan. The observation with a series of 60 sec exposures started at 2020-10-27 18:43:12 UT(17.2 hour after trigger). Since the first 18 images were taken under high airmass conditions, we stacked the images with good conditions. We did not find any new point sources within the enhanced Swift/XRT circle (J.P. Osborne et al., GCN #28792) in all three bands. We obtained the 5-sigma limits of the stacked images as follows. T0+[hour] MID-UT T-EXP[sec] 5-sigma limits ------------------------------------------------------------------------------------------------ 17.6 19:19:32 3180 g'>19.5,Rc>20.0,Ic>19.1 ------------------------------------------------------------------------------------------------ T0+ : Elapsed time after the burst T-EXP: Total Exposure time We used the PS1 catalog for flux calibration. The magnitudes are expressed in the AB system. The images were processed in real-time through the MITSuME GPU reduction pipeline (Niwano et al., https://doi.org/10.1093/pasj/psaa091, https://arxiv.org/abs/2008.11486; https://github.com/MNiwano/Eclaire). Title: GRB 201001A: MITSuME Akeno optical upper limits Authors: Hosokawa, R.; Ogata, S.; Murata, K. L.; Adachi, R.; Niwano, M.; Ogawa, F.; Nakamura, N.; Ito, N.; Takamatsu, H.; Hara, H.; Yatsu, Y.; Kawai, N.; MITSuME Collaboration Bibcode: 2020GCN.28548....1H Altcode: We observed the field of GRB 201001A(Fermi GBM Team, GCN 28538; David et al., GCN 28539) with the optical three color (g', Rc, and Ic) CCD cameras attached to the MITSuME 50 cm telescope of Akeno Observatory, Yamanashi, Japan. The observation with a series of 60 sec exposures started at 2020-10-01 16:44:38UT. Since some images were heavily affected by the moon, we stacked the images with good conditions. We did not find any new point sources within the enhanced Swift/XRT error circle (Evans et al., GCN 28540) in the 60 sec exposure images and the stacked images. We obtained the 5-sigma limits of the stacked images as follows. T0+[hour] MID-UT T-EXP[sec] 5-sigma limits ------------------------------------------------------------------------------------------------ 6.8 2020-10-01T19:06:10.46 4020 g'>19.0, Rc>19.3, Ic>18.9 ------------------------------------------------------------------------------------------------ T0+: Elapsed time after the burst T-EXP: Total Exposure time We used the PS1 catalog for flux calibration. The magnitudes are expressed in the AB system. The images were processed in real-time through the MITSuME GPU reduction pipeline (Niwano et al., accepted for publication in PASJ, https://arxiv.org/abs/2008.11486; https://github.com/MNiwano/Eclaire). -- ____________ 東京工業大学 河合研究室 修士1年 細川稜平 hosokawa@hp.phys.titech.ac.jp Title: GRB 201006A: MITSuME Akeno optical upper limits Authors: Ito, N.; Hosokawa, R.; Murata, K. L.; Adachi, R.; Niwano, M.; Ogawa, F.; Nakamura, N.; Ogata, S.; Takamatsu, H.; Hara, H.; Yatsu, Y.; Kawai, N.; MITSuME Collaboration Bibcode: 2020GCN.28571....1I Altcode: We observed the field of GRB 201006A (J.D. Gropp et al.,GCN #28560, S.Mereghetti et al., GCN #28561, R. Hamburg et al., GCN # 28564) with the optical three color (g', Rc, and Ic) CCD cameras attached to the MITSuME 50 cm telescope of Akeno Observatory, Yamanashi, Japan. The observation started at 13:31:53 UT. Since some images were heavily affected by bad weather and the moon, we stacked the images with good conditions. We did not find any new point sources within the enhanced Swift/XRT circle (M.R. Goad et al., GCN #28562) in all three bands. We obtained the 5-sigma limits as follows. T0+[hour] MID-UT T-EXP[sec] 5-sigma limits ------------------------------------------------------------------------------------------------ 12.2 16:27:01 4020.0 g'>19.5,Rc>19.4,Ic>18.9 ------------------------------------------------------------------------------------------------ T0+ : Elapsed time after the burst T-EXP: Total Exposure time We used PS1 catalog for flux calibration. The magnitudes are expressed in the AB system. The images were processed in real-time through the MITSuME GPU reduction pipeline (Niwano et al., accepted for publication in PASJ; arXiv2008.11486 https://github.com/MNiwano/Eclaire) Title: GRB 200907B: MITSuME Okayama optical upper limits Authors: Hosokawa, R.; Murata, K. L.; Adachi, R.; Niwano, M.; Ogawa, F.; Nakamura, N.; Ito, N.; Ogata, S.; Takamatsu, H.; Hara, H.; Yatsu, Y.; Kawai, N.; MITSuME Collaboration Bibcode: 2020GCN.28393....1H Altcode: We observed the field of GRB 200907B (Beardmore et al., GCN 28384; Evans et al., GCN 28385,28391) with the optical three color (g', Rc, and Ic) CCD cameras attached to the MITSuME 50 cm telescope of Okayama Astrophysical Observatory, Okayama, Japan. The observation with a series of 60 sec exposures started at 2020-09-07 18:52:16UT. We did not find any new point sources within the enhanced Swift/XRT error circle (Evans et al., GCN 28391) in the 60 sec exposure images and the stacked images. We obtained the 5-sigma limits of the stacked images as follows. T0+[sec] MID-UT T-EXP[sec] 5-sigma limits ------------------------------------------------------------------------------------------------ 65 2020-09-07T19:19:48 2100 g'>17.1, Rc>17.9, Ic>17.3 ------------------------------------------------------------------------------------------------ T0+: Elapsed time after the burst T-EXP: Total Exposure time We used the PS1 catalog for flux calibration. The magnitudes are expressed in the AB system. The images were processed in real-time through the MITSuME GPU reduction pipeline (Niwano et al., accepted for publication in PASJ, https://arxiv.org/abs/2008.11486; https://github.com/MNiwano/Eclaire). Title: GRB 200819A: MITSuME Akeno optical upper limits Authors: Murata, K. L.; Hosokawa, R.; Adachi, R.; Niwano, M.; Ogawa, F.; Nakamura, N.; Ito, N.; Ogata, S.; Takamatsu, H.; Hara, H.; Yatsu, Y.; Kawai, N.; Horiuchi, Takashi; Hanayama, Hidekazu; MITSuME Collaboration Bibcode: 2020GCN.28269....1M Altcode: We observed the field of GRB 200819A (Dichiara et al., GCN 28263; Evans et al., GCN 28265) with the optical three color (g', Rc, and Ic) CCD cameras attached to the MITSuME 50 cm telescope of Akeno Observatory, Yamanashi, Japan. The observation with a series of 60 sec exposures started on 2020-08-19 15:45:44 UT. Some images were heavily affected by bad weather conditions. We stacked the images with good weather conditions. We did not find any new point sources within the enhanced Swift/XRT error circle (Evans et al., GCN 28265) of the stacked images. We obtained the 5-sigma limits as follows. T0+[sec] MID-UT T-EXP[sec] 5-sigma limits ------------------------------------------------------------------------------------------------ ~290 2020-08-19T17:36:48 5640 g'>18.4, Rc>19.0, Ic>19.3 ------------------------------------------------------------------------------------------------ T0+: Elapsed time after the burst T-EXP: Total Exposure time We used the PS1 catalog for flux calibration. The magnitudes are expressed in the AB system. The images were processed in real-time through the MITSuME GPU reduction pipeline (Niwano et al., submitted; https://github.com/MNiwano/Eclaire) Title: GRB 200806A: MITSuME Akeno optical upper limits Authors: Murata, K. L.; Adachi, R.; Hosokawa, R.; Niwano, M.; Ogawa, F.; Nakamura, N.; Ito, N.; Ogata, S.; Takamatsu, H.; Hara, H.; Yatsu, Y.; Kawai, N.; MITSuME Collaboration Bibcode: 2020GCN.28215....1M Altcode: We observed the field of GRB 200806A (Ambrosi et al., GCN 28211; Beardmore et al., GCN 28214) with the optical three color (g', Rc, and Ic) CCD cameras attached to the MITSuME 50 cm telescope of Akeno Observatory, Yamanashi, Japan. The observation with a series of 60 sec exposures started on 2020-08-06 15:30:34 UT. The first 15 images were heavily affected by the presence of the moon. We stacked the images excluding the 15 images and did not find any new point sources within the enhanced Swift/XRT error circle (Beardmore et al., GCN 28214) of the stacked images. We obtained the 5-sigma limits as follows. T0+[min] MID-UT T-EXP[sec] 5-sigma limits ------------------------------------------------------------------------------------------------ 19 2020-08-06T15:57:10 960 g'>16.7, Rc>16.7, Ic>16.9 ------------------------------------------------------------------------------------------------ T0+: Elapsed time after the burst T-EXP: Total Exposure time We used the PS1 catalog for flux calibration. The magnitudes are expressed in the AB system. The images were processed in real-time through the MITSuME GPU reduction pipeline (Niwano et al., submitted; https://github.com/MNiwano/Eclaire) Title: Resonant electron impact excitation of highly charged Fe ions studied with a compact electron beam ion trap Authors: Monobe, Masashi; Sakaue, Hiroyuki A.; Kato, Daiji; Murakami, Izumi; Hara, Hirohisa; Watanabe, Tetsuya; Nakamura, Nobuyuki Bibcode: 2020XRS....49..511M Altcode: No abstract at ADS Title: GRB 200613A: MITSuME Akeno optical upper limits Authors: Murata, K. L.; Ito, N.; Hosokawa, R.; Adachi, R.; Niwano, M.; Ogawa, F.; Nakamura, N.; Ogata, S.; Takamatsu, H.; Hara, H.; Yatsu, Y.; Kawai, N.; MITSuME Collaboration Bibcode: 2020GCN.27962....1M Altcode: We observed the field of GRB 200613A (Fermi GBM team, GCN 27926; Bissaldi et al., GCN 27930; Ohno et al., GCN 27931) with the optical three color (g', Rc, and Ic) CCD cameras attached to the MITSuME 50 cm telescope of Akeno Observatory, Yamanashi, Japan. The observation started on 2020-06-15 11:33. We did not detect the optical afterglow (Kann et al., GCN 27935; Kennea et al., GCN 27936; Pozanenko et al., GCN 27937; Izzo et al., GCN 27939; Zhu et al., GCN 27943; Marshall et al., GCN 27944; Liu et al., GCN 27949; Belkin et al., GCN 27958) in the stacked image. We obtained the 5-sigma limits as follows. T0+[hour] MID-UT T-EXP[sec] 5-sigma limits ------------------------------------------------------------------------------------------------ 54 2020-06-15T12:29:27 2040 g'>19.3, Rc>19.5, Ic>18.6 ------------------------------------------------------------------------------------------------ T0+: Elapsed time after the burst T-EXP: Total Exposure time We used the PS1 catalog for flux calibration. The magnitudes are expressed in the AB system. The images were processed in real-time through the MITSuME GPU reduction pipeline (Niwano et al., submitted; https://github.com/MNiwano/Eclair) Title: A Solar Magnetic-fan Flaring Arch Heated by Nonthermal Particles and Hot Plasma from an X-Ray Jet Eruption Authors: Lee, Kyoung-Sun; Hara, Hirohisa; Watanabe, Kyoko; Joshi, Anand D.; Brooks, David H.; Imada, Shinsuke; Prasad, Avijeet; Dang, Phillip; Shimizu, Toshifumi; Savage, Sabrina L.; Moore, Ronald; Panesar, Navdeep K.; Reep, Jeffrey W. Bibcode: 2020ApJ...895...42L Altcode: 2020arXiv200509875L We have investigated an M1.3 limb flare, which develops as a magnetic loop/arch that fans out from an X-ray jet. Using Hinode/EIS, we found that the temperature increases with height to a value of over 107 K at the loop top during the flare. The measured Doppler velocity (redshifts of 100-500 km s-1) and the nonthermal velocity (≥100 km s-1) from Fe XXIV also increase with loop height. The electron density increases from 0.3 × 109 cm-3 early in the flare rise to 1.3 × 109 cm-3 after the flare peak. The 3D structure of the loop derived with Solar TErrestrial RElations Observatory/EUV Imager indicates that the strong redshift in the loop-top region is due to upflowing plasma originating from the jet. Both hard X-ray and soft X-ray emission from the Reuven Ramaty High Energy Solar Spectroscopic Imager were only seen as footpoint brightenings during the impulsive phase of the flare, then, soft X-ray emission moved to the loop top in the decay phase. Based on the temperature and density measurements and theoretical cooling models, the temperature evolution of the flare arch is consistent with impulsive heating during the jet eruption followed by conductive cooling via evaporation and minor prolonged heating in the top of the fan loop. Investigating the magnetic field topology and squashing factor map from Solar Dynamics Observatory/HMI, we conclude that the observed magnetic-fan flaring arch is mostly heated from low atmospheric reconnection accompanying the jet ejection, instead of from reconnection above the arch as expected in the standard flare model. Title: Locating Hot Plasma in Small Flares using Spectroscopic Overlappogram Data from the Hinode EUV Imaging Spectrometer Authors: Harra, Louise; Matthews, Sarah; Long, David; Hasegawa, Takahiro; Lee, Kyoung-Sun; Reeves, Katharine K.; Shimizu, Toshifumi; Hara, Hirohisa; Woods, Magnus Bibcode: 2020SoPh..295...34H Altcode: 2020arXiv200302908H One of the key processes associated with the "standard" flare model is chromospheric evaporation, a process during which plasma heated to high temperatures by energy deposition at the flare footpoints is driven upwards into the corona. Despite several decades of study, a number of open questions remain, including the relationship between plasma produced during this process and observations of earlier "superhot" plasma. The Extreme ultraviolet Imaging Spectrometer (EIS) onboard Hinode has a wide slot, which is often used as a flare trigger in the He II emission-line band. Once the intensity passes a threshold level, the study will switch to one focussed on the flaring region. However, when the intensity is not high enough to reach the flare trigger threshold, these datasets are then available during the entire flare period and provide high-cadence spectroscopic observations over a large field of view. We make use of data from two such studies of a C4.7 flare and a C1.6 flare to probe the relationship between hot Fe XXIV plasma and plasmas observed by the Reuven Ramaty High Energy Solar Spectroscopic Imager (RHESSI) and the X-ray Telescope (XRT) to track where the emission comes from and when it begins. The flare trigger slot data used in our analysis has one-minute cadence. Although the spatial and spectral information are merged in the wide-slot data, it is still possible to extract when the hot plasma appears, through the appearance of the Fe Xxiv spectral image. It is also possible to derive spectrally pure Fe XXIV light curves from the EIS data, and compare them with those derived from hard X-rays, enabling a full exploration of the evolution of hot emission. The Fe XXIV emission peaks just after the peak in the hard X-ray lightcurve; consistent with an origin in the evaporation of heated plasma following the transfer of energy to the lower atmosphere. A peak was also found for the C4.7 flare in the RHESSI peak temperature, which occurred before the hard X-rays peaked. This suggests that the first peak in hot-plasma emission is likely to be directly related to the energy-release process. Title: Nonthermal Motions in a Polar Coronal Hole Measured with Hinode/EIS during an on-Orbit Partial Solar Eclipse on 2017 August 21 Authors: Hara, Hirohisa Bibcode: 2019ApJ...887..122H Altcode: We have performed a spectroscopic observation over the south polar coronal hole (PCH) with the Hinode Extreme-ultraviolet (EUV) Imaging Spectrometer (EIS) during an on-orbit partial solar eclipse. In this partial eclipse, the Moon passed through the EIS observing area that was set in the south PCH at the height of 0.9-1.4 solar radii. Using the lunar occultation, we have corrected for the scattered light contamination from bright regions of the Sun that is present in the dark PCH emission line profiles. The nonthermal width of the corrected emission line profile in the PCH increases from the limb toward the high-altitude corona. It has also been confirmed that the nonthermal width tends to decrease beyond ∼1.2 solar radii. These results are consistent with the model in which outward-propagating Alfvén waves start being dissipated at ∼1.2 solar radii, as previously reported. The reduced energy within ∼1.4 solar radii contributes to atmospheric heating and the initial acceleration for the solar wind in the low corona. The remaining energy flux at 1.4 solar radii may be dissipated in the distant corona and is sufficient to provide the additional acceleration required to drive the fast solar wind. Title: Achievements of Hinode in the first eleven years Authors: Hinode Review Team; Al-Janabi, Khalid; Antolin, Patrick; Baker, Deborah; Bellot Rubio, Luis R.; Bradley, Louisa; Brooks, David H.; Centeno, Rebecca; Culhane, J. Leonard; Del Zanna, Giulio; Doschek, George A.; Fletcher, Lyndsay; Hara, Hirohisa; Harra, Louise K.; Hillier, Andrew S.; Imada, Shinsuke; Klimchuk, James A.; Mariska, John T.; Pereira, Tiago M. D.; Reeves, Katharine K.; Sakao, Taro; Sakurai, Takashi; Shimizu, Toshifumi; Shimojo, Masumi; Shiota, Daikou; Solanki, Sami K.; Sterling, Alphonse C.; Su, Yingna; Suematsu, Yoshinori; Tarbell, Theodore D.; Tiwari, Sanjiv K.; Toriumi, Shin; Ugarte-Urra, Ignacio; Warren, Harry P.; Watanabe, Tetsuya; Young, Peter R. Bibcode: 2019PASJ...71R...1H Altcode: Hinode is Japan's third solar mission following Hinotori (1981-1982) and Yohkoh (1991-2001): it was launched on 2006 September 22 and is in operation currently. Hinode carries three instruments: the Solar Optical Telescope, the X-Ray Telescope, and the EUV Imaging Spectrometer. These instruments were built under international collaboration with the National Aeronautics and Space Administration and the UK Science and Technology Facilities Council, and its operation has been contributed to by the European Space Agency and the Norwegian Space Center. After describing the satellite operations and giving a performance evaluation of the three instruments, reviews are presented on major scientific discoveries by Hinode in the first eleven years (one solar cycle long) of its operation. This review article concludes with future prospects for solar physics research based on the achievements of Hinode. Title: Development of Solar-C_EUVST structural design Authors: Suematsu, Yoshinori; Shimizu, Toshifumi; Hara, Hirohisa; Katsukawa, Yukio; Kawate, Tomoko; Ichimoto, Kiyoshi; Imada, Shinsuke Bibcode: 2019SPIE11118E..1OS Altcode: The Solar-C_EUVST is a mission designed to provide high-quality solar spectroscopic data covering a wide temperature range of the chromosphere to flaring corona. To fulfill a high throughput requirement, the instrument consists of only two optical components; a 28-cm primary mirror and a segmented toroidal grating which have high reflective coatings in EUV-UV range. We present a mission payload structural design which accommodates long focal length optical components and a launcher condition/launch environment (JAXA Epsilon). We also present a mechanical design of primary mirror assembly which enables slit-scan observations, an image stabilizing tip-tilt control, and a focus adjustment on orbit, together with an optomechanical design of the primary mirror and its supporting system which gives optically tolerant wavefront error against a large temperature increase due to an absorption of visible and IR lights. Title: Concept study of Solar-C_EUVST optical design Authors: Kawate, Tomoko; Shimizu, Toshifumi; Imada, Shinsuke; Tsuzuki, Toshihiro; Katsukawa, Yukio; Hara, Hirohisa; Suematsu, Yoshinori; Ichimoto, Kiyoshi; Warren, Harry; Teriaca, Luca; Korendyke, Clarence M.; Brown, Charles Bibcode: 2019SPIE11118E..1NK Altcode: The main characteristics of Solar-C_EUVST are the high temporal and high spatial resolutions over a wide temperature coverage. In order to realize the instrument for meeting these scientific requirements under size constraints given by the JAXA Epsilon vehicle, we examined four-dimensional optical parameter space of possible solutions of geometrical optical parameters such as mirror diameter, focal length, grating magnification, and so on. As a result, we have identified the solution space that meets the EUVST science objectives and rocket envelope requirements. A single solution was selected and used to define the initial optical parameters for the concept study of the baseline architecture for defining the mission concept. For this solution, we optimized the grating and geometrical parameters by ray tracing of the Zemax software. Consequently, we found an optics system that fulfills the requirement for a 0.4" angular resolution over a field of view of 100" (including margins) covering spectral ranges of 170-215, 463-542, 557-637, 690-850, 925-1085, and 1115-1275 A. This design achieves an effective area 10 times larger than the Extreme-ultraviolet Imaging Spectrometer onboard the Hinode satellite, and will provide seamless observations of 4.2-7.2 log(K) plasmas for the first time. Tolerance analyses were performed based on the optical design, and the moving range and step resolution of focus mechanisms were identified. In the presentation, we describe the derivation of the solution space, optimization of the optical parameters, and show the results of ray tracing and tolerance analyses. Title: The Solar-C_EUVST mission Authors: Shimizu, Toshifumi; Imada, Shinsuke; Kawate, Tomoko; Ichimoto, Kiyoshi; Suematsu, Yoshinori; Hara, Hirohisa; Katsukawa, Yukio; Kubo, Masahito; Toriumi, Shin; Watanabe, Tetsuya; Yokoyama, Takaaki; Korendyke, Clarence M.; Warren, Harry P.; Tarbell, Ted; De Pontieu, Bart; Teriaca, Luca; Schühle, Udo H.; Solanki, Sami; Harra, Louise K.; Matthews, Sarah; Fludra, A.; Auchère, F.; Andretta, V.; Naletto, G.; Zhukov, A. Bibcode: 2019SPIE11118E..07S Altcode: Solar-C EUVST (EUV High-Throughput Spectroscopic Telescope) is a solar physics mission concept that was selected as a candidate for JAXA competitive M-class missions in July 2018. The onboard science instrument, EUVST, is an EUV spectrometer with slit-jaw imaging system that will simultaneously observe the solar atmosphere from the photosphere/chromosphere up to the corona with seamless temperature coverage, high spatial resolution, and high throughput for the first time. The mission is designed to provide a conclusive answer to the most fundamental questions in solar physics: how fundamental processes lead to the formation of the solar atmosphere and the solar wind, and how the solar atmosphere becomes unstable, releasing the energy that drives solar flares and eruptions. The entire instrument structure and the primary mirror assembly with scanning and tip-tilt fine pointing capability for the EUVST are being developed in Japan, with spectrograph and slit-jaw imaging hardware and science contributions from US and European countries. The mission will be launched and installed in a sun-synchronous polar orbit by a JAXA Epsilon vehicle in 2025. ISAS/JAXA coordinates the conceptual study activities during the current mission definition phase in collaboration with NAOJ and other universities. The team is currently working towards the JAXA final down-selection expected at the end of 2019, with strong support from US and European colleagues. The paper provides an overall description of the mission concept, key technologies, and the latest status. Title: Design of all-reflective space-borne 1-m aperture solar optical telescope Authors: Suematsu, Y.; Hara, H.; Katsukawa, Y.; Kano, R.; Shimizu, T.; Ichimoto, K. Bibcode: 2019SPIE11180E..0RS Altcode: A 1-m aperture optical telescope is planned for a future Japanese solar mission. The telescope is designed to provide high spatial resolution data of solar lower atmosphere from the photosphere to the uppermost chromosphere with enhanced spectroscopic and spectro-polarimetric capabilities covering a wide wavelength region from UV to near IR where many useful spectral lines and continua exist for physical diagnosis of the solar magnetized atmosphere. We designed an allreflective telescope to fulfill the scientific and engineering requirements. From a thermal view point, a Gregorian telescope is the most suitable. To avoid chromatic aberration, a tri-aspheric-mirror collimator coupling to the Gregorian was designed to give a diffraction-limited performance over the FOV by allowing a field curvature. The field curvature can be compensated by an off-axis Ritchey Chretien reimaging optics at an entrance of focal plane instrument, which has an opposite sign in the field curvature to the Gregorian. We also briefly studied structural design of all-reflective 1-m aperture solar optical telescope for the space solar mission. Title: Structure and dynamics of the hot flaring loop-top source observed by Hinode, SDO, RHESSI, and STEREO Authors: Lee, Kyoung-Sun; Hara, Hirohisa; Watanabe, Kyoko; Joshi, Anand D.; Imada, Shinsuke; Brooks, David H.; Dang, Phillip; Shimizu, Toshifumi; Savage, Sabrina Bibcode: 2019AAS...23421605L Altcode: We have investigated an M1.3 flare on 2014 January 13 around 21:48 UT observed at the west limb using the Hinode, SDO, RHESSI, and STEREO. Especially, the Hinode/EIS scanned the flaring loop covering the loop-top region over the limb, which is a good target to investigate the dynamics of the flaring loop with their height. Using the multi-wavelength observations from the Hinode/EIS and SDO/AIA, we found a very hot emission above the loop-top observed in Fe XXIV and 131Å channel. Measuring the intensity, Doppler velocity and line width for the flaring loop, we found that hot emission observed at the cusp-like shape of the loop-top region which shows strong redshift about 500 km s-1 in Doppler velocity and strong enhancement of the non-thermal velocity (line width enhancement) larger than 100 km s-1. Combining with the STEREO observation, we have examined the 3D structure with loop tilt angle and have investigated the velocity distribution of the loop-top region. With the loop tilt angle, we could identify the strong redshift at the loop-top region may indicate an up-flow along the loop-top region. From RHESSI hard X-ray (HXR), and soft X-ray (SXR) emission, we found that the footpoint brightening region at the beginning of the flare has a both HXR (25-50 keV) and SXR (12-25 keV) emission in which imply that the region has non-thermal emission or accelerated particles. Then, within 10 minutes the soft X-ray (SXR) emission observed near the cusp shape region at loop top. The temporal variation of the HXR and SXR emissions and the Doppler velocity variation of the hot plasma component at the loop-top imply that the strong flow in a hot component near loop-top could be the evaporation flows which detected at the corona along the tilted loop. Moreover, The temporal evolution of the temperature observed by SDO/AIA and Hinode/EIS also shows the cooling process of the flare plasma which is consistent with the impulsively heated flare model. Title: Comparison of Scattering Polarization Signals Observed by CLASP: Possible Indication of the Hanle Effect Authors: Ishikawa, R.; Trujillo Bueno, J.; Uitenbroek, H.; Kubo, M.; Tsuneta, S.; Goto, M.; Kano, R.; Narukage, N.; Bando, T.; Katsukawa, Y.; Ishikawa, S.; Giono, G.; Suematsu, Y.; Hara, H.; Shimizu, T.; Sakao, T.; Winebarger, A.; Kobayashi, K.; Cirtain, J.; Champey, P.; Auchère, F.; Štěpán, J.; Belluzzi, L.; Asensio Ramos, A.; Manso Sainz, R.; De Pomtieu, B.; Ichimoto, K.; Carlsson, M.; Casini, R. Bibcode: 2019ASPC..526..305I Altcode: The Chromospheric Lyman-Alpha Spectro-Polarimeter (CLASP; Kano et al. 2012; Kobayashi et al. 2012; Kubo et al. 2014) observed, for the first time, the linear polarization produced by scattering processes in the hydrogen Lyman-α (121.57 nm) and Si III (120.56 nm) lines of the solar disk radiation. The complexity of the observed scattering polarization (i.e., conspicuous spatial variations in Q/I and U/I at spatial scales of 10″-20″ and the absence of center-to- limb variation at the Lyman-α center; see Kano et al. 2017) motivated us to search for possible hints of the operation of the Hanle effect by comparing: (a) the Lyman-α line center signal, for which the critical field strength (BH) for the onset of the Hanle effect is 53 G, (b) the Lyman-α wing, which is insensitive to the Hanle effect, and (c) the Si III line, whose BH = 290 G. We focus on four regions with different total unsigned photospheric magnetic fluxes (estimated from SDO/HMI observations), and compare the corresponding U/I spatial variations in the Lyman-α wing, Lyman-α center, and Si III line. The U/I signal in the Lyman-α wing shows an antisymmetric spatial distribution, which is caused by the presence of a bright structure in all the selected regions, regardless of the total unsigned photospheric magnetic flux. In an internetwork region, the Lyman-α center shows an antisymmetric spatial variation across the selected bright structure, but it does not show it in other more magnetized regions. In the Si III line, the spatial variation of U/I deviates from the above-mentioned antisymmetric shape as the total unsigned photospheric magnetic flux increases. We argue that a plausible explanation of this differential behavior is the operation of the Hanle effect. This work, presented in an oral contribution at this Workshop, has been published on The Astrophysical Journal (Ishikawa et al. 2017). Title: CLASP Constraints on the Magnetization and Geometrical Complexity of the Chromosphere-Corona Transition Region Authors: Trujillo Bueno, J.; Štěpán, J.; Belluzzi, L.; Asensio Ramos, A.; Manso Sainz, R.; del Pino Alemán, T.; Casini, R.; Ishikawa, R.; Kano, R.; Winebarger, A.; Auchère, F.; Narukage, N.; Kobayashi, K.; Bando, T.; Katsukawa, Y.; Kubo, M.; Ishikawa, S.; Giono, G.; Hara, H.; Suematsu, Y.; Shimizu, T.; Sakao, T.; Tsuneta, S.; Ichimoto, K.; Cirtain, J.; Champey, P.; De Pontieu, B.; Carlsson, M. Bibcode: 2018ApJ...866L..15T Altcode: 2018arXiv180908865T The Chromospheric Lyman-Alpha Spectro-Polarimeter (CLASP) is a suborbital rocket experiment that on 2015 September 3 measured the linear polarization produced by scattering processes in the hydrogen Lyα line of the solar disk radiation. The line-center photons of this spectral line radiation mostly stem from the chromosphere-corona transition region (TR). These unprecedented spectropolarimetric observations revealed an interesting surprise, namely that there is practically no center-to-limb variation (CLV) in the Q/I line-center signals. Using an analytical model, we first show that the geometric complexity of the corrugated surface that delineates the TR has a crucial impact on the CLV of the Q/I and U/I line-center signals. Second, we introduce a statistical description of the solar atmosphere based on a 3D model derived from a state-of-the-art radiation magnetohydrodynamic simulation. Each realization of the statistical ensemble is a 3D model characterized by a given degree of magnetization and corrugation of the TR, and for each such realization we solve the full 3D radiative transfer problem taking into account the impact of the CLASP instrument degradation on the calculated polarization signals. Finally, we apply the statistical inference method presented in a previous paper to show that the TR of the 3D model that produces the best agreement with the CLASP observations has a relatively weak magnetic field and a relatively high degree of corrugation. We emphasize that a suitable way to validate or refute numerical models of the upper solar chromosphere is by confronting calculations and observations of the scattering polarization in ultraviolet lines sensitive to the Hanle effect. Title: A Statistical Inference Method for Interpreting the CLASP Observations Authors: Štěpán, J.; Trujillo Bueno, J.; Belluzzi, L.; Asensio Ramos, A.; Manso Sainz, R.; del Pino Alemán, T.; Casini, R.; Kano, R.; Winebarger, A.; Auchère, F.; Ishikawa, R.; Narukage, N.; Kobayashi, K.; Bando, T.; Katsukawa, Y.; Kubo, M.; Ishikawa, S.; Giono, G.; Hara, H.; Suematsu, Y.; Shimizu, T.; Sakao, T.; Tsuneta, S.; Ichimoto, K.; Cirtain, J.; Champey, P.; De Pontieu, B.; Carlsson, M. Bibcode: 2018ApJ...865...48S Altcode: 2018arXiv180802725S On 2015 September 3, the Chromospheric Lyman-Alpha SpectroPolarimeter (CLASP) successfully measured the linear polarization produced by scattering processes in the hydrogen Lyα line of the solar disk radiation, revealing conspicuous spatial variations in the Q/I and U/I signals. Via the Hanle effect, the line-center Q/I and U/I amplitudes encode information on the magnetic field of the chromosphere-corona transition region, but they are also sensitive to the three-dimensional structure of this corrugated interface region. With the help of a simple line-formation model, here we propose a statistical inference method for interpreting the Lyα line-center polarization observed by CLASP. Title: Sunrise Chromospheric Infrared spectroPolarimeter (SCIP) for the SUNRISE balloon-borne solar observatory Authors: Suematsu, Yoshinori; Katsukawa, Yukio; Hara, Hirohisa; Ichimoto, Kiyoshi; Shimizu, Toshifumi; Kubo, Masahito; Barthol, Peter; Riethmueller, Tino; Gandorfer, Achim; Feller, Alex; Orozco Suárez, David; Del Toro Iniesta, Jose Carlos; Kano, Ryouhei; Ishikawa, Shin-nosuke; Ishikawa, Ryohko; Tsuzuki, Toshihiro; Uraguchi, Fumihiro; Quintero Noda, Carlos; Tamura, Tomonori; Oba, Takayoshi; Kawabata, Yusuke; Nagata, Shinichi; Anan, Tetsu; Cobos Carrascosa, Juan Pedro; Lopez Jimenez, Antonio Carlos; Balaguer Jimenez, Maria; Solanki, Sami Bibcode: 2018cosp...42E3285S Altcode: The SUNRISE balloon-borne solar observatory carries a 1 m aperture optical telescope, and allows us to perform seeing-free continuous observations at visible-IR wavelengths from an altitude higher than 35 km. In the past two flights, in 2009 and 2013, observations mainly focused on fine structures of photospheric magnetic fields. For the third flight planned for 2021, we are developing a new instrument for conducting spectro-polarimetry of spectral lines formed over a larger height range in the solar atmosphere from the photosphere to the chromosphere. Targets of the spectro-polarimetric observation are (1) to determine 3D magnetic structure from the photosphere to the chromosphere, (2) to trace MHD waves from the photosphere to the chromosphere, and (3) to reveal the mechanism driving chromospheric jets, by measuring height- and time-dependent velocities and magnetic fields. To achieve these goals, a spectro-polarimeter called SCIP (Sunrise Chromospheric Infrared spectroPolarimeter) is designed to observe near-infrared spectrum lines sensitive to solar magnetic fields. The spatial and spectral resolutions are 0.2 arcsec and 200,000, respectively, while 0.03% polarimetric sensitivity is achieved within a 10 sec integration time. The optical system employs an Echelle grating and off-axis aspheric mirrors to observe the two wavelength ranges centered at 850 nm and 770 nm simultaneously by two cameras. Polarimetric measurements are performed using a rotating waveplate and polarization beam-splitters in front of the cameras. For detecting minute polarization signals with good precision, we carefully assess the temperature dependence of polarization optics, and make the opto-structural design that minimizes the thermal deformation of the spectrograph optics. Another key technique is to attain good (better than 30 msec) synchronization among the rotating phase of the waveplate, read-out timing of cameras, and step timing of a slit-scanning mirror. On-board accumulation and data processing are also critical because we cannot store all the raw data read-out from the cameras. We demonstrate that we can reduce the data down to almost 10% with loss-less image compression and without sacrificing polarimetric information in the data. The SCIP instrument is developed by internal collaboration among Japanese institutes including Japan Aerospace Exploration Agency (JAXA), the Spanish Sunrise consortium, and the German Max Planck Institute for Solar System Research (MPS) with a leadership of the National Astronomical Observatory of Japan (NAOJ). Title: Probing the evolution of a coronal cavity within a solar coronal mass ejection. Authors: Harra, Louise K.; Doschek, G. A.; Hara, Hirohisa; Long, David; Warren, Harry; Matthews, Sarah; Lee, Kyoung-Sun; Jenkins, Jack Bibcode: 2018cosp...42E1381H Altcode: On the 10 September 2017, an X-class solar flare erupted at the solar limb. The associated coronal mass ejection (CME) had the classic three part structure with a bright core surrounded by a dark cavity. This event was captured perfectly by the Hinode EUV imaging spectrometer (EIS). The EIS instrument captured spectroscopically the flaring loops, the current sheet and the cavity for the first time. In the 'standard flare model', magnetic reconnection of coronal loops occurs following the eruption of a magnetic flux rope. The flux rope is a key element of the flare process and eruption but is inherently difficult to observe. Dark cavities observed within a CME are assumed to be flux ropes. The observations we describe here, provide an insight into the characteristics of a cavity, and how the rapid injection of energy from the flare underneath forces the rapid expansion of the flux rope resulting in the eruption. Doppler shifts of over 200 km/s are measured at either end of the cavity. There is mixed temperature plasma - cool material in the centre that also has strong flows, and hot FeXXIV emission being observed. SDO Atmospheric Imaging Assembly (AIA) data shows that the cavity erupts rapidly, and is being driven by the non-thermal energy input from the flare below as measured from Fermi data. Title: Current State of UV Spectro-Polarimetry and its Future Direction Authors: Ishikawa, Ryohko; Sakao, Taro; Katsukawa, Yukio; Hara, Hirohisa; Ichimoto, Kiyoshi; Shimizu, Toshifumi; Kubo, Masahito; Auchere, Frederic; De Pontieu, Bart; Winebarger, Amy; Kobayashi, . Ken; Kano, Ryouhei; Narukage, Noriyuki; Trujillo Bueno, Javier; Song, Dong-uk; Manso Sainz, Rafael; Asensio Ramos, Andres; Leenaarts, Jorritt; Carlsson, Mats; Bando, Takamasa; Ishikawa, Shin-nosuke; Tsuneta, Saku; Belluzzi, Luca; Suematsu, Yoshinori; Giono, Gabriel; Yoshida, Masaki; Goto, Motoshi; Del Pino Aleman, Tanausu; Stepan, Jiri; Okamoto, Joten; Tsuzuki, Toshihiro; Uraguchi, Fumihiro; Champey, Patrick; Alsina Ballester, Ernest; Casini, Roberto; McKenzie, David; Rachmeler, Laurel; Bethge, Christian Bibcode: 2018cosp...42E1564I Altcode: To obtain quantitative information on the magnetic field in low beta regions (i.e., upper chromosphere and above) has been increasingly important to understand the energetic phenomena of the outer solar atmosphere such as flare, coronal heating, and the solar wind acceleration. In the UV range, there are abundant spectral lines that originate in the upper chromosphere and transition region. However, the Zeeman effect in these spectral lines does not give rise to easily measurable polarization signals because of the weak magnetic field strength and the larger Doppler broadening compared with the Zeeman effect. Instead, the Hanle effect in UV lines is expected to be a