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1 宇宙線研究の百年 村木綏 by Yasushi Muraki A 100 years of cosmic ray research --- Present and Future ---

2 この漫画は名大太陽地球環境研究所の home page から取得できます

3 今日の話の主な内容 (today s talk) 宇宙線とは何か? What are cosmic rays? それはどういう方法で測られるのか? How do we measure HE cosmic rays? 現在何が問題なのか? What are current problems?

4 宇宙線研究の百年 - A 100 years of cosmic ray research - 1. 宇宙線研究の黎明期 ( ) (Early study on cosmic rays) 2. 宇宙線による素粒子物理学の研究 (1933-) (Study of elementary particles by cosmic rays) 3. 宇宙線による宇宙物理学の研究 (1941-) 最近の話題 (Study of universe by cosmic rays) 4. 宇宙線実験の最近の話題 (2009) (From recent topics and highlights of the studies)

5 Discovery of Radioactivity( 放射能の発見 ) 1900 年頃の物理学の最前線 (frontier of physics around 1900) 1896 Röntgen X 線の発見 1896 Becquerel ウラン鉱石から ray が出ている 1898 M. Curie, Schmidt pitchblende トリウム ラジウム ポロニウムからの放射線の発見 1903 Nobel prize to M+P. Curie and Becquerel 1900 α,β,γ 線の発見 3 種類がある

6 1. Discovery of Cosmic Rays 放射線は見えない 霧箱で見える (1911 Wilson) (cannot recognize by the naked eyes, by the cloud chamber) 電離計で測る (measurement by the ion chamber) 取りきれない成分が残った (existence of the background that is difficult to remove.)

7 The photograph of Hess and his Experiment around 最初の気球実験 Prof. Hess

8 Hess は高空ほど強度が上がる放射線の存在を確信した 高空でイオン強度が高まることを知った (The ionization rate increased at higher altitude) ヘスは気球に乗って高度依存性を調べたが 7 回目のフライトで上空からきている確信を得た (Hess used the balloon to investigate it.) 高空放射線となずけられた (Hohen-strahlung) Hess, Kolhