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Abstract:   太陽の彩層・遷移層は、プラズマ圧優勢から磁気圧優勢に切り替わる領域であり、ここでの詳 細な磁場計測とプラズマの動的現象との同時観測こそが次の太陽物理のフロンティアである。 これはまさに次期太陽観測衛星計画SOLAR-­‐Cでも挙げられている課題であるが、SOLAR-­‐ C計画に先駆けて我々はNASA観測ロケットを用いた実験で、彩層・遷移層磁場計測に取り組も うとしている。それが、Chromospheric  Lyman-­‐Alpha  Spectro-­‐Polarimeter  (CLASP)   計画であり、彩層・遷移層が放つライマンα輝線(121.6nm)の直線偏光を0.1%の高精度で検出し 、ハンレ効果という新手法で彩層・遷移層の磁場情報を取得する。日米欧共同観測ロケット実 験として2012年11月にNASAに採択されて本格始動した本計画では、フライト観測装置の組立て 作業が2014年春から始まり、現在、光学素子のアライメントが実施されているところである。 この後、2015年夏の観測実施に向けて性能評価へと進む予定である。本講演では計画内容を改 めて説明するとともに、全体の開発・準備現状の概要を報告する。     Authors:   • Ryohei  Kano       [email protected]   • Takamasa  Bando   [email protected]   • Noriyuki  Narukage   [email protected]   • Ryoko  Ishikawa     [email protected]   • Masahito  Kubo     [email protected]   • Yukio  Katsukawa   [email protected]   • Shin-­‐nosuke  Ishikawa   [email protected]   • Hirohisa  Hara     [email protected]   • Yoshinori  Suematsu   [email protected]   • Gabriel  Giono     [email protected]   • Toshifumi  Shimizu   [email protected]   • Taro  Sakao     [email protected]   • Kiyoshi  Ichimoto   [email protected]­‐u.ac.jp   • Motoshi  Goto     [email protected]   • Amy  Winebarger   [email protected]   • Ken  Kobayashi     ken.kobayashi-­‐[email protected]   • Javier  Trujillo-­‐Bueno   [email protected]   • Frederic  Auchere   [email protected]­‐psud.fr (cid:4788)(cid:14183)(cid:2146)(cid:5740)(cid:5273)(cid:2285)(cid:13380)(cid:9955)(cid:5273)(cid:2147)(cid:2058)(cid:2249)(cid:2267)(cid:2220)(cid:2256)(cid:4477)(cid:3459)(cid:3779)(cid:2111)(cid:2173)(cid:9762)(cid:7868)(cid:4477)(cid:3459)(cid:3779)(cid:2143)(cid:3625)(cid:2174)(cid:7024)(cid:2179)(cid:2175)(cid:14463)(cid:4582)(cid:2139)(cid:2102)(cid:2174)(cid:2058)(cid:2119)(cid:2119)(cid:2139)(cid:2146)(cid:12530) (cid:10493)(cid:2142)(cid:9762)(cid:4633)(cid:12451)(cid:8196)(cid:2140)(cid:2249)(cid:2267)(cid:2220)(cid:2256)(cid:2146)(cid:3767)(cid:9431)(cid:8999)(cid:12767)(cid:2140)(cid:2146)(cid:4000)(cid:6892)(cid:12411)(cid:8196)(cid:2119)(cid:2129)(cid:2112)(cid:7711)(cid:2146)(cid:4788)(cid:14183)(cid:8768)(cid:9006)(cid:2146)(cid:2247)(cid:2271)(cid:2277)(cid:2232)(cid:2197)(cid:2196)(cid:2139)(cid:2102)(cid:2175)(cid:2059) (cid:2119)(cid:2176)(cid:2147)(cid:2162)(cid:2121)(cid:2143)(cid:7711)(cid:7047)(cid:4788)(cid:14183)(cid:12411)(cid:8196)(cid:12200)(cid:6861)(cid:12451)(cid:9196)SOLAR-C(cid:2139)(cid:2166)(cid:6386)(cid:2118)(cid:2173)(cid:2176)(cid:2138)(cid:2104)(cid:2175)(cid:12578)(cid:14495)(cid:2139)(cid:2102)(cid:2175)(cid:2112)(cid:2058)SOLAR- C(cid:12451)(cid:9196)(cid:2143)(cid:3483)(cid:14673)(cid:2117)(cid:2138)(cid:6211)(cid:2062)(cid:2147)NASA(cid:12411)(cid:8196)(cid:2271)(cid:2211)(cid:2229)(cid:2234)(cid:2182)(cid:9181)(cid:2104)(cid:2131)(cid:5127)(cid:14722)(cid:2139)(cid:2058)(cid:5740)(cid:5273)(cid:2285)(cid:13380)(cid:9955)(cid:5273)(cid:9762)(cid:4633)(cid:12451)(cid:8196)(cid:2143)(cid:3958)(cid:2174)(cid:10508)(cid:2166) (cid:2106)(cid:2140)(cid:2123)(cid:2138)(cid:2104)(cid:2175)(cid:2059)(cid:2129)(cid:2176)(cid:2112)(cid:2058)Chromospheric Lyman-Alpha Spectro-Polarimeter (CLASP) (cid:12451)(cid:9196)(cid:2139)(cid:2102)(cid:2174)(cid:2058)(cid:5740)(cid:5273)(cid:2285)(cid:13380)(cid:9955)(cid:5273)(cid:2112)(cid:6714)(cid:2136)(cid:2267)(cid:2198)(cid:2256)(cid:2277)(cid:626)(cid:13156)(cid:10618)(121.6nm)(cid:2146)(cid:9508)(cid:10618)(cid:3307)(cid:3484)(cid:2182)0.1%(cid:2146)(cid:14807)(cid:10413)(cid:5592)(cid:2139)(cid:7400)(cid:3615)(cid:2123) (cid:2058)(cid:2241)(cid:2277)(cid:2270)(cid:3744)(cid:7133)(cid:2140)(cid:2104)(cid:2106)(cid:6786)(cid:6253)(cid:7986)(cid:2139)(cid:5740)(cid:5273)(cid:2285)(cid:13380)(cid:9955)(cid:5273)(cid:2146)(cid:9762)(cid:4633)(cid:5983)(cid:4631)(cid:2182)(cid:3958)(cid:5779)(cid:2125)(cid:2175)(cid:2059)(cid:6821)(cid:10367)(cid:7714)(cid:3513)(cid:4000)(cid:12411)(cid:8196)(cid:2271)(cid:2211)(cid:2229)(cid:2234)(cid:5127) (cid:14722)(cid:2140)(cid:2123)(cid:2138)2012(cid:5562)11(cid:7030)(cid:2143)NASA(cid:2143)(cid:6471)(cid:6309)(cid:2121)(cid:2176)(cid:2138)(cid:7055)(cid:7233)(cid:4894)(cid:3767)(cid:2123)(cid:2131)(cid:7055)(cid:12451)(cid:9196)(cid:2139)(cid:2147)(cid:2058)(cid:2247)(cid:2267)(cid:2198)(cid:2234)(cid:12411)(cid:8196)(cid:12262)(cid:10792)(cid:2146)(cid:10508)(cid:10087)(cid:2138) (cid:3128)(cid:7447)(cid:2112)2014(cid:5562)(cid:6867)(cid:2111)(cid:2173)(cid:4894)(cid:2162)(cid:2174)(cid:2058)(cid:8999)(cid:4478)(cid:2058)(cid:3484)(cid:5083)(cid:10482)(cid:5066)(cid:2146)(cid:2196)(cid:2267)(cid:2198)(cid:2259)(cid:2277)(cid:2234)(cid:2112)(cid:5127)(cid:6795)(cid:2121)(cid:2176)(cid:2138)(cid:2104)(cid:2175)(cid:2140)(cid:2119)(cid:2177)(cid:2139)(cid:2102)(cid:2175)(cid:2059) (cid:2119)(cid:2146)(cid:5771)(cid:2058)2015(cid:5562)(cid:4767)(cid:2146)(cid:12411)(cid:8196)(cid:5127)(cid:6795)(cid:2143)(cid:4005)(cid:2117)(cid:2138)(cid:5878)(cid:11039)(cid:12507)(cid:3183)(cid:2156)(cid:2140)(cid:13325)(cid:2164)(cid:2979)(cid:5123)(cid:2139)(cid:2102)(cid:2175)(cid:2059)(cid:7055)(cid:12654)(cid:8327)(cid:2139)(cid:2147)(cid:12451)(cid:9196)(cid:3526)(cid:5148)(cid:2182)(cid:6709) (cid:2165)(cid:2138)(cid:12573)(cid:6850)(cid:2125)(cid:2175)(cid:2140)(cid:2140)(cid:2166)(cid:2143)(cid:2058)(cid:3506)(cid:3119)(cid:2146)(cid:14052)(cid:9422)(cid:2285)(cid:8253)(cid:3355)(cid:8999)(cid:8807)(cid:2146)(cid:7467)(cid:12379)(cid:2182)(cid:4631)(cid:4044)(cid:2125)(cid:2175)(cid:2059) Chromospheric Lyman-Alpha SpectroPolarimeter (CLASP) Authors: (cid:120) Ryohei Kano [email protected] (cid:120) Takamasa Bando [email protected] (cid:120) Noriyuki Narukage [email protected] (cid:120) Ryoko Ishikawa [email protected] (cid:120) Masahito Kubo [email protected] (cid:120) Yukio Katsukawa [email protected] (cid:120) Shin-nosuke Ishikawa [email protected] (cid:120) Hirohisa Hara [email protected] (cid:120) Yoshinori Suematsu [email protected] (cid:120) Gabriel Giono [email protected] (cid:120) Toshifumi Shimizu [email protected] (cid:120) Taro Sakao [email protected] (cid:120) Kiyoshi Ichimoto [email protected] (cid:120) Motoshi Goto [email protected] (cid:120) Amy Winebarger [email protected] (cid:120) Ken Kobayashi [email protected] (cid:120) Javier Trujillo-Bueno [email protected] (cid:120) Frederic Auchere [email protected] Google translation: Chromosphere, the transition layer of the sun is a region to switch to the magnetic pressure dominated from plasma pressure dominated, simultaneous observation of the detailed magnetic field measurement and plasma of dynamic phenomenon here is what is the frontier of the next solar physics. As This is a challenge that has just mentioned, even the next solar observation satellite plan SOLAR-C, in the experiments we had used a NASA sounding rocket for the first time in the SOLAR-C plan, will address the chromosphere-transition layer magnetic field measurement there. It is, is a Chromospheric Lyman- Alpha Spectro-Polarimeter (CLASP) plan, the linear polarization of Lyman (cid:626) emission lines chromosphere-transition layer shoots (121.6nm) were detected in 0.1% of high accuracy, a new technique called Hanre effect I get the magnetic field information of chromosphere-transition layer. In Japan, the US and Europe joint observation in November 2012 as a rocket experiment is adopted to NASA this plan that full-scale start-up, start from assembly work is 2014 spring flight observation device, currently, it is where the alignment of the optical elements have been implemented . After this, it is planned to continue with the performance evaluation towards the observation implementation of summer 2015. In addition to once again explain the contents of the plan In this presentation, we report an overview of the entire development and preparation current status.

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