suitable diagnostic tool of the magnetic field in the upper atmospheric layers. To investigate the validity of UV spectro-polarimetry and the Hanle effect, the Chromospheric Lyman-Alpha Spectro-Polarimeter (CLASP), which is a NASA sounding- rocket experiment, was launched at White Sands in US on September 3, 2015. During its 5 minutes ballistic flight, it successfully performed spectro-polarimetric observations of the hydrogen Lyman-alpha line (121.57 nm) with an unprecedentedly high polarization sensitivity of 0.1% in this wavelength range. CLASP observed the linear polarization produced by scattering process in VUV lines for the first time and detected the polarization signals which indicate the operation of the Hanle effect. Following the success of CLASP, we are confident that UV spectro-polarimetry is the way to proceed, and we are planning the second flight of CLASP (CLASP2: Chromospheric LAyer SpectroPolarimeter 2). For this second flight we will carry out spectro-polarimetry in the Mg II h and k lines around 280 nm, with minimum modifications of the CLASP1 instrument. The linear polarization in the Mg II k line is induced by scattering processes and the Hanle effect, being sensitive to magnetic field strengths of 5 to 50 G. In addition, the circular polarizations in the Mg II h and k lines induced by the Zeeman effect can be measurable in at least plage and active regions. The combination of the Hanle and Zeeman effects could help us to more reliably infer the magnetic fields of the upper solar chromosphere. CLASP2 was selected for flight and is being developed for launch in the spring of 2019.Based on these sounding rocket experiments (CLASP1 and 2), we aim at establishing the strategy and refining the instrument concept for future space missions to explore the enigmatic atmospheric layers via UV spectro-polarimetry. Title: Optical alignment of the high-precision UV spectro-polarimeter (CLASP2) Authors: Song, Donguk; Ishikawa, Ryohko; Kano, Ryouhei; Yoshida, Masaki; Tsuzuki, Toshihiro; Uraguchi, Fumihiro; Shinoda, Kazuya; Hara, Hirohisa; Okamoto, Takenori J.; Auchère, Frédéric; McKenzie, David E.; Rachmeler, Laurel A.; Trujillo Bueno, Javier Bibcode: 2018SPIE10699E..2WS Altcode: Chromospheric LAyer Spectro-Polarimeter (CLASP2) is our next sounding rocket experiment after the success of Chromospheric Lyman-Alpha Spectro-Polarimeter (CLASP1). CLASP2 is scheduled to launch in 2019, and aims to achieve high precision measurements (< 0.1 %) of the linear and circular polarizations in the Mg ii h and k lines near the 280 nm, whose line cores originate in the upper solar chromosphere. The CLASP2 spectro-polarimeter follows very successful design concept of the CLASP1 instrument with the minimal modification. A new grating was fabricated with the same radius of curvature as the CLASP1 grating, but with a different ruling density. This allows us to essentially reuse the CLASP1 mechanical structures and layout of the optics. However, because the observing wavelength of CLASP2 is twice longer than that of CLASP1, a magnifier optical system was newly added in front of the cameras to double the focal length of CLASP2 and to maintain the same wavelength resolution as CLASP1 (0.01 nm). Meanwhile, a careful optical alignment of the spectro-polarimeter is required to reach the 0.01 nm wavelength resolution. Therefore, we established an efficient alignment procedure for the CLASP2 spectro-polarimeter based on an experience of CLASP1. Here, we explain in detail the methods for achieving the optical alignment of the CLASP2 spectro-polarimeter and discuss our results by comparing with the performance requirements. Title: Plasma Evolution within an Erupting Coronal Cavity Authors: Long, David M.; Harra, Louise K.; Matthews, Sarah A.; Warren, Harry P.; Lee, Kyoung-Sun; Doschek, George A.; Hara, Hirohisa; Jenkins, Jack M. Bibcode: 2018ApJ...855...74L Altcode: 2018arXiv180201391L Coronal cavities have previously been observed to be associated with long-lived quiescent filaments and are thought to correspond to the associated magnetic flux rope. Although the standard flare model predicts a coronal cavity corresponding to the erupting flux rope, these have only been observed using broadband imaging data, restricting an analysis to the plane-of-sky. We present a unique set of spectroscopic observations of an active region filament seen erupting at the solar limb in the extreme ultraviolet. The cavity erupted and expanded rapidly, with the change in rise phase contemporaneous with an increase in nonthermal electron energy flux of the associated flare. Hot and cool filamentary material was observed to rise with the erupting flux rope, disappearing suddenly as the cavity appeared. Although strongly blueshifted plasma continued to be observed flowing from the apex of the erupting flux rope, this outflow soon ceased. These results indicate that the sudden injection of energy from the flare beneath forced the rapid eruption and expansion of the flux rope, driving strong plasma flows, which resulted in the eruption of an under-dense filamentary flux rope. Title: Photospheric and Coronal Abundances in an X8.3 Class Limb Flare Authors: Doschek, G. A.; Warren, H. P.; Harra, L. K.; Culhane, J. L.; Watanabe, T.; Hara, H. Bibcode: 2018ApJ...853..178D Altcode: We analyze solar elemental abundances in coronal post-flare loops of an X8.3 flare (SOL2017-09-10T16:06) observed on the west limb on 2017 September 10 near 18 UT using spectra recorded by the Extreme-ultraviolet Imaging Spectrometer (EIS) on the Hinode spacecraft. The abundances in the corona can differ from photospheric abundances due to the first ionization potential (FIP) effect. In some loops of this flare, we find that the abundances appear to be coronal at the loop apices or cusps, but steadily transform from coronal to photospheric as the loop footpoint is approached. This result is found from the intensity ratio of a low-FIP ion spectral line (Ca XIV) to a high-FIP ion spectral line (Ar XIV) formed at about the same temperature (4-5 MK). Both lines are observed close in wavelength. Temperature, which could alter the interpretation, does not appear to be a factor based on intensity ratios of Ca XV lines to a Ca XIV line. We discuss the abundance result in terms of the Laming model of the FIP effect, which is explained by the action of the ponderomotive force in magnetohydrodynamic (MHD) waves in coronal loops and in the underlying chromosphere. Title: Coronal Heating: Issues Revealed from Hinode Observations Authors: Hara, Hirohisa Bibcode: 2018ASSL..449...65H Altcode: No abstract at ADS Title: From Hinode to the Next-Generation Solar Observation Missions Authors: Ichimoto, Kiyoshi; Hara, Hirohisa; Katsukawa, Yukio; Ishikawa, Ryoko Bibcode: 2018ASSL..449..231I Altcode: No abstract at ADS Title: Resonant Electron Impact Excitation of 3d Levels in Fe14+ and Fe15+ Authors: Tsuda, Takashi; Shimizu, Erina; Ali, Safdar; Sakaue, Hiroyuki A.; Kato, Daiji; Murakami, Izumi; Hara, Hirohisa; Watanabe, Tetsuya; Nakamura, Nobuyuki Bibcode: 2017ApJ...851...82T Altcode: 2017arXiv171003548T We present laboratory spectra of the 3p-3d transitions in Fe14+ and Fe15+ excited with a mono-energetic electron beam. In the energy-dependent spectra obtained by sweeping the electron energy, resonant excitation is confirmed as an intensity enhancement at specific electron energies. The experimental results are compared with theoretical cross sections calculated based on fully relativistic wave functions and the distorted wave approximation. Comparisons between the experimental and theoretical results show good agreement for the resonance strength. A significant discrepancy is, however, found for the non-resonant cross section in Fe14+. This discrepancy is considered to be the fundamental cause of the previously reported inconsistency of the model with the observed intensity ratio between the {}3{P}2{--}{}3{D}3 and {}1{P}1{--}{}1{D}2 transitions. Title: SOLARIS: Solar Sail Investigation of the Sun Authors: Appourchaux, Thierry; Auchère, Frédéric; Antonucci, Ester; Gizon, Laurent; MacDonald, Malcolm; Hara, Hirohisa; Sekii, Takashi; Moses, Daniel; Vourlidas, Angelos Bibcode: 2017arXiv170708193A Altcode: In this paper, we detail the scientific objectives and outline a strawman payload of the SOLAR sail Investigation of the Sun (SOLARIS). The science objectives are to study the 3D structure of the solar magnetic and velocity field, the variation of total solar irradiance with latitude, and the structure of the corona. We show how we can meet these science objective using solar-sail technologies currently under development. We provide a tentative mission profile considering several trade-off approaches. We also provide a tentative mass budget breakdown and a perspective for a programmatic implementation. Title: Measuring Velocities in the Early Stage of an Eruption: Using “Overlappogram” Data from Hinode EIS Authors: Harra, Louise K.; Hara, Hirohisa; Doschek, George A.; Matthews, Sarah; Warren, Harry; Culhane, J. Leonard; Woods, Magnus M. Bibcode: 2017ApJ...842...58H Altcode: In order to understand the onset phase of a solar eruption, plasma parameter measurements in the early phases are key to constraining models. There are two current instrument types that allow us to make such measurements: narrow-band imagers and spectrometers. In the former case, even narrow-band filters contain multiple emission lines, creating some temperature confusion. With imagers, however, rapid cadences are achievable and the field of view can be large. Velocities of the erupting structures can be measured by feature tracking. In the spectrometer case, slit spectrometers can provide spectrally pure images by “rastering” the slit to build up an image. This method provides limited temporal resolution, but the plasma parameters can be accurately measured, including velocities along the line of sight. Both methods have benefits and are often used in tandem. In this paper we demonstrate for the first time that data from the wide slot on the Hinode EUV Imaging Spectrometer, along with imaging data from AIA, can be used to deconvolve velocity information at the start of an eruption, providing line-of-sight velocities across an extended field of view. Using He II 256 Å slot data at flare onset, we observe broadening or shift(s) of the emission line of up to ±280 km s-1. These are seen at different locations—the redshifted plasma is seen where the hard X-ray source is later seen (energy deposition site). In addition, blueshifted plasma shows the very early onset of the fast rise of the filament. Title: Neon-like Iron Ion Lines Measured in NIFS/Large Helical Device (LHD) and Hinode/EUV Imaging Spectrometer (EIS) Authors: Watanabe, Tetsuya; Hara, Hirohisa; Murakami, Izumi; Kato, Daiji; Sakaue, Hiroyuki A.; Morita, Shigeru; Suzuki, Chihiro; Tamura, Naoki; Yamamoto, Norimasa; Nakamura, Nobuyuki Bibcode: 2017ApJ...842...12W Altcode: Line intensities emerging from the Ne-sequence iron ion (Fe XVII) are measured in the laboratory, by the Large Helical Device at the National Institute for Fusion Science, and in the solar corona by the EUV Imaging Spectrometer (EIS) on board the Hinode mission. The intensity ratios of Fe XVII λ 204.6/λ 254.8 are derived in the laboratory by unblending the contributions of the Fe XIII and XII line intensities. They are consistent with theoretical predictions and solar observations, the latter of which endorses the in-flight radiometric calibrations of the EIS instrument. The still remaining temperature-dependent behavior of the line ratio suggests the contamination of lower-temperature iron lines that are blended with the λ 204.6 line. Title: Indication of the Hanle Effect by Comparing the Scattering Polarization Observed by CLASP in the Lyα and Si III 120.65 nm Lines Authors: Ishikawa, R.; Trujillo Bueno, J.; Uitenbroek, H.; Kubo, M.; Tsuneta, S.; Goto, M.; Kano, R.; Narukage, N.; Bando, T.; Katsukawa, Y.; Ishikawa, S.; Giono, G.; Suematsu, Y.; Hara, H.; Shimizu, T.; Sakao, T.; Winebarger, A.; Kobayashi, K.; Cirtain, J.; Champey, P.; Auchère, F.; Štěpán, J.; Belluzzi, L.; Asensio Ramos, A.; Manso Sainz, R.; De Pontieu, B.; Ichimoto, K.; Carlsson, M.; Casini, R. Bibcode: 2017ApJ...841...31I Altcode: The Chromospheric Lyman-Alpha Spectro-Polarimeter is a sounding rocket experiment that has provided the first successful measurement of the linear polarization produced by scattering processes in the hydrogen Lyα line (121.57 nm) radiation of the solar disk. In this paper, we report that the Si III line at 120.65 nm also shows scattering polarization and we compare the scattering polarization signals observed in the Lyα and Si III lines in order to search for observational signatures of the Hanle effect. We focus on four selected bright structures and investigate how the U/I spatial variations vary between the Lyα wing, the Lyα core, and the Si III line as a function of the total unsigned photospheric magnetic flux estimated from Solar Dynamics Observatory/Helioseismic and Magnetic Imager observations. In an internetwork region, the Lyα core shows an antisymmetric spatial variation across the selected bright structure, but it does not show it in other more magnetized regions. In the Si III line, the spatial variation of U/I deviates from the above-mentioned antisymmetric shape as the total unsigned photospheric magnetic flux increases. A plausible explanation of this difference is the operation of the Hanle effect. We argue that diagnostic techniques based on the scattering polarization observed simultaneously in two spectral lines with very different sensitivities to the Hanle effect, like Lyα and Si III, are of great potential interest for exploring the magnetism of the upper solar chromosphere and transition region. Title: Measurements of density dependent intensity ratios of extreme ultraviolet line emission from Fe X, XI, and XII Authors: Shimizu, Erina; Ali, Safdar; Tsuda, Takashi; Sakaue, Hiroyuki A.; Kato, Daiji; Murakami, Izumi; Hara, Hirohisa; Watanabe, Tetsuya; Nakamura, Nobuyuki Bibcode: 2017A&A...601A.111S Altcode: We report high-resolution density dependent intensity ratio measurements for middle charge states of iron in the extreme ultraviolet (EUV) spectral wavelength range of 160-200 Å. The measurements were performed at the Tokyo EBIT laboratory by employing a flat-field grazing incidence spectrometer installed on a low energy compact electron beam ion trap. The intensity ratios for several line pairs stemming from Fe X, Fe XI and Fe XII were extracted from spectra collected at the electron beam energies of 340 and 400 eV by varying the beam current between 7.5 and 12 mA at each energy. In addition, the effective electron densities were obtained experimentally by imaging the electron beam profile and ion cloud size with a pinhole camera and visible spectrometer, respectively. In this paper, the experimental results are compared with previous data from the literature and with the present calculations performed using a collisional-radiative model. Our experimental results show a rather good agreement with the calculations and previous reported results. Title: Polarization Calibration of the Chromospheric Lyman-Alpha SpectroPolarimeter for a 0.1% Polarization Sensitivity in the VUV Range. Part II: In-Flight Calibration Authors: Giono, G.; Ishikawa, R.; Narukage, N.; Kano, R.; Katsukawa, Y.; Kubo, M.; Ishikawa, S.; Bando, T.; Hara, H.; Suematsu, Y.; Winebarger, A.; Kobayashi, K.; Auchère, F.; Trujillo Bueno, J.; Tsuneta, S.; Shimizu, T.; Sakao, T.; Cirtain, J.; Champey, P.; Asensio Ramos, A.; Štěpán, J.; Belluzzi, L.; Manso Sainz, R.; De Pontieu, B.; Ichimoto, K.; Carlsson, M.; Casini, R.; Goto, M. Bibcode: 2017SoPh..292...57G Altcode: The Chromospheric Lyman-Alpha SpectroPolarimeter is a sounding rocket instrument designed to measure for the first time the linear polarization of the hydrogen Lyman-α line (121.6 nm). The instrument was successfully launched on 3 September 2015 and observations were conducted at the solar disc center and close to the limb during the five-minutes flight. In this article, the disc center observations are used to provide an in-flight calibration of the instrument spurious polarization. The derived in-flight spurious polarization is consistent with the spurious polarization levels determined during the pre-flight calibration and a statistical analysis of the polarization fluctuations from solar origin is conducted to ensure a 0.014% precision on the spurious polarization. The combination of the pre-flight and the in-flight polarization calibrations provides a complete picture of the instrument response matrix, and a proper error transfer method is used to confirm the achieved polarization accuracy. As a result, the unprecedented 0.1% polarization accuracy of the instrument in the vacuum ultraviolet is ensured by the polarization calibration. Title: Discovery of Scattering Polarization in the Hydrogen Lyα Line of the Solar Disk Radiation Authors: Kano, R.; Trujillo Bueno, J.; Winebarger, A.; Auchère, F.; Narukage, N.; Ishikawa, R.; Kobayashi, K.; Bando, T.; Katsukawa, Y.; Kubo, M.; Ishikawa, S.; Giono, G.; Hara, H.; Suematsu, Y.; Shimizu, T.; Sakao, T.; Tsuneta, S.; Ichimoto, K.; Goto, M.; Belluzzi, L.; Štěpán, J.; Asensio Ramos, A.; Manso Sainz, R.; Champey, P.; Cirtain, J.; De Pontieu, B.; Casini, R.; Carlsson, M. Bibcode: 2017ApJ...839L..10K Altcode: 2017arXiv170403228K There is a thin transition region (TR) in the solar atmosphere where the temperature rises from 10,000 K in the chromosphere to millions of degrees in the corona. Little is known about the mechanisms that dominate this enigmatic region other than the magnetic field plays a key role. The magnetism of the TR can only be detected by polarimetric measurements of a few ultraviolet (UV) spectral lines, the Lyα line of neutral hydrogen at 121.6 nm (the strongest line of the solar UV spectrum) being of particular interest given its sensitivity to the Hanle effect (the magnetic-field-induced modification of the scattering line polarization). We report the discovery of linear polarization produced by scattering processes in the Lyα line, obtained with the Chromospheric Lyman-Alpha Spectro-Polarimeter (CLASP) rocket experiment. The Stokes profiles observed by CLASP in quiet regions of the solar disk show that the Q/I and U/I linear polarization signals are of the order of 0.1% in the line core and up to a few percent in the nearby wings, and that both have conspicuous spatial variations with scales of ∼10 arcsec. These observations help constrain theoretical models of the chromosphere-corona TR and extrapolations of the magnetic field from photospheric magnetograms. In fact, the observed spatial variation from disk to limb of polarization at the line core and wings already challenge the predictions from three-dimensional magnetohydrodynamical models of the upper solar chromosphere. Title: UV/EUV High-Throughput Spectroscopic Telescope: A Next Generation Solar Physics Mission white paper Authors: Imada, S.; Shimizu, T.; Kawate, T.; Hara, H.; Watanabe, T. Bibcode: 2017arXiv170104972I Altcode: The origin of the activity in the solar corona is a long-standing problem in solar physics. Recent satellite observations, such as Hinode, Solar Dynamics Observatory (SDO), Interface Region Imaging Spectrograph (IRIS), show the detail characteristics of the solar atmosphere and try to reveal the energy transfer from the photosphere to the corona through the magnetic fields and its energy conversion by various processes. However, quantitative estimation of energy transfer along the magnetic field is not enough. There are mainly two reason why it is difficult to observe the energy transfer from photosphere to corona; 1) spatial resolution gap between photosphere (a few 0.1 arcsec) and corona (a few arcsec), 2) lack in temperature coverage. Furthermore, there is not enough observational knowledge of the physical parameters in the energy dissipation region. There are mainly three reason why it is difficult to observe in the vicinity of the energy dissipation region; 1) small spatial scale, 2) short time scale, 3) low emission. It is generally believed that the energy dissipation occurs in the very small scale and its duration is very short (10 second). Further, the density in the dissipation region might be very low. Therefore, the high spatial and temporal resolution UV/EUV spectroscopic observation with wide temperature coverage is crucial to estimate the energy transport from photosphere to corona quantitatively and diagnose the plasma dynamics in the vicinity of the energy dissipation region. Main Science Target for the telescope is quantitative estimation for the energy transfer from the photosphere to the corona, and clarification of the plasma dynamics in the vicinity of the energy dissipation region, where is the key region for coronal heating, solar wind acceleration, and/or solar flare, by the high spatial and temporal resolution UV/EUV spectroscopy. Title: Polarization Calibration of the Chromospheric Lyman-Alpha SpectroPolarimeter for a 0.1 % Polarization Sensitivity in the VUV Range. Part I: Pre-flight Calibration Authors: Giono, G.; Ishikawa, R.; Narukage, N.; Kano, R.; Katsukawa, Y.; Kubo, M.; Ishikawa, S.; Bando, T.; Hara, H.; Suematsu, Y.; Winebarger, A.; Kobayashi, K.; Auchère, F.; Trujillo Bueno, J. Bibcode: 2016SoPh..291.3831G Altcode: 2016SoPh..tmp..177G The Chromospheric Lyman-Alpha SpectroPolarimeter (CLASP) is a sounding rocket experiment designed to measure for the first time the linear polarization of the hydrogen Lyman-α line (121.6 nm) and requires a 0.1 % polarization sensitivity, which is unprecedented for a spectropolarimeter in the vacuum UV (VUV) spectral range. Title: Discovery of Ubiquitous Fast-Propagating Intensity Disturbances by the Chromospheric Lyman Alpha Spectropolarimeter (CLASP) Authors: Kubo, M.; Katsukawa, Y.; Suematsu, Y.; Kano, R.; Bando, T.; Narukage, N.; Ishikawa, R.; Hara, H.; Giono, G.; Tsuneta, S.; Ishikawa, S.; Shimizu, T.; Sakao, T.; Winebarger, A.; Kobayashi, K.; Cirtain, J.; Champey, P.; Auchère, F.; Trujillo Bueno, J.; Asensio Ramos, A.; Štěpán, J.; Belluzzi, L.; Manso Sainz, R.; De Pontieu, B.; Ichimoto, K.; Carlsson, M.; Casini, R.; Goto, M. Bibcode: 2016ApJ...832..141K Altcode: High-cadence observations by the slit-jaw (SJ) optics system of the sounding rocket experiment known as the Chromospheric Lyman Alpha Spectropolarimeter (CLASP) reveal ubiquitous intensity disturbances that recurrently propagate in either the chromosphere or the transition region or both at a speed much higher than the speed of sound. The CLASP/SJ instrument provides a time series of two-dimensional images taken with broadband filters centered on the Lyα line at a 0.6 s cadence. The multiple fast-propagating intensity disturbances appear in the quiet Sun and in an active region, and they are clearly detected in at least 20 areas in a field of view of 527″ × 527″ during the 5 minute observing time. The apparent speeds of the intensity disturbances range from 150 to 350 km s-1, and they are comparable to the local Alfvén speed in the transition region. The intensity disturbances tend to propagate along bright elongated structures away from areas with strong photospheric magnetic fields. This suggests that the observed fast-propagating intensity disturbances are related to the magnetic canopy structures. The maximum distance traveled by the intensity disturbances is about 10″, and the widths are a few arcseconds, which are almost determined by a pixel size of 1.″03. The timescale of each intensity pulse is shorter than 30 s. One possible explanation for the fast-propagating intensity disturbances observed by CLASP is magnetohydrodynamic fast-mode waves. Title: The Characteristics of Solar X-Class Flares and CMEs: A Paradigm for Stellar Superflares and Eruptions? Authors: Harra, Louise K.; Schrijver, Carolus J.; Janvier, Miho; Toriumi, Shin; Hudson, Hugh; Matthews, Sarah; Woods, Magnus M.; Hara, Hirohisa; Guedel, Manuel; Kowalski, Adam; Osten, Rachel; Kusano, Kanya; Lueftinger, Theresa Bibcode: 2016SoPh..291.1761H Altcode: 2016SoPh..tmp..111H This paper explores the characteristics of 42 solar X-class flares that were observed between February 2011 and November 2014, with data from the Solar Dynamics Observatory (SDO) and other sources. This flare list includes nine X-class flares that had no associated CMEs. In particular our aim was to determine whether a clear signature could be identified to differentiate powerful flares that have coronal mass ejections (CMEs) from those that do not. Part of the motivation for this study is the characterization of the solar paradigm for flare/CME occurrence as a possible guide to the stellar observations; hence we emphasize spectroscopic signatures. To do this we ask the following questions: Do all eruptive flares have long durations? Do CME-related flares stand out in terms of active-region size vs. flare duration? Do flare magnitudes correlate with sunspot areas, and, if so, are eruptive events distinguished? Is the occurrence of CMEs related to the fraction of the active-region area involved? Do X-class flares with no eruptions have weaker non-thermal signatures? Is the temperature dependence of evaporation different in eruptive and non-eruptive flares? Is EUV dimming only seen in eruptive flares? We find only one feature consistently associated with CME-related flares specifically: coronal dimming in lines characteristic of the quiet-Sun corona, i.e. 1 - 2 MK. We do not find a correlation between flare magnitude and sunspot areas. Although challenging, it will be of importance to model dimming for stellar cases and make suitable future plans for observations in the appropriate wavelength range in order to identify stellar CMEs consistently. Title: Optical alignment of the Chromospheric Lyman-Alpha Spectro-Polarimeter using sophisticated methods to minimize activities under vacuum Authors: Giono, G.; Katsukawa, Y.; Ishikawa, R.; Narukage, N.; Kano, R.; Kubo, M.; Ishikawa, S.; Bando, T.; Hara, H.; Suematsu, Y.; Winebarger, A.; Kobayashi, K.; Auchère, F.; Trujillo Bueno, J. Bibcode: 2016SPIE.9905E..3DG Altcode: The Chromospheric Lyman-Alpha Spectro-Polarimeter (CLASP) is a sounding-rocket instrument developed at the National Astronomical Observatory of Japan (NAOJ) as a part of an international collaboration. The instrument main scientific goal is to achieve polarization measurement of the Lyman-α line at 121.56 nm emitted from the solar upper-chromosphere and transition region with an unprecedented 0.1% accuracy. The optics are composed of a Cassegrain telescope coated with a "cold mirror" coating optimized for UV reflection and a dual-channel spectrograph allowing for simultaneous observation of the two orthogonal states of polarization. Although the polarization sensitivity is the most important aspect of the instrument, the spatial and spectral resolutions of the instrument are also crucial to observe the chromospheric features and resolve the Ly-α profiles. A precise alignment of the optics is required to ensure the resolutions, but experiments under vacuum conditions are needed since Ly-α is absorbed by air, making the alignment experiments difficult. To bypass this issue, we developed methods to align the telescope and the spectrograph separately in visible light. We explain these methods and present the results for the optical alignment of the CLASP telescope and spectrograph. We then discuss the combined performances of both parts to derive the expected resolutions of the instrument, and compare them with the flight observations performed on September 3rd 2015. Title: Development of a near-infrared detector and a fiber-optic integral field unit for a space solar observatory SOLAR-C Authors: Katsukawa, Yukio; Kamata, Yukiko; Anan, Tetsu; Hara, Hirohisa; Suematsu, Yoshinori; Bando, Takamasa; Ichimoto, Kiyoshi; Shimizu, Toshifumi Bibcode: 2016SPIE.9904E..5IK Altcode: We are developing a high sensitivity and fast readout near-infrared (NIR) detector and an integral field unit (IFU) for making spectro-polarimetric observations of rapidly varying chromospheric spectrum lines, such as He I 1083 nm and Ca II 854 nm, in the next space-based solar mission SOLAR-C. We made tests of a 1.7 μm cutoff H2RG detector with the SIDECAR ASIC for the application in SOLAR-C. It's important to verify its perfor- mance in the temperature condition around -100 °C, which is hotter than the typical temperature environment used for a NIR detector. We built a system for testing the detector between -70 °C and -140 °C. We verified linearity, read-out noise, and dark current in both the slow and fast readout modes. We found the detector has to be cooled down lower than -100 °C because of significant increase of the number of hot pixels in the hotter environment. The compact and polarization maintenance IFU was designed using fiber-optic ribbons consisting of rectangular cores which exhibit good polarization maintenance. A Silicone adhesive DC-SE9187L was used to hold the fragile fiber-optic ribbons in a metal housing. Polarization maintenance property was confirmed though polarization calibration as well as temperature control are required to suppress polarization crosstalk and to achieve the polarization accuracy in SOLAR-C. Title: MAVEN observations of the Cycle 24 solar wind conditions at 1.5 AU Authors: Lee, Christina O.; Halekas, J.; Espley, J.; Thiemann, E.; Luhmann, J. G.; Hara; Lillis, R. J.; Larson, D.; Eparvier, F.; Jakosky, B. M. Bibcode: 2016shin.confE.177L Altcode: The Mars Atmosphere and Volatile EvolutioN (MAVEN) spacecraft went into orbit around Mars on 21 September 2014. The mission was designed in part to study the response of the upper atmosphere, ionosphere, and magnetosphere of Mars to solar and solar wind inputs. When MAVEN is on the Martian dayside and orbiting around its apoapsis altitude of 6200 km, the suite of instruments onboard can measure the upstream solar wind plasma (density, velocity), interplanetary magnetic field (magnitude and direction) and particle counts of SEP protons and electrons, as well as the EUV solar irradiance. Given the suite of plasma, particles, and field instruments onboard MAVEN, these 1.5 AU observations provide a unique and comprehensive data set that may be used to study the heliospheric conditions beyond the orbits of Earth and STEREO. Such studies may include understanding the dynamics and evolution of ICMEs and CIRs from the Sun out to 1.5 AU, or comparing the space weather effects observed at 1 AU and 1.5 AU for a given solar-heliospheric event period. We will present an overview of the space weather conditions observed thus far by MAVEN and highlight a number of space weather events at Mars triggered by CMEs, SEPs, flares, and CIRs of cycle 24. Numerical 3D simulations from WSA-Enlil-cone as well as observations from SOHO/LASCO, SDO/AIA, STEREO, and ACE will also be presented to provide global context to the events discussed. Title: Recent progress of SPAN towards neutrino mass spectroscopy Authors: Masuda, T.; Hara, H.; Miyamoto, Y.; Sasao, N.; Tanaka, M.; Uetake, S.; Yoshimi, A.; Yoshimura, K.; Yoshimura, M. Bibcode: 2016JPhCS.718f2043M Altcode: SPAN (Spectroscopy of Atomic Neutrino) project aims to determine the absolute neutrino mass. The process we plan to use is a cooperative de-excitation of atoms in a metastable level emitting a neutrino pair associated with a photon. The photon energy spectrum of this process contains information on the absolute mass of neutrino. Key items of this experiment are a rate amplification using macro-coherence in a target medium in case of plural particles emission and an external triggering of the emission in order to scan the spectrum. We have demonstrated the rate amplification in two-photon emission from para-hydrogen gas which was coherently excited to its first vibrationally excited state. The coherence in the medium was generated by irradiating two driving laser pulses. The emission was stimulated by irradiating a mid-infrared laser pulse. The enhancement factor of more than 1018 with respect to the spontaneous emission was achieved. This paper briefly summarizes the results. Title: Spectro-polarimetric observation in UV with CLASP to probe the chromosphere and transition region Authors: Kano, Ryouhei; Ishikawa, Ryohko; Winebarger, Amy R.; Auchère, Frédéric; Trujillo Bueno, Javier; Narukage, Noriyuki; Kobayashi, Ken; Bando, Takamasa; Katsukawa, Yukio; Kubo, Masahito; Ishikawa, Shin-Nosuke; Giono, Gabriel; Hara, Hirohisa; Suematsu, Yoshinori; Shimizu, Toshifumi; Sakao, Taro; Tsuneta, Saku; Ichimoto, Kiyoshi; Goto, Motoshi; Cirtain, Jonathan W.; De Pontieu, Bart; Casini, Roberto; Manso Sainz, Rafael; Asensio Ramos, Andres; Stepan, Jiri; Belluzzi, Luca; Carlsson, Mats Bibcode: 2016SPD....4710107K Altcode: The Chromospheric Lyman-Alpha Spectro-Polarimeter (CLASP) is a NASA sounding-rocket experiment that was performed in White Sands in the US on September 3, 2015. During its 5-minute ballistic flight, CLASP successfully made the first spectro-polarimetric observation in the Lyman-alpha line (121.57 nm) originating in the chromosphere and transition region. Since the Lyman-alpha polarization is sensitive to magnetic field of 10-100 G by the Hanle effect, we aim to infer the magnetic field information in such upper solar atmosphere with this experiment.The obtained CLASP data showed that the Lyman-alpha scattering polarization is about a few percent in the wings and the order of 0.1% in the core near the solar limb, as it had been theoretically predicted, and that both polarization signals have a conspicuous spatio-temporal variability. CLASP also observed another upper-chromospheric line, Si III (120.65 nm), whose critical field strength for the Hanle effect is 290 G, and showed a measurable scattering polarization of a few % in this line. The polarization properties of the Si III line could facilitate the interpretation of the scattering polarization observed in the Lyman-alpha line.In this presentation, we would like to show how the upper chromosphere and transition region are seen in the polarization of these UV lines and discuss the possible source of these complicated polarization signals. 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: Doppler Shift of the Quiet Region Measured by Meridional Scans with the EUV Imaging Spectrometer on board Hinode Authors: Kitagawa, N.; Hara, H.; Yokoyama, T. Bibcode: 2016ApJ...816...14K Altcode: 2015arXiv151105213K Spatially averaged (> 50") EUV spectral lines in the transition region of solar quiet regions are known to be redshifted. Because the mechanism underlying this phenomenon is unclear, we require additional physical information on the lower corona in order to limit the theoretical models. To acquire this information, we measured the Doppler shifts over a wide coronal temperature range ({log}T[{{K}}]=5.7-6.3) using the spectroscopic data taken by the Hinode EUV Imaging Spectrometer. By analyzing the data over the center-to-limb variations covering the meridian from the south to the north pole, we successfully measured the velocity to an accuracy of 3 {{km}} {{{s}}}-1. Below {log}T [{{K}}]=6.0, the Doppler shifts of the emission lines were almost zero with an error of 1-3 {{km}} {{{s}}}-1; above this temperature, they were blueshifted with a gradually increasing magnitude, reaching -6.3+/- 2.1 {{km}} {{{s}}}-1 at {log}T [{{K}}]=6.25. Title: A Study of the Coronal Non-thermal Velocity in Polar Regions During the Rise from Solar Minimum to Solar Maximum in Cycle 24 Authors: Harra, L.; Baker, D.; Edwards, S. J.; Hara, H.; Howe, R.; van Driel-Gesztelyi, L. Bibcode: 2015SoPh..290.3203H Altcode: 2015SoPh..tmp....8H We explore the changes in coronal non-thermal velocity (Vnt) measurements at the poles from solar minimum to solar maximum using Hinode EUV Imaging Spectrometer data. We find that although the intensity in the corona at the poles does tend to increase with the cycle, there are no significant changes in the Vnt values. The locations of enhanced Vnt values measured do not always have a counterpart in intensity, and they are sometimes located in weak emission regions. Unipolar magnetic streams, created through diffusion of the following polarity of the decaying active regions, slowly progress towards the poles. These streams are expected to be related to magnetic nulls as locations that indicate an increased likelihood for magnetic reconnection to occur. Through global potential field source-surface modelling, we determine how the number of nulls varied during the cycle and find that those that lie at < 1.1 solar radii vary significantly. We search for a correlation between the variation of the magnetic nulls and the Vnt values, as it may be expected that with an increasing number of nulls, the Vnt values in the corona increase as well. There is no correlation with the Vnt values, however. This indicates that the magnetic structures that create the enhanced Vnt behaviour are small-scale features and hence not easily measurable at the poles. Because they do not change during the solar cycle, they are likely to be created by a local dynamo. The variation of the upper range of Vnt is reduced, which highlights that strongly dynamic behaviour is reduced as the solar maximum approaches. This is likely to be due to the reduced area of the polar coronal hole, which allows fewer opportunities for reconnection to occur between open and closed magnetic fields. Title: CLASP: A UV Spectropolarimeter on a Sounding Rocket for Probing theChromosphere-Corona Transition Regio Authors: Ishikawa, Ryohko; Kano, Ryouhei; Winebarger, Amy; Auchere, Frederic; Trujillo Bueno, Javier; Bando, Takamasa; Narukage, Noriyuki; Kobayashi, Ken; Katsukawa, Yukio; Kubo, Masahito; Ishikawa, Shin-nosuke; Giono, Gabriel; Tsuneta, Saku; Hara, Hirohisa; Suematsu, Yoshinori; Shimizu, Toshifumi; Sakao, Taro; Ichimoto, Kiyoshi; Cirtain, Jonathan; De Pontieu, Bart; Casini, Roberto; Manso Sainz, Rafael; Asensio Ramos, Andres; Stepan, Jiri; Belluzzi, Luca Bibcode: 2015IAUGA..2254536I Altcode: The wish to understand the energetic phenomena of the outer solar atmosphere makes it increasingly important to achieve quantitative information on the magnetic field in the chromosphere-corona transition region. To this end, we need to measure and model the linear polarization produced by scattering processes and the Hanle effect in strong UV resonance lines, such as the hydrogen Lyman-alpha line. A team consisting of Japan, USA, Spain, France, and Norway has been developing a sounding rocket experiment called the Chromospheric Lyman-alpha Spectro-Polarimeter (CLASP). The aim is to detect the scattering polarization produced by anisotropic radiation pumping in the hydrogen Lyman-alpha line (121.6 nm), and via the Hanle effect to try to constrain the magnetic field vector in the upper chromosphere and transition region. In this talk, we will present an overview of our CLASP mission, its scientific objectives, ground tests made, and the latest information on the launch planned for the Summer of 2015. Title: Precision VUV Spectro-Polarimetry for Solar Chromospheric Magnetic Field Measurements Authors: Ishikawa, R.; Bando, T.; Hara, H.; Ishikawa, S.; Kano, R.; Kubo, M.; Katsukawa, Y.; Kobiki, T.; Narukage, N.; Suematsu, Y.; Tsuneta, S.; Aoki, K.; Miyagawa, K.; Ichimoto, K.; Kobayashi, K.; Auchère, F.; Clasp Team Bibcode: 2014ASPC..489..319I Altcode: The Chromospheric Lyman-Alpha Spectro-Polarimeter (CLASP) is a VUV spectro-polarimeter optimized for measuring the linear polarization of the Lyman-α line (121.6 nm) to be launched in 2015 with NASA's sounding rocket (Ishikawa et al. 2011; Narukage et al. 2011; Kano et al. 2012; Kobayashi et al. 2012). With this experiment, we aim to (1) observe the scattering polarization in the Lyman-α line, (2) detect the Hanle effect, and (3) assess the magnetic fields in the upper chromosphere and transition region for the first time. The polarization measurement error consists of scale error δ a (error in amplitude of linear polarization), azimuth error Δφ (error in the direction of linear polarization), and spurious polarization ɛ (false linear polarization signals). The error ɛ should be suppressed below 0.1% in the Lyman-α core (121.567 nm ±0.02 nm), and 0.5% in the Lyman-α wing (121.567 nm ±0.05 nm), based on our scientific requirements shown in Table 2 of Kubo et al. (2014). From scientific justification, we adopt Δ φ<2° and δ a<10% as the instrument requirements. The spectro-polarimeter features a continuously rotating MgF2 waveplate (Ishikawa et al. 2013), a dual-beam spectrograph with a spherical grating working also as a beam splitter, and two polarization analyzers (Bridou et al. 2011), which are mounted at 90 degree from each other to measure two orthogonal polarization simultaneously. For the optical layout of the CLASP instrument, see Figure 3 in Kubo et al. (2014). Considering the continuous rotation of the half-waveplate, the modulation efficiency is 0.64 both for Stokes Q and U. All the raw data are returned and demodulation (successive addition or subtraction of images) is done on the ground. We control the CLASP polarization performance in the following three steps. First, we evaluate the throughput and polarization properties of each optical component in the Lyman-α line, using the Ultraviolet Synchrotron ORbital Radiation Facility (UVSOR) at the Institute for Molecular Science. The second step is polarization calibration of the spectro-polarimeter after alignment. Since the spurious polarization caused by the axisymmetric telescope is estimated to be negligibly small because of the symmetry (Ishikawa et al. 2014), we do not perform end-to-end polarization calibration. As the final step, before the scientific observation near the limb, we make a short observation at the Sun center and verify the polarization sensitivity, because the scattering polarization is expected to be close to zero at the Sun center due to symmetric geometry. In order to clarify whether we will be able to achieve the required polarization sensitivity and accuracy via these steps, we exercise polarization error budget, by investigating all the possible causes and their magnitudes of polarization errors, all of which are not necessarily verified by the polarization calibration. Based on these error budgets, we conclude that a polarization sensitivity of 0.1% in the line core, δ a<10% and Δ φ<2° can be achieved combined with the polarization calibration of the spectro-polarimeter and the onboard calibration at the Sun center(refer to Ishikawa et al. 2014, for the detail). We are currently conducting verification tests of the flight components and development of the UV light source for the polarization calibration. From 2014 spring, we will begin the integration, alignment, and calibration. We will update the error budgets throughout the course of these tests. Title: A Sounding Rocket Experiment for the Chromospheric Lyman-Alpha Spectro-Polarimeter (CLASP) Authors: Kubo, M.; Kano, R.; Kobayashi, K.; Bando, T.; Narukage, N.; Ishikawa, R.; Tsuneta, S.; Katsukawa, Y.; Ishikawa, S.; Suematsu, Y.; Hara, H.; Shimizu, T.; Sakao, T.; Ichimoto, K.; Goto, M.; Holloway, T.; Winebarger, A.; Cirtain, J.; De Pontieu, B.; Casini, R.; Auchère, F.; Trujillo Bueno, J.; Manso Sainz, R.; Belluzzi, L.; Asensio Ramos, A.; Štěpán, J.; Carlsson, M. Bibcode: 2014ASPC..489..307K Altcode: A sounding-rocket experiment called the Chromospheric Lyman-Alpha Spectro-Polarimeter (CLASP) is presently under development to measure the linear polarization profiles in the hydrogen Lyman-alpha (Lyα) line at 121.567 nm. CLASP is a vacuum-UV (VUV) spectropolarimeter to aim for first detection of the linear polarizations caused by scattering processes and the Hanle effect in the Lyα line with high accuracy (0.1%). This is a fist step for exploration of magnetic fields in the upper chromosphere and transition region of the Sun. Accurate measurements of the linear polarization signals caused by scattering processes and the Hanle effect in strong UV lines like Lyα are essential to explore with future solar telescopes the strength and structures of the magnetic field in the upper chromosphere and transition region of the Sun. The CLASP proposal has been accepted by NASA in 2012, and the flight is planned in 2015. Title: Large aperture solar optical telescope and instruments for the SOLAR-C mission Authors: Suematsu, Y.; Katsukawa, Y.; Hara, H.; Kano, R.; Shimizu, T.; Ichimoto, K. Bibcode: 2014SPIE.9143E..1PS Altcode: A large aperture solar optical telescope and its instruments for the SOLAR-C mission are under study to provide the critical physical parameters in the lower solar atmosphere and to resolve the mechanism of magnetic dynamic events happening there and in the upper atmosphere as well. For the precise magnetic field measurements and high angular resolution in wide wavelength region, covering FOV of 3 arcmin x3 arcmin, an entrance aperture of 1.4 m Gregorian telescope is proposed. Filtergraphs are designed to realize high resolution imaging and pseudo 2D spectro-polarimetry in several magnetic sensitive lines of both photosphere and chromosphere. A full stokes polarimetry is carried out at three magnetic sensitive lines with a four-slit spectrograph of 2D image scanning mechanism. We present a progress in optical and structural design of SOLAR-C large aperture optical telescope and its observing instruments which fulfill science requirements. Title: Development of a universal tunable filter for future solar observations Authors: Hagino, M.; Ichimoto, K.; Kimura, G.; Nakatani, Y.; Kawate, T.; Shinoda, K.; Suematsu, Y.; Hara, H.; Shimizu, T. Bibcode: 2014SPIE.9151E..5VH Altcode: We have developed a new narrowband tunable filter to perform imaging spectroscopy of the solar chromosphere. Using Liquid Crystal Variable Retarders (LCVRs) as the tuning elements for wavelength, wide-band polarizers and super achromatic half-wave plates, it is possible to make high speed tuning (about 0.1Sec), to exclude mechanical drives (and oil tank), and to cover a wide wavelength range (510-100nm). This filter builds up with seven stages each consisting of a pair of calcites, LCVR, half-wave plates and linear polarizer. The full width at half maximum (FWHM) of the filter transmission is about 0.025nm at 656.3nm.We demonstrate that the concept of the universal tunable filter using the LCVR's as tuning elements is highly promising for future application to space mission and ground based observations. Title: New developments in rotating and linear motion mechanisms used in contamination sensitive space telescopes Authors: Shimizu, Toshifumi; Watanabe, Kyoko; Nakayama, Satoshi; Tajima, Takao; Obara, Shingo; Imada, Shinsuke; Nishizuka, Naoto; Ishikawa, Shin-nosuke; Hara, Hirohisa Bibcode: 2014SPIE.9151E..38S Altcode: We have been developing a rotating mechanism and a linear motion mechanism for their usage in contamination sensitive space telescopes. They both are needed for ~1.4 meter optical telescope and its focal plane instrument onboard SOLAR-C, the next-generation spaceborne solar observatory following Hinode. Highly reliable long life performance, low outgassing properties, and low level of micro-vibration are required along with their scientific performance. With the proto-type mechanisms, the long life performance and outgassing properties of the mechanisms have been evaluated in vacuum chambers. The level of micro-vibration excited during the operations of the rotating mechanism was measured by operating it on the Kestler table. This paper provides the overall descriptions of our mechanism developments. Title: RHESSI and EIS observations of an above-the-looptop reconnection region Authors: Glesener, Lindsay; Hara, Hirohisa; Krucker, Sam Bibcode: 2014AAS...22410406G Altcode: A variety of solar flare observations suggest particle acceleration in the corona, at or above the flare looptop. Hard X-ray (HXR) studies, for example, occasionally reveal accelerated electrons above flare looptops, in some cases suggesting the location of the acceleration region. However, since coronal HXR sources are faint and the structure of the flare as seen in extreme ultraviolet (EUV) images is complicated, it is difficult to say where these sources lie with respect to, for example, the reconnection region.HXR and EUV observations can provide complementary information for investigating this topic. EUV imaging spectroscopy reveals bulk flows and locations of line-broadened (potentially turbulent) sources. Such observations can, for example, identify outflows from the reconnection region. HXR imaging places the flare-accelerated electrons in the context of the overall flare geometry, allowing comparison of the locations of accelerated electrons, the reconnection region, and the flare loop.In this work, data from RHESSI and Hinode/EIS are used to investigate above-the-looptop sources in the 2013 May 15 X-class flare. Above-the-looptop EIS flows and loop-top line-broadening are compared with RHESSI HXR sources in the preimpulsive phase of the flare. Title: The SOLAR-C Mission Authors: Hara, Hirohisa Bibcode: 2014cosp...40E1153H Altcode: The SOLAR-C is a planned satellite mission that is led by the JAXA SOLAR-C working group as the 4th Japanese space solar observatory that follows the 3rd satellite mission, Hinode. Hinode equips three major science payloads to cover from the photosphere to the corona simultaneously and has revealed the ubiquitous emergence/submergence of small-scale bipolar fields and the formation of kilo Gauss magnetic flux tubes from vector magnetic field measurements on the photosphere, unexpected dynamical phenomena in the chromosphere, spectral signatures of small-scale coronal heating events near the chromosphere below its spatial resolution, and so forth. These are the universal magnetized plasma activity in the nearest star, and the essential energy source of the phenomena is of magnetic-field origin coupled with photospheric convective motion. To elucidate the newly-found solar active phenomena and the problems that have been tackled for a long time in solar physics, we try to understand the causal linkage between solar magnetic fields and active phenomena on the Sun in the true sense by high-resolution (0.1-0.3 arcsecs) instruments in space. SOLAR-C will observe photospheric and chromospheric activity by imaging and measure chromospheric magnetic fields by spectropolarimetry, in addition to photospheric magnetic fields. It visualizes the site of dynamical events for chromospheric and coronal heating by imaging and spectroscopy with comparable resolution and by high-resolution chromospheric magnetometry. In addition, SOLAR-C essentially contributes to space weather by estimating the stored magnetic energy in the corona via measurements of chromospheric magnetic fields. The coming sounding-rocket program CLASP and the further satellite mission SOLAR-D that may follow the SOLAR-C mission are also briefly mentioned. Title: Velocity structure of solar flare plasmas Authors: Watanabe, Tetsuya; Watanabe, Kyoko; Hara, Hirohisa; Imada, Shinsuke Bibcode: 2014cosp...40E3606W Altcode: Thanks to its increased sensitivity and spectral resolution, EIS enabled emission line profile analysis for the first time in solar EUV spectroscopy, and it found detailed structures in velocity and temperature in solar flares. A widely accepted model for solar flares incorporates magnetic reconnection in the corona which results in local heating as well as acceleration of nonthermal particle beams. The standard model of solar flares is called the CSHKP model, arranging the initials of model proposers. We find loop-top hot source, fast outflows nearby, inflow structure flowing to the hot source that appeared in the impulsive phase of long-duration eruptive flares. From the geometrical relationships of these phenomena, we conclude that they provide evidence for magnetic reconnection that occurs near the loop-top region. The reconnection rate is estimated to 0.05 - 0.1, which supports the Petschek-type magnetic reconnection. The nonthermal particle beams will travel unimpeded until they reach the cold, dense chromosphere, where the energy of the beam is predominantly used to heat the chromosphere at the foot points of flaring loops. Explosive chromospheric evaporation happens when the beam energy is high enough that the chromosphere cannot radiate away energy fast enough and hence expands at high velocities into the corona. Spatially resolved observations of chromopheric evaporation during the initial phases of impulsive flares, a few bright points of Fexxiii and Fexxiv emission lines at the footpoints of flaring loops present dominated blue-shifted components of 300 - 400 kms (-1) , while Fexv/xvi lines are nearly stationary, and Feviii and Sivii lines present +50 kms (-1) red shifts. We will review these new views on dynamical structure in flares. Title: Spectroscopy of Reconnection Inflow and Outflow in Solar Flares Authors: Hara, Hirohisa Bibcode: 2014cosp...40E1154H Altcode: We report reconnection inflow and outflow structures in a type of solar flares that were observed by spectroscopic observations with the Hinode EUV Imaging Spectrometer. A dark outflow has been found by EIS raster scan observations in hot emission lines like Fe XXIII and Fe XXIV as a structure extended from a site above a bright flare loop. The outflow structure is heated to ~10 MK, and the electron density of the outflow is enhanced by about a factor of 2 from the surrounding corona. The hot emission lines in the outflow structure show a large excess width, which may imply the presence of an internal flow structure or the plasma in a turbulent state. A high-density blob structure that appears above the loop-top region where the reconnection outflow collides shows the Doppler motion toward the low-altitude direction. The reconnection rate is estimated to be 0.01-0.1 in combination with the signature of reconnection inflow from the Doppler velocity measurement. Title: UV spectropolarimeter design for precise polarization measurement and its application to the CLASP for exploration of magnetic fields in solar atmosphere Authors: Narukage, Noriyuki; Katsukawa, Yukio; Hara, Hirohisa; Kubo, Masahito; Auchere, Frederic; Ishikawa, Ryohko; Kano, Ryouhei; Bando, Takamasa; Ishikawa, Shin-nosuke; Suematsu, Yoshinori; Tsuneta, Saku Bibcode: 2014cosp...40E2232N Altcode: In order to measure the magnetic field in the region where the hot plasma from 10 (4) K to 10 (6) K is occupied, e.g., for solar atmosphere, the polarimetric measurements in ultra violet (UV) with 0.1% accuracy are required. In this paper, we propose a new UV spectropolarimeter design with 0.1% sensitivity in polarization measurement. This spectropolarimeter has two devices for the 0.1% accuracy. First, all optical components except the waveplate are the reflective type ones that can be equipped with the high reflectivity coating for the high throughput. Secondly, it equips the optically symmetric dual channels to measure the orthogonal linear polarization state simultaneously, using a concave diffraction grating as both the spectral dispersion element and the beam splitter. These two devices make the spurious polarizations caused by the photon noise, by the intensity variation of the observation target, and, by the instrument itself, enough small to achieve the 0.1% accuracy in polarization measurement. The spectropolarimeter thus designed is currently under fabrication for the sounding rocket project of Chromospheric Lyman-Alpha SpectroPolarimeter (CLASP) that aims at the direct measurement of the magnetic fields in solar atmosphere with Lyman-alpha line (121.6 nm) for the first time. Title: Hot Plasma Associated with a Coronal Mass Ejection Authors: Landi, E.; Miralles, M. P.; Raymond, J. C.; Hara, H. Bibcode: 2013ApJ...778...29L Altcode: We analyze coordinated observations from the EUV Imaging Spectrometer (EIS) and X-Ray Telescope (XRT) on board Hinode of an X-ray Plasma Ejection (XPE) that occurred during the coronal mass ejection (CME) event of 2008 April 9. The XPE was trailing the CME core from behind, following the same trajectory, and could be identified both in EIS and XRT observations. Using the EIS spectrometer, we have determined the XPE plasma parameters, measuring the electron density, thermal distribution, and elemental composition. We have found that the XPE composition and electron density were very similar to those of the pre-event active region plasma. The XPE temperature was higher, and its thermal distribution peaked at around 3 MK also, typical flare lines were absent from EIS spectra, indicating that any XPE component with temperatures in excess of 5 MK was likely either faint or absent. We used XRT data to investigate the presence of hotter plasma components in the XPE that could have gone undetected by EIS and found that—if at all present—these components have small emission measure values and their temperature is in the 8-12.5 MK range. The very hot plasma found in earlier XPE observations obtained by Yohkoh seems to be largely absent in this CME, although plasma ionization timescales may lead to non-equilibrium ionization effects that could make bright lines from ions formed in a 10 MK plasma not detectable by EIS. Our results supersede the XPE findings of Landi et al., who studied the same event with older response functions for the XRT Al-poly filter; the differences in the results stress the importance of using accurate filter response functions. Title: Evidence for Hot Fast Flow above a Solar Flare Arcade Authors: Imada, S.; Aoki, K.; Hara, H.; Watanabe, T.; Harra, L. K.; Shimizu, T. Bibcode: 2013ApJ...776L..11I Altcode: 2013arXiv1309.3401I Solar flares are one of the main forces behind space weather events. However, the mechanism that drives such energetic phenomena is not fully understood. The standard eruptive flare model predicts that magnetic reconnection occurs high in the corona where hot fast flows are created. Some imaging or spectroscopic observations have indicated the presence of these hot fast flows, but there have been no spectroscopic scanning observations to date to measure the two-dimensional structure quantitatively. We analyzed a flare that occurred on the west solar limb on 2012 January 27 observed by the Hinode EUV Imaging Spectrometer (EIS) and found that the hot (~30MK) fast (>500 km s-1) component was located above the flare loop. This is consistent with magnetic reconnection taking place above the flare loop. Title: The Location of Non-thermal Velocity in the Early Phases of Large Flares—Revealing Pre-eruption Flux Ropes Authors: Harra, Louise K.; Matthews, Sarah; Culhane, J. L.; Cheung, Mark C. M.; Kontar, Eduard P.; Hara, Hirohisa Bibcode: 2013ApJ...774..122H Altcode: Non-thermal velocity measurements of the solar atmosphere, particularly from UV and X-ray emission lines have demonstrated over the decades that this parameter is important in understanding the triggering of solar flares. Enhancements have often been observed before intensity enhancements are seen. However, until the launch of Hinode, it has been difficult to determine the spatial location of the enhancements to better understand the source region. The Hinode EUV Imaging Spectrometer has the spectral and spatial resolution to allow us to probe the early stages of flares in detail. We analyze four events, all of which are GOES M- or X-classification flares, and all are located toward the limb for ease of flare geometry interpretation. Three of the flares were eruptive and one was confined. In all events, pre-flare enhancement in non-thermal velocity at the base of the active region and its surroundings has been found. These enhancements seem to be consistent with the footpoints of the dimming regions, and hence may be highlighting the activation of a coronal flux rope for the three eruptive events. In addition, pre-flare enhancements in non-thermal velocity were found above the looptops for the three eruptive events. Title: Chromospheric Lyman Alpha SpectroPolarimeter: CLASP Authors: Kobayashi, Ken; Kano, R.; Trujillo Bueno, J.; Winebarger, A. R.; Cirtain, J. W.; Bando, T.; De Pontieu, B.; Ishikawa, R.; Katsukawa, Y.; Kubo, M.; Narukage, N.; Sakao, T.; Tsuneta, S.; Auchère, F.; Asensio Ramos, A.; Belluzzi, L.; Carlsson, M.; Casini, R.; Hara, H.; Ichimoto, K.; Manso Sainz, R.; Shimizu, T.; Stepan, J.; Suematsu, Y.; Holloway, T. Bibcode: 2013SPD....44..142K Altcode: The Chromospheric Lyman-Alpha Spectro-Polarimeter (CLASP) is a VUV spectropolarimeter optimized for measuring the linear polarization of the Lyman-alpha line (121.6 nm). The Lyman-alpha line is predicted to show linear polarization caused by atomic scattering in the chromosphere and modified by the magnetic field through the Hanle effect. The Hanle effect is sensitive to weaker magnetic fields than Zeeman effect, and is not canceled by opposing fields, making it sensitive to tangled or unresolved magnetic field structures. These factors make the Hanle effect a valuable tool for probing the magnetic field in the chromosphere above the quiet sun. To meet this goal, CLASP is designed to measure linear polarization with 0.1% polarization sensitivity at 0.01 nm spectral resolution and 10" spatial resolution. CLASP is scheduled to be launched in 2015. Title: Properties of a Solar Flare Kernel Observed by Hinode and SDO Authors: Young, P. R.; Doschek, G. A.; Warren, H. P.; Hara, H. Bibcode: 2013ApJ...766..127Y Altcode: 2012arXiv1212.4388Y Flare kernels are compact features located in the solar chromosphere that are the sites of rapid heating and plasma upflow during the rise phase of flares. An example is presented from a M1.1 class flare in active region AR 11158 observed on 2011 February 16 07:44 UT for which the location of the upflow region seen by EUV Imaging Spectrometer (EIS) can be precisely aligned to high spatial resolution images obtained by the Atmospheric Imaging Assembly (AIA) and Helioseismic and Magnetic Imager (HMI) on board the Solar Dynamics Observatory (SDO). A string of bright flare kernels is found to be aligned with a ridge of strong magnetic field, and one kernel site is highlighted for which an upflow speed of ≈400 km s-1 is measured in lines formed at 10-30 MK. The line-of-sight magnetic field strength at this location is ≈1000 G. Emission over a continuous range of temperatures down to the chromosphere is found, and the kernels have a similar morphology at all temperatures and are spatially coincident with sizes at the resolution limit of the AIA instrument (lsim400 km). For temperatures of 0.3-3.0 MK the EIS emission lines show multiple velocity components, with the dominant component becoming more blueshifted with temperature from a redshift of 35 km s-1 at 0.3 MK to a blueshift of 60 km s-1 at 3.0 MK. Emission lines from 1.5-3.0 MK show a weak redshifted component at around 60-70 km s-1 implying multi-directional flows at the kernel site. Significant non-thermal broadening corresponding to velocities of ≈120 km s-1 is found at 10-30 MK, and the electron density in the kernel, measured at 2 MK, is 3.4 × 1010 cm-3. Finally, the Fe XXIV λ192.03/λ255.11 ratio suggests that the EIS calibration has changed since launch, with the long wavelength channel less sensitive than the short wavelength channel by around a factor two. Title: SDO and Hinode observations of coronal heating at a flare kernel site Authors: Young, P. R.; Doschek, G. A.; Warren, H. P.; Hara, H. Bibcode: 2013enss.confE..36Y Altcode: Flare kernels are compact features located in the chromosphere that are the sites of rapid heating and plasma upflow during the rise phase of flares. They provide an excellent opportunity for testing models of energy transport and dissipation in the solar atmosphere as they are very bright and emit over a wide temperature range. A M1.1 class flare that peaked at 07:44 UT on 2011 February 16 was observed simultaneously by SDO and Hinode, and one flare kernel observed prior to the flare peak is highlighted. It is found to emit at all temperatures from the chromosphere through to 30 MK, with all AIA channels brightening simultaneously and rise times of only 1 minute. The kernel is located on a ridge of strong magnetic field close to a neutral line in the active region. The kernel is at the resolution limit of AIA, suggesting a size of < 0.6 arcsec. Hinode/EIS allows velocity patterns in the kernel to be tracked over a wide temperature range and reveals a dominant high speed upflow of 400 km/s at temperatures of 10-30 MK, with both down and upflows measured at cooler temperatures of 1.5-3.0 MK, suggesting unresolved structures. All emission lines show evidence of significant non-thermal broadening, and the electron density of the plasma is 3.4 x 10^10 cm-3. The observations are compared to models of chromospheric evaporation and similarities and differences are highlighted. Title: Observations from SDO, Hinode, and STEREO of a Twisting and Writhing Start to a Solar-filament-eruption Cascade Authors: Sterling, Alphonse C.; Moore, Ronald L.; Hara, Hirohisa Bibcode: 2012ApJ...761...69S Altcode: We analyze data from SDO (AIA, HMI), Hinode (SOT, XRT, EIS), and STEREO (EUVI) of a solar eruption sequence of 2011 June 1 near 16:00 UT, with an emphasis on the early evolution toward eruption. Ultimately, the sequence consisted of three emission bursts and two filament ejections. SDO/AIA 304 Å images show absorbing-material strands initially in close proximity which over ~20 minutes form a twisted structure, presumably a flux rope with ~1029 erg of free energy that triggers the resulting evolution. A jump in the filament/flux rope's displacement (average velocity ~20 km s-1) and the first burst of emission accompanies the flux-rope formation. After ~20 more minutes, the flux rope/filament kinks and writhes, followed by a semi-steady state where the flux rope/filament rises at (~5 km s-1) for ~10 minutes. Then the writhed flux rope/filament again becomes MHD unstable and violently erupts, along with rapid (50 km s-1) ejection of the filament and the second burst of emission. That ejection removed a field that had been restraining a second filament, which subsequently erupts as the second filament ejection accompanied by the third (final) burst of emission. Magnetograms from SDO/HMI and Hinode/SOT, and other data, reveal several possible causes for initiating the flux-rope-building reconnection, but we are not able to say which is dominant. Our observations are consistent with magnetic reconnection initiating the first burst and the flux-rope formation, with MHD processes initiating the further dynamics. Both filament ejections are consistent with the standard model for solar eruptions. Title: Next space solar observatory SOLAR-C: mission instruments and science objectives Authors: Katsukawa, Y.; Watanabe, T.; Hara, H.; Ichimoto, K.; Kubo, M.; Kusano, K.; Sakao, T.; Shimizu, T.; Suematsu, Y.; Tsuneta, S. Bibcode: 2012IAUSS...6E.207K Altcode: SOLAR-C, the fourth space solar mission in Japan, is under study with a launch target of fiscal year 2018. A key concept of the mission is to view the photosphere, chromosphere, and corona as one system coupled by magnetic fields along with resolving the size scale of fundamental physical processes connecting these atmospheric layers. It is especially important to study magnetic structure in the chromosphere as an interface layer between the photosphere and the corona. The SOLAR-C satellite is equipped with three telescopes, the Solar UV-Visible-IR Telescope (SUVIT), the EUV/FUV High Throughput Spectroscopic Telescope (EUVS/LEMUR), and the X-ray Imaging Telescope (XIT). Observations with SUVIT of photospheric and chromospheric magnetic fields make it possible to infer three dimensional magnetic structure extending from the photosphere to the chromosphere and corona.This helps to identify magnetic structures causing magnetic reconnection, and clarify how waves are propagated, reflected, and dissipated. Phenomena indicative of or byproducts of magnetic reconnection, such as flows and shocks, are to be captured by SUVIT and by spectroscopic observations using EUVS/LEMUR, while XIT observes rapid changes in temperature distribution of plasma heated by shock waves. Title: Production of High-Temperature Plasmas During the Early Phases of a C9.7 Flare. II. Bi-directional Flows Suggestive of Reconnection in a Pre-flare Brightening Region Authors: Watanabe, T.; Hara, H.; Sterling, A. C.; Harra, L. K. Bibcode: 2012SoPh..281...87W Altcode: 2012SoPh..tmp..185W The 6 June 2007 16:55 UT flare was well observed with high time-cadence sparse raster scans by the EUV Imaging Spectrometer (EIS) on board the Hinode spacecraft. The observation covers an active region area of 240 arcsec × 240 arcsec with the 1 arcsec slit in about 160 seconds. Title: Design of large aperture solar optical telescope for the SOLAR-C mission Authors: Suematsu, Y.; Katsukawa, Y.; Hara, H.; Shimizu, T.; Ichimoto, K. Bibcode: 2012SPIE.8442E..25S Altcode: A large aperture optical telescope is planned for the next Japanese solar mission SOLAR-C as one of major three observing instruments. The optical telescope is designed to provide high-angular-resolution investigation of lower atmosphere from the photosphere to the uppermost chromosphere with enhanced spectroscopic and spectro-polarimetric capability covering a wide wavelength region from 280 nm to 1100 nm. The opto-mechanical and -thermal performance of the telescope is crucial to attain high-quality solar observations and we present a study of optical and structural design of the large aperture space solar telescope, together with conceptual design of its accompanying focal plane instruments: wide-band and narrow-band filtergraphs and a spectro-polarimeter for high spatial and temporal observations in the solar photospheric and chromospheric lines useful for sounding physical condition of dynamical phenomena. Title: Chromospheric Lyman-alpha spectro-polarimeter (CLASP) Authors: Kano, Ryouhei; Bando, Takamasa; Narukage, Noriyuki; Ishikawa, Ryoko; Tsuneta, Saku; Katsukawa, Yukio; Kubo, Masahito; Ishikawa, Shin-nosuke; Hara, Hirohisa; Shimizu, Toshifumi; Suematsu, Yoshinori; Ichimoto, Kiyoshi; Sakao, Taro; Goto, Motoshi; Kato, Yoshiaki; Imada, Shinsuke; Kobayashi, Ken; Holloway, Todd; Winebarger, Amy; Cirtain, Jonathan; De Pontieu, Bart; Casini, Roberto; Trujillo Bueno, Javier; Štepán, Jiří; Manso Sainz, Rafael; Belluzzi, Luca; Asensio Ramos, Andres; Auchère, Frédéric; Carlsson, Mats Bibcode: 2012SPIE.8443E..4FK Altcode: One of the biggest challenges in heliophysics is to decipher the magnetic structure of the solar chromosphere. The importance of measuring the chromospheric magnetic field is due to both the key role the chromosphere plays in energizing and structuring the outer solar atmosphere and the inability of extrapolation of photospheric fields to adequately describe this key boundary region. Over the last few years, significant progress has been made in the spectral line formation of UV lines as well as the MHD modeling of the solar atmosphere. It is found that the Hanle effect in the Lyman-alpha line (121.567 nm) is a most promising diagnostic tool for weaker magnetic fields in the chromosphere and transition region. Based on this groundbreaking research, we propose the Chromospheric Lyman-Alpha Spectro-Polarimeter (CLASP) to NASA as a sounding rocket experiment, for making the first measurement of the linear polarization produced by scattering processes and the Hanle effect in the Lyman-alpha line (121.567 nm), and making the first exploration of the magnetic field in the upper chromosphere and transition region of the Sun. The CLASP instrument consists of a Cassegrain telescope, a rotating 1/2-wave plate, a dual-beam spectrograph assembly with a grating working as a beam splitter, and an identical pair of reflective polarization analyzers each equipped with a CCD camera. We propose to launch CLASP in December 2014. Title: Flare Onset Observed with Hinode in the 2006 December 13 Flare Authors: Asai, A.; Hara, H.; Watanabe, T.; Imada, S. Bibcode: 2012ASPC..454..303A Altcode: We present a detailed examination of the preflare phenomena of the X3.4 flare that occurred on 2006 December 13. This flare was associated with a faint arc-shaped ejection, which is thought to be an MHD fast-mode shock wave, seen in the soft X-ray images taken with the Hinode X-Ray Telescope (XRT), just at the start of the impulsive phase of the flare. Even before the ejection, we found many preflare features, such as an S-shaped brightening (sigmoid) with XRT, chromospheric brightening at the footpoints of the sigmoid loops with the Solar Optical Telescope (SOT), a faint X-ray eruption with XRT, and so on. The EUV Imaging Spectrometer (EIS) also observed the flare, and therefore, enabled us to examine the spectroscopic features. We discuss these phenomena and the energy release prosses. Title: Propagating Slow Magnetoacoustic Waves along the Continuous Outflows Observed with EIS/Hinode Authors: Nishizuka, N.; Matsumoto, T.; Morita, S.; Hara, H.; Shibata, K. Bibcode: 2012ASPC..454..157N Altcode: The high temporal relation data obtained from EIS/Hinode has been analyzed. In the ‘sit-and-stare’ mode observations, we focused on continuous outflows at the edge of the active region NOAA 10942 on 2007 February 20. We found that the Doppler blueshift (∼20-50 km s-1) components, in Fe XII 195 Å emission line, propagating with the continuous plasma outflows from the edge of the active region, with the transverse velocity ranging 140-160 km s-1. This suggests slow magnetoacoustic wave propagation along the open field line. We also found a jet around the active region, whose transverse velocity ∼170 km s-1 and line-of-sight Doppler velocity ∼150 km s-1. Title: The Chromospheric Lyman-Alpha SpectroPolarimeter: CLASP Authors: Kobayashi, K.; Kano, R.; Trujillo-Bueno, J.; Asensio Ramos, A.; Bando, T.; Belluzzi, L.; Carlsson, M.; De Pontieu, R. C. B.; Hara, H.; Ichimoto, K.; Ishikawa, R.; Katsukawa, Y.; Kubo, M.; Manso Sainz, R.; Narukage, N.; Sakao, T.; Stepan, J.; Suematsu, Y.; Tsuneta, S.; Watanabe, H.; Winebarger, A. Bibcode: 2012ASPC..456..233K Altcode: The magnetic field plays a crucial role in the chromosphere and the transition region, and our poor empirical knowledge of the magnetic field in the upper chromosphere and transition region is a major impediment to advancing the understanding of the solar atmosphere. The Hanle effect promises to be a valuable alternative to Zeeman effect as a method of measuring the magnetic field in the chromosphere and transition region; it is sensitive to weaker magnetic fields, and also sensitive to tangled, unresolved field structures. CLASP is a sounding rocket experiment that aims to observe the Hanle effect polarization of the Lyman α (1215.67Å) line in the solar chromosphere and transition region, and prove the usefulness of this technique in placing constraints on the magnetic field strength and orientation in the low plasma-β region of the solar atmosphere. The Ly-α line has been chosen because it is a chromospheric/transition-region line, and because the Hanle effect polarization of this line is predicted to be sensitive to 10-250 Gauss, encompassing the range of interest. The CLASP instrument is designed to measure linear polarization in the Ly-α line with a polarization sensitivity of 0.1%. The instrument is currently funded for development. The optical design of the instrument has been finalized, and an extensive series of component-level tests are underway to validate the design. Title: Post-Coronal Mass Ejection Plasma Observed by Hinode Authors: Landi, E.; Raymond, J. C.; Miralles, M. P.; Hara, H. Bibcode: 2012ApJ...751...21L Altcode: In the present work we study the evolution of an active region after the eruption of a coronal mass ejection (CME) using observations from the EIS and XRT instruments on board Hinode. The field of view includes a post-eruption arcade, a current sheet, and a coronal dimming. The goal of this paper is to provide a comprehensive set of measurements for all these aspects of the CME phenomenon made on the same CME event. The main physical properties of the plasma along the line of sight—electron density, thermal structure, plasma composition, size, and, when possible, mass—are measured and monitored with time for the first three hours following the CME event of 2008 April 9. We find that the loop arcade observed by EIS and XRT may not be related to the post-eruption arcade. Post-CME plasma is hotter than the surrounding corona, but its temperature never exceeds 3 MK. Both the electron density and thermal structure do not show significant evolution with time, while we found that the size of the loop arcade in the Hinode plane of the sky decreased with time. The plasma composition is the same in the current sheet, in the loop arcade, and in the ambient plasma, so all these plasmas are likely of coronal origin. No significant plasma flows were detected. Title: Spectroscopic Observations of Continuous Outflows and Propagating Waves in Active Region NOAA 10942 with Hinode/EIS Authors: Nishizuka, N.; Hara, H. Bibcode: 2012ASPC..455..219N Altcode: We analyze "sit-and-stare" mode observations of continuous outflows and waves with the Extreme ultraviolet Imaging Spectrometer (EIS) on board Hinode, whose slit was located along the open field lines at the edge of active region NOAA 10942 on February 20, 2007. We found both intensity and velocity disturbances in Fe xii 195.12 Å propagating along the field lines with apparent speeds of 140 km s-1. The Doppler shifts shows mean upward velocities of 30-50 km s-1 and small velocity disturbances with amplitudes of 5-15 km s-1 in phase with intensity disturbances of 3-5% amplitude relative to the mean intensity. Not only a quasi-periodicity of 10-13 minutes but also “tad pole'' signatures—which may be evidence of propagating waves—were observed at the footpoints of the loops. Covariation of intensity and Doppler velocity is consistent with upward motion of propagating slow-mode magnetoacoustic waves. The energy flux of the waves was estimated to be 1-3× 105 erg s-1 cm-2, which is not enough to account for coronal heating but sufficient for solar wind acceleration. High temporal spectroscopic observation also revealed intermittent signatures of line broadening at the footpoints of the loops. Each of them seems to correspond to the footpoints of propagating disturbances. This may indicate that the origins of flows and waves are unresolved explosive events at the lower atmosphere, by analogy to spectroscopic observations of a jet. Title: Photosphere-Corona Connection in Active-Region Plage Authors: Hara, H. Bibcode: 2012decs.confE..94H Altcode: We discuss the relationships between the temperature of coronal loops and photospheric magnetic properties at their footpoints in an active-region plage from observations by Hinode. The motion of photospheric magnetic fields is tracked by the correlation tracking of SOT FG Stokes-V maps to estimate the photospheric horizontal velocity. We find that the horizontal velocity is anti-correlated with the filling factor of photospheric magnetic fields estimated from the SOT SP data. It is confirmed from high-resolution observations by Hinode that the footpoints of hot (warm) coronal loops in X-ray (EUV) observations are rooted at low (high) magnetic filing factor regions within the plage. The distribution of energy flux to the corona in the plage is calculated from observations according to a model in Katsukawa & Tsuneta (2005). The distribution appears to explain the footpoint position of hot and warm loops. Title: One-dimensional Modeling for Temperature-dependent Upflow in the Dimming Region Observed by Hinode/EUV Imaging Spectrometer Authors: Imada, S.; Hara, H.; Watanabe, T.; Murakami, I.; Harra, L. K.; Shimizu, T.; Zweibel, E. G. Bibcode: 2011ApJ...743...57I Altcode: 2011arXiv1108.5031I We previously found a temperature-dependent upflow in the dimming region following a coronal mass ejection observed by the Hinode EUV Imaging Spectrometer (EIS). In this paper, we reanalyzed the observations along with previous work on this event and provided boundary conditions for modeling. We found that the intensity in the dimming region dramatically drops within 30 minutes from the flare onset, and the dimming region reaches the equilibrium stage after ~1 hr. The temperature-dependent upflows were observed during the equilibrium stage by EIS. The cross-sectional area of the flux tube in the dimming region does not appear to expand significantly. From the observational constraints, we reconstructed the temperature-dependent upflow by using a new method that considers the mass and momentum conservation law and demonstrated the height variation of plasma conditions in the dimming region. We found that a super-radial expansion of the cross-sectional area is required to satisfy the mass conservation and momentum equations. There is a steep temperature and velocity gradient of around 7 Mm from the solar surface. This result may suggest that the strong heating occurred above 7 Mm from the solar surface in the dimming region. We also showed that the ionization equilibrium assumption in the dimming region is violated, especially in the higher temperature range. Title: The Chromospheric Lyman-Alpha SpectroPolarimeter (CLASP)j Authors: Kobayashi, K.; Tsuneta, S.; Trujillo Bueno, J.; Bando, T.; Belluzzi, L.; Casini, R.; Carlsson, M.; Cirtain, J. W.; De Pontieu, B.; Hara, H.; Ichimoto, K.; Ishikawa, R.; Kano, R.; Katsukawa, Y.; Kim, T.; Kubo, M.; Manso Sainz, R.; Narukage, N.; Asensio Ramos, A.; Robinson, B.; Sakao, T.; Shimizu, T.; Stepan, J.; Suematsu, Y.; Watanabe, H.; West, E.; Winebarger, A. R. Bibcode: 2011AGUFM.P14C..05K Altcode: We present an overview of the Chromospheric Lyman-Alpha SpectroPolarimeter (CLASP) program. CLASP is a proposed sounding rocket experiment currently under development as collaboration between Japan, USA and Spain. The aim is to achieve the first measurement of magnetic field in the upper chromosphere and transition region of the Sun through the detection and measurement of Hanle effect polarization of the Lyman alpha line. The Hanle effect (i.e. the magnetic field induced modification of the linear polarization due to scattering processes in spectral lines) is believed to be a powerful tool for measuring the magnetic field in the upper chromosphere, as it is more sensitive to weaker magnetic fields than the Zeeman effect, and also sensitive to magnetic fields tangled at spatial scales too small to be resolved. The Lyman-alpha (121.567 nm) line has been chosen because it is a chromospheric/transition-region line, and because the Hanle effect polarization of the Lyman-alpha line is predicted to be sensitive to 10-250 Gauss, encompassing the range of interest. Hanle effect is predicted to be observable as linear polarization or depolarization, depending on the geometry, with a fractional polarization amplitude varying between 0.1% and 1% depending on the strength and orientation of the magnetic field. This quantification of the chromospheric magnetic field requires a highly sensitive polarization measurement. The CLASP instrument consists of a large aperture (287 mm) Cassegrain telescope mated to a polarizing beamsplitter and a matched pair of grating spectrographs. The polarizing beamsplitter consists of a continuously rotating waveplate and a linear beamsplitter, allowing simultaneous measurement of orthogonal polarizations and in-flight self-calibration. Development of the instrument is underway, and prototypes of all optical components have been tested using a synchrotron beamline. The experiment is proposed for flight in 2014. Title: Magnetic Reconnection in Non-equilibrium Ionization Plasma Authors: Imada, S.; Murakami, I.; Watanabe, T.; Hara, H.; Shimizu, T. Bibcode: 2011ApJ...742...70I Altcode: 2011arXiv1108.5026I We have studied the effect of time-dependent ionization and the recombination processes on magnetic reconnection in the solar corona. Petschek-type steady reconnection, in which the magnetic energy is mainly converted at the slow-mode shocks, was assumed. We carried out the time-dependent ionization calculation in the magnetic reconnection structure. We only calculated the transient ionization of iron; the other species were assumed to be in ionization equilibrium. The intensity of line emissions at specific wavelengths was also calculated for comparison with Hinode or other observations in future. We found the following: (1) iron is mostly in non-equilibrium ionization in the reconnection region; (2) the intensity of line emission estimated by the time-dependent ionization calculation is significantly different from that determined from the ionization equilibrium assumption; (3) the effect of time-dependent ionization is sensitive to the electron density in the case where the electron density is less than 1010 cm-3 (4) the effect of thermal conduction lessens the time-dependent ionization effect; and (5) the effect of radiative cooling is negligibly small even if we take into account time-dependent ionization. Title: Plasma Motions and Heating by Magnetic Reconnection in a 2007 May 19 Flare Authors: Hara, Hirohisa; Watanabe, Tetsuya; Harra, Louise K.; Culhane, J. Leonard; Young, Peter R. Bibcode: 2011ApJ...741..107H Altcode: Based on scanning spectroscopic observations with the Hinode EUV imaging spectrometer, we have found a loop-top hot source, a fast jet nearby, and an inflow structure flowing to the hot source that appeared in the impulsive phase of a long-duration flare at the disk center on 2007 May 19. The hot source observed in Fe XXIII and Fe XXIV emission lines has the electron temperature of 12 MK and density of 1 × 1010 cm-3. It shows excess line broadening, which exceeds the thermal Doppler width by ~100 km s-1, with a weak redshift of ~30 km s-1. We have also observed a blueshifted faint jet whose Doppler velocity exceeds 200 km s-1 with an electron temperature of 9 MK. Coronal plasmas with electron temperature of 1.2 MK and density of 2.5 × 109 cm-3 that flow into the loop-top region with a Doppler velocity of 20 km s-1 have been identified in the Fe XII observation. They disappeared near the hot source, possibly by being heated to the hotter faint jet temperature. From the geometrical relationships of these phenomena, we conclude that they provide evidence for magnetic reconnection that occurs near the loop-top region. The estimated reconnection rate is 0.05-0.1, which supports the Petschek-type magnetic reconnection. Further supporting evidence for the presence of the slow-mode and fast-mode MHD shocks in the reconnection geometry is given based on the observed quantities. Title: Overview of Chromospheric Lyman-Alpha SpectroPolarimeter (CLASP) Authors: Narukage, Noriyuki; Tsuneta, Saku; Bando, Takamasa; Kano, Ryouhei; Kubo, Masahito; Ishikawa, Ryoko; Hara, Hirohisa; Suematsu, Yoshinori; Katsukawa, Yukio; Watanabe, Hiroko; Ichimoto, Kiyoshi; Sakao, Taro; Shimizu, Toshifumi; Kobayashi, Ken; Robinson, Brian; Kim, Tony; Winebarger, Amy; West, Edward; Cirtain, Jonathan; De Pontieu, Bart; Casini, Roberto; Trujillo Bueno, Javier; Stepan, Jiri; Manso Sainz, Rafael; Belluzzi, Luca; Asensio Ramos, Andres; Carlsson, Mats Bibcode: 2011SPIE.8148E..0HN Altcode: 2011SPIE.8148E..16N The solar chromosphere is an important boundary, through which all of the plasma, magnetic fields and energy in the corona and solar wind are supplied. Since the Zeeman splitting is typically smaller than the Doppler line broadening in the chromosphere and transition region, it is not effective to explore weak magnetic fields. However, this is not the case for the Hanle effect, when we have an instrument with high polarization sensitivity (~ 0.1%). "Chromospheric Lyman- Alpha SpectroPolarimeter (CLASP)" is the sounding rocket experiment to detect linear polarization produced by the Hanle effect in Lyman-alpha line (121.567 nm) and to make the first direct measurement of magnetic fields in the upper chromosphere and lower transition region. To achieve the high sensitivity of ~ 0.1% within a rocket flight (5 minutes) in Lyman-alpha line, which is easily absorbed by materials, we design the optical system mainly with reflections. The CLASP consists of a classical Cassegrain telescope, a polarimeter and a spectrometer. The polarimeter consists of a rotating 1/2-wave plate and two reflecting polarization analyzers. One of the analyzer also works as a polarization beam splitter to give us two orthogonal linear polarizations simultaneously. The CLASP is planned to be launched in 2014 summer. Title: The SOLAR-C mission: current status Authors: Shimizu, Toshifumi; Tsuneta, Saku; Hara, Hirohisa; Ichimoto, Kiyoshi; Kusano, Kanya; Sakao, Taro; Sekii, Takashi; Suematsu, Yoshinori; Watanabe, Tetsuya Bibcode: 2011SPIE.8148E..0BS Altcode: 2011SPIE.8148E..10S Two mission concepts (plan A: out-of-ecliptic mission and plan B: high resolution spectroscopic mission) have been studied for the next Japanese-led solar mission Solar-C, which will follow the scientific success of the Hinode mission. The both mission concepts are concluded as equally important and attractive for the promotion of space solar physics. In the meantime we also had to make efforts for prioritizing the two options, in order to proceed to next stage of requesting the launch of Solar-C mission at the earliest opportunity. This paper briefly describes the two mission concepts and the current status on our efforts for prioritizing the two options. More details are also described for the plan B option as the first-priority Solar-C mission. The latest report from the Solar-C mission concept studies was documented as "Interim Report on the Solar-C Mission Concept." Title: Intensity Ratio of Density-sensitive Lines in Fe Ions Observed with a Well-defined Laboratory Plasma Authors: Nakamura, Nobuyuki; Watanabe, Etsushi; Sakaue, Hiroyuki A.; Kato, Daiji; Murakami, Izumi; Yamamoto, Norimasa; Hara, Hirohisa; Watanabe, Tetsuya Bibcode: 2011ApJ...739...17N Altcode: We present spectra of highly charged Fe ions in the extreme ultraviolet range observed using an electron beam ion trap equipped with a flat-field grazing incidence spectrometer. The density dependence of line intensity ratios is investigated for several density-sensitive lines of Fe XIII, XIV, and XV. Unlike previous studies where the electron density was estimated from theoretical considerations, here it is derived from electron beam profile measurements. The experimental data are compared with model calculations. Title: Spectroscopic Observations of Continuous Outflows and Propagating Waves from NOAA 10942 with Extreme Ultraviolet Imaging Spectrometer/Hinode Authors: Nishizuka, N.; Hara, H. Bibcode: 2011ApJ...737L..43N Altcode: We focused on "sit-and-stare" observations of an outflow region at the edge of active region NOAA 10942 on 2007 February 20 obtained by the Extreme ultraviolet Imaging Spectrometer on board Hinode. We analyzed the data above the base of the outflow and found both continuous outflows and waves, which propagate from the base of the outflow. The spectra at the base of the outflow and at higher locations show different properties. The line profiles show blue-side asymmetry at the base of the outflow where nonthermal broadening becomes large because of fast upflows generated by heating events. On the other hand, at higher locations line profiles are symmetric and the intensity disturbances vary in phase with the velocity disturbances. The correlations between the intensity and velocity disturbances become noticeable at higher locations, so this indicates evidence of (at least locally) upward propagating slow-mode waves along the outflow. We also found a transient oscillation of different period in the wavelet spectrum. This indicates that a different wave is additionally observed during a limited period. High cadence spectroscopic observations revealed intermittent signatures of nonthermal velocities. Each of them seems to correspond to the base of the propagating disturbances. Furthermore, a jet was captured by the sit-and-stare observations across the slit. The similarity of line profiles of the outflow and the jet may indicate that the flows and waves originate in unresolved explosive events in the lower atmosphere of the corona. Title: A Sounding Rocket Experiment for Spectropolarimetric Observations with the Lyα Line at 121.6 nm (CLASP) Authors: Ishikawa, R.; Bando, T.; Fujimura, D.; Hara, H.; Kano, R.; Kobiki, T.; Narukage, N.; Tsuneta, S.; Ueda, K.; Wantanabe, H.; Kobayashi, K.; Trujillo Bueno, J.; Manso Sainz, R.; Stepan, J.; de Pontieu, B.; Carlsson, M.; Casini, R. Bibcode: 2011ASPC..437..287I Altcode: A team consisting of Japan, USA, Spain, and Norway is developing a high-throughput Chromospheric Lyman-Alpha SpectroPolarimeter (CLASP), which is proposed to fly with a NASA sounding rocket in 2014. CLASP will explore the magnetism of the upper solar chromosphere and transition region via the Hanle effect of the Lyα line for the first time. This experiment requires spectropolarimetric observations with high polarimetric sensitivity (∼0.1%) and wavelength resolution (0.1 Å). The final spatial resolution (slit width) is being discussed taking into account the required high signal-to-noise ratio. We have demonstrated the performance of the Lyα polarimeter by extensively using the Ultraviolet Synchrotron ORbital Radiation Facility (UVSOR) at the Institute for Molecular Sciences. In this contribution, we report these measurements at UVSOR together with the current status of the CLASP project. Title: Coronal-Temperature-Diagnostic Capability of the Hinode/ X-Ray Telescope Based on Self-Consistent Calibration Authors: Narukage, N.; Sakao, T.; Kano, R.; Hara, H.; Shimojo, M.; Bando, T.; Urayama, F.; DeLuca, E.; Golub, L.; Weber, M.; Grigis, P.; Cirtain, J.; Tsuneta, S. Bibcode: 2011SoPh..269..169N Altcode: 2010arXiv1011.2867N; 2011SoPh..tmp....1N The X-Ray Telescope (XRT) onboard the Hinode satellite is an X-ray imager that observes the solar corona with unprecedentedly high angular resolution (consistent with its 1″ pixel size). XRT has nine X-ray analysis filters with different temperature responses. One of the most significant scientific features of this telescope is its capability of diagnosing coronal temperatures from less than 1 MK to more than 10 MK, which has never been accomplished before. To make full use of this capability, accurate calibration of the coronal temperature response of XRT is indispensable and is presented in this article. The effect of on-orbit contamination is also taken into account in the calibration. On the basis of our calibration results, we review the coronal-temperature-diagnostic capability of XRT. Title: Ionization non-equilibrium plasma during magnetic reconnection in solar corona Authors: Imada, S.; Murakami, I.; Watanabe, T.; Hara, H.; Shimizu, T. Bibcode: 2010AGUFMSH31A1788I Altcode: Hinode can provide us both of the stored magnetic field energy in corona before magnetic reconnection and the most part of energy post reconnection stage. On the other hand, there is not enough observational knowledge of the physical parameters in the reconnection region. The inflow into the reconnection region, the temperature of the plasma in the reconnection region, and the temperatures and densities of the plasma jets predicted by reconnection, have not been quantitatively measured in sufficient. EIS on Hinode may provide some answers if solar cycle 24 ever produces a solar maximum. But it is important to answer why the most observation cannot detect the predicted flow or temperature in the reconnection region. One of the reasons why we cannot observe inside the magnetic reconnection region is due to its darkness. Generally we can see the bright cusp-like structure during solar flare, although the reconnection region is faint/blind. One may think that the temperature in the reconnection region is enough higher than that of cusp-like flare loops. Thus the wavelength of emission from reconnection region is different from flare loops. However, this is not entirely true. Magnetic reconnection causes rapid heating. Thus ionization cannot reach to the equilibrium stage. We have calculated the ionization process in the down stream of Petschek type magnetic reconnection. From our result, we can clearly see that plasma cannot reach the ionization equilibrium in the down stream of slow-mode shock. The typical emissions from magnetic reconnection region are FeIXX or FeXX, although the plasma temperature is equal to 40MK. The typical temperature and density of post flare loops are 10 MK and 10^11 /cc, and the dominant emissions from post flare loops are from FeIXX to FeXXIII. Thus the wavelength of emission from reconnection region is not so much different from post flare loops. We will discuss how the emissions from reconnection region looks like by using several ionization calculations of magnetic reconnection. Title: The Chromospheric Lyman Alpha SpectroPolarimeter (CLASP) Authors: Kobayashi, K.; Tsuneta, S.; Trujillo Bueno, J.; Cirtain, J. W.; Bando, T.; Kano, R.; Hara, H.; Fujimura, D.; Ueda, K.; Ishikawa, R.; Watanabe, H.; Ichimoto, K.; Sakao, T.; de Pontieu, B.; Carlsson, M.; Casini, R. Bibcode: 2010AGUFMSH11B1632K Altcode: Magnetic fields in the solar chromosphere play a key role in the energy transfer and dynamics of the solar atmosphere. Yet a direct observation of the chromospheric magnetic field remains one of the greatest challenges in solar physics. While some advances have been made for observing the Zeeman effect in strong chromospheric lines, the effect is small and difficult to detect outside sunspots. The Hanle effect offers a promising alternative; it is sensitive to weaker magnetic fields (e.g., 5-500 G for Ly-Alpha), and while its magnitude saturates at stronger magnetic fields, the linear polarization signals remain sensitive to the magnetic field orientation. The Hanle effect is not only limited to off-limb observations. Because the chromosphere is illuminated by an anisotropic radiation field, the Ly-Alpha line is predicted to show linear polarization for on-disk, near-limb regions, and magnetic field is predicted to cause a measurable depolarization. At disk center, the Ly-Alpha radiation is predicted to be negligible in the absence of magnetic field, and linearly polarized to an order of 0.3% in the presence of an inclined magnetic field. The proposed CLASP sounding rocket instrument is designed to detect 0.3% linear polarization of the Ly-Alpha line at 1.5 arcsecond spatial resolution (0.7’’ pixel size) and 10 pm spectral resolution. The instrument consists of a 30 cm aperture Cassegrain telescope and a dual-beam spectropolarimeter. The telescope employs a ``cold mirror’’ design that uses multilayer coatings to reflect only the target wavelength range into the spectropolarimeter. The polarization analyzer consists of a rotating waveplate and a polarizing beamsplitter that comprises MgF2 plates placed at Brewster’s Angle. Each output beam of the polarizing beamsplitter, representing two orthogonal linear polarizations, is dispersed and focused using a separate spherical varied-line-space grating, and imaged with a separate 512x512 CCD camera. Prototypes of key optical components have been fabricated and tested. Instrument design is being finalized, and the experiment will be proposed for a 2014 flight aboard a NASA sounding rocket. Title: Hinode, STEREO and SOHO obervations of a CME event Authors: Landi, E.; Raymond, J. C.; Miralles, M. P.; Hara, H. Bibcode: 2010AGUFMSH31D..01L Altcode: Coronal Mass Ejections (CMEs) are among the most dramatic and violent dynamic events occurring in the solar atmosphere, and have significant impact on the near-Earth environment. So far, the physical processes responsible for their release and acceleration have not been completely understood, in part because of the lack of direct measurements of the CME plasma phycical parameters and evolution during the CME onset. Here we describe the analysis of multiwavelength observations from Hinode, SOHO and STEREO of the very early phases of a CME observed during the Whole Heliospheric Interval campaign. SECCHI/EUVI, SECCHI/COR1, SOHO/EIT and SOHO/LASCO images are used to reconstruct the 3D trajectory, velocity and acceleration up to 20 solar radii. Hinode/EIS, Hinode/XRT and SOHO/UVCS high resolution EUV spectra and X-ray images are used to measure the physical properties and the thermal structure of the core of the CME ejecta as a function of time up to 2.0 solar radii. The physical properties of the current sheet that formed after the CME erupted are also measured as a function of time. Title: Modeling of EIS Spectrum Drift from Instrumental Temperatures Authors: Kamio, S.; Hara, H.; Watanabe, T.; Fredvik, T.; Hansteen, V. H. Bibcode: 2010SoPh..266..209K Altcode: 2010SoPh..tmp..137K; 2010arXiv1003.3540K An empirical model has been developed to reproduce the drift of the spectrum recorded by the EIS on Hinode using instrumental temperatures and relative motion of the spacecraft. The EIS spectrum shows an artificial drift in wavelength dimension in sync with the revolution of the spacecraft, which is caused by temperature variations inside the spectrometer. The drift amounts to 70 km s−1 in Doppler velocity and introduces difficulties in velocity measurements. An artificial neural network is incorporated to establish a relationship between the instrumental temperatures and the spectral drift. This empirical model reproduces observed spectrum shift with an rms error of 4.4 km s−1. This procedure is robust and applicable to any spectrum obtained with EIS, regardless of the observing field. In addition, spectral curvatures and spatial offset in the north - south direction are determined to compensate for instrumental effects. Title: Mode Identification of MHD Waves in an Active Region Observed with Hinode/EIS Authors: Kitagawa, N.; Yokoyama, T.; Imada, S.; Hara, H. Bibcode: 2010ApJ...721..744K Altcode: 2010arXiv1008.1823K In order to better understand the possibility of coronal heating by MHD waves, we analyze Fe XII 195.12Å data observed with the EUV Imaging Spectrometer on board Hinode. We performed a Fourier analysis of EUV intensity and Doppler velocity time series data in the active region corona. Notable intensity and Doppler velocity oscillations were found for two moss regions out of the five studied, while only small oscillations were found for five apexes of loops. The amplitudes of the oscillations were 0.4%-5.7% for intensity and 0.2-1.2 km s-1 for Doppler velocity. In addition, oscillations of only the Doppler velocity were seen relatively less often in the data. We compared the amplitudes of intensity and those of Doppler velocity in order to identify MHD wave modes and calculated the phase delays between Fourier components of intensity and those of Doppler velocity. The results are interpreted in terms of MHD waves as follows: (1) few kink modes or torsional Alfvén mode waves were seen in both moss regions and the apexes of loops, (2) upwardly propagating and standing slow mode waves were found in moss regions, and (3) consistent with previous studies, estimated values of energy flux of the waves were several orders of magnitude lower than that required for heating active regions. Title: On Redshifts and Blueshifts in the Transition Region and Corona Authors: Hansteen, V. H.; Hara, H.; De Pontieu, B.; Carlsson, M. Bibcode: 2010ApJ...718.1070H Altcode: 2010arXiv1001.4769H Emission lines formed in the transition region (TR) of the Sun have long been known to show pervasive redshifts. Despite a variety of proposed explanations, these TR downflows (and the slight upflows in the low corona) remain poorly understood. We present results from comprehensive three-dimensional MHD models that span the upper convection zone up to the corona, 15 Mm above the photosphere. The TR and coronal heating in these models is caused by the stressing of the magnetic field by photospheric and convection "zone dynamics," but also in some models by the injection of emerging magnetic flux. We show that rapid, episodic heating, at low heights of the upper chromospheric plasma to coronal temperatures naturally produces downflows in TR lines, and slight upflows in low coronal lines, with similar amplitudes to those observed with EUV/UV spectrographs. We find that TR redshifts naturally arise in episodically heated models where the average volumetric heating scale height lies between that of the chromospheric pressure scale height of 200 km and the coronal scale height of 50 Mm. Title: Production of High-temperature Plasmas During the Early Phases of a C9.7 Flare Authors: Watanabe, Tetsuya; Hara, Hirohisa; Sterling, Alphonse C.; Harra, Louise K. Bibcode: 2010ApJ...719..213W Altcode: Explosive chromospheric evaporation is predicted from some current solar flare models. In this paper, we analyze a flare with high time cadence raster scans with the EUV Imaging Spectrometer (EIS) on board the Hinode spacecraft. This observation covers an area of 240'' × 240'', with the 1'' slit in about 160 s. The early phases of a C9.7 flare that occurred on 2007 June 6 were well observed. The purpose of our analysis is to study for the first time the spatially resolved spectra of high-temperature plasma, especially from Fe XXIII and Fe XXIV, allowing us to explore the explosive chromospheric evaporation scenario further. Sections of raster images obtained between 17:20:09 and 17:20:29 (UT) show a few bright patches of emission from Fe XXIII/Fe XXIV lines at the footpoints of the flaring loops; these footpoints were not clearly seen in the images taken earlier, between 17:17:30 and 17:17:49 (UT). Fe XXIII spectra at these footpoints show dominating blueshifted components of -(300 to 400) km s-1, while Fe XV/XIV lines are nearly stationary; Fe XII lines and/or lower temperature lines show slightly redshifted features, and Fe VIII and Si VII to He II lines show ~+50 km s-1 redshifted components. The density of the 1.5-2 MK plasma at these footpoints is estimated to be 3 × 1010 cm-3 by the Fe XIII/XIV line pairs around the maximum of the flare. High-temperature loops connecting the footpoints appear in the Fe XXIII/XXIV images taken over 17:22:49-17:23:08 (UT) which is near the flare peak. Line profiles of these high-temperature lines at this flare peak time show only slowly moving components. The concurrent cooler Fe XVII line at 254.8 Å is relatively weak, indicating the predominance of high-temperature plasma (>107 K) in these loops. The characteristics observed during the early phases of this flare are consistent with the scenario of explosive chromospheric evaporation. Title: Physical Conditions in a CME from Hinode, STEREO, and SOHO Observations Authors: Landi, E.; Raymond, J. C.; Miralles, M. P.; Hara, H. Bibcode: 2010ASPC..428..201L Altcode: In the present work we analyze multiwavelength observations from Hinode, SOHO, and STEREO of the early phases of a CME. We use EIS, UVCS, and XRT to measure the physical properties of the CME ejecta as a function of time at 1.1 and 1.9 Rsun. EUVI, COR 1, EIT, and LASCO images are used to measure the CME trajectory, velocity, and acceleration in 3D up to 5 Rsun. The diagnostic results are used to determine the energy budget of the CME plasma and the heating rate, and to compare it to theoretical predictions. Title: Response of the Solar Atmosphere to the Emergence of `Serpentine' Magnetic Field Authors: Harra, L. K.; Magara, T.; Hara, H.; Tsuneta, S.; Okamoto, T. J.; Wallace, A. J. Bibcode: 2010SoPh..263..105H Altcode: Active region magnetic flux that emerges to the photosphere from below will show complexity in the structure, with many small-scale fragmented features appearing in between the main bipole and then disappearing. Some fragments seen will be absorbed into the main polarities and others seem to cancel with opposite magnetic field. In this paper we investigate the response of the corona to the behaviour of these small fragments and whether energy through reconnection will be transported into the corona. In order to investigate this we analyse data from the Hinode space mission during flux emergence on 1 - 2 December 2006. At the initial stages of flux emergence several small-scale enhancements (of only a few pixels size) are seen in the coronal line widths and diffuse coronal emission exists. The magnetic flux emerges as a fragmented structure, and coronal loops appear above these structures or close to them. These loops are large-scale structures - most small-scale features predominantly stay within the chromosphere or at the edges of the flux emergence. The most distinctive feature in the Doppler velocity is a strong ring of coronal outflows around the edge of the emerging flux region on the eastern side which is either due to reconnection or compression of the structure. This feature lasts for many hours and is seen in many wavelengths. We discuss the implications of this feature in terms of the onset of persistent outflows from an active region that could contribute to the slow solar wind. Title: Physical Conditions in a Coronal Mass Ejection from Hinode, Stereo, and SOHO Observations Authors: Landi, E.; Raymond, J. C.; Miralles, M. P.; Hara, H. Bibcode: 2010ApJ...711...75L Altcode: In the present work, we analyze multiwavelength observations from Hinode, Solar and Heliospheric Observatory (SOHO), and STEREO of the early phases of a coronal mass ejection (CME). We use Hinode/EIS and SOHO/UVCS high-resolution spectra to measure the physical properties of the CME ejecta as a function of time at 1.1 and 1.9 solar radii. Hinode/XRT images are used in combination with EIS spectra to constrain the high temperature plasma properties of the ejecta. SECCHI/EUVI, SECCHI/COR 1, SOHO/EIT, and SOHO/LASCO images are used to measure the CME trajectory, velocity, and acceleration. The combination of measurements of plane of the sky velocities from two different directions allows us to determine the total velocity of the CME plasma up to 5 solar radii. Plasma properties, dynamical status, thermal structure, and brightness distributions are used to constrain the energy content of the CME plasma and to determine the heating rate. We find that the heating is larger than the kinetic energy, and compare it to theoretical predictions from models of CME plasma heating and acceleration. Title: On red-shifts in the transition region and corona . Authors: Hansteen, V. H.; Hara, H.; de Pontieu, B.; Carlsson, M. Bibcode: 2010MmSAI..81..729H Altcode: We present evidence that transition region red-shifts are naturally produced in episodically heated models where the average volumetric heating scale height lies between that of the chromospheric pressure scale height of 200 km and the coronal scale height of 50 Mm. In order to do so we present results from 3d MHD models spanning the upper convection zone up to the corona, 15 Mm above the photosphere. Transition region and coronal heating in these models is due both the stressing of the magnetic field by photospheric and convection `zone dynamics, but also in some models by the injection of emerging magnetic flux. Title: Flows in active regions revealed from Hinode EIS Observations Authors: Hara, Hirohisa Bibcode: 2010cosp...38.2930H Altcode: 2010cosp.meet.2930H Hinode EUV imaging spectrometer (EIS) has revealed the presence of high-velocity upflow components of nearly coronal sound speed near footpoints of coronal loops in quiescent active regions. The upflow is detected as an enhancement with low emission at the blue wing of the emission-line profile. The low-emission component suggests the presence of spatially unresolved upflows and smallness of each heating volume. Such fast flows are not observed in the high corona in general, and are expected when the heat input to the loop system is concentrated at the footpoints of coronal loops. We will discuss the implications for coronal heating mechanisms from the EIS observations and other observable such as photospheric magnetic fields. Title: Plasma Heating and Velocity Fields nearby Magnetic Reconnection Site Revealed from an EUV Emission-line Spectroscopy Authors: Hara, Hirohisa Bibcode: 2010cosp...38.2958H Altcode: 2010cosp.meet.2958H We report observational properties in the impulsive phase of a long duration flare on 2007 May 19 from spectroscopic observations with the Hinode EUV imaging spectrometer (EIS) with supplemental observations of Hinode SOT XRT, TRACE, and RHESSI. We have found an isolated hot source showing a largely enhanced nonthermal line broadening, a fast jet nearby, and an inflow structure to the hot source. Magnetic reconnection occurring above the loop-top region of the flare loop can account for these observations. Title: Characteristics of the Nonthermal Velocity Signature Observed in the Impulsive Phase of the 2007 May 19 Flare Authors: Hara, H.; Watanabe, T.; Bone, L. A.; Culhane, J. L.; van Driel-Gesztelyi, L.; Young, P. R. Bibcode: 2009ASPC..415..459H Altcode: The Hinode EUV Imaging Spectrometer (EIS) observed a long duration flare with a weak impulsive phase that appears to conform to the standard two-ribbon flare reconnection model. EIS scanned the flare site during the impulsive phase and observed Fe XXIII and Fe XXIV line emission that closely followed the flare hard X-ray emission while the line profiles showed significant non-thermal broadening. We suggest that a shock originating at the reconnection site which sweeps up and heats the coronal plasma can account for our observations. Title: Coronal Plasma Motions in Active Region Loops Observed with Hinode EIS Authors: Hara, H. Bibcode: 2009ASPC..415..252H Altcode: The Hinode EUV Imaging Spectrometer (EIS) has revealed the presence of high-velocity upflow components of nearly coronal sound speed near the footpoints of active region loops in a quiescent active region. The upflow is detected as subsonic line shifts with enhanced line broadenings when the emission line fitting by a Gaussian function is applied to the line-profile analysis for hot coronal emission lines, and it contributes to the line broadening because of the multiple components within the EIS spatial resolution, suggesting the presence of spatially unresolved upflows and the smallness of each heating volume. Title: Ion Temperature and Non-Thermal Velocity in a Solar Active Region: Using Emission Lines of Different Atomic Species Authors: Imada, S.; Hara, H.; Watanabe, T. Bibcode: 2009ApJ...705L.208I Altcode: We have studied the characteristics of the ion thermal temperature and non-thermal velocity in an active region observed by the EUV Imaging Spectrometer onboard Hinode. We used two emission lines of different atomic species (Fe XVI 262.98 Å and S XIII 256.69 Å) to distinguish the ion thermal velocity from the observed full width at half-maximum. We assumed that the sources of the two emission lines are the same thermal temperature. We also assumed that they have the same non-thermal velocity. With these assumptions, we could obtain the ion thermal temperature, after noting that M sulfur ~ 0.6M iron. We have carried out the ion thermal temperature analysis in the active region where the photon counts are sufficient (>4500). What we found is as follows: (1) the common ion thermal temperatures obtained by Fe XVI and S XIII are ~2.5 MK, (2) the typical non-thermal velocities are ~13 km s-1, (3) the highest non-thermal velocities (>20 km s-1) are preferentially observed between the bright points in Fe XVI, while (4) the hottest material (>3 MK) is observed relatively inside the bright points compared with the highest non-thermal velocity region. Title: Distribution of jets and magnetic fields in a coronal hole Authors: Kamio, S.; Hara, H.; Watanabe, T.; Curdt, W. Bibcode: 2009A&A...502..345K Altcode: Context: Recent observations of ubiquitous jets in coronal holes suggest that they play an important role in coronal heating and solar wind acceleration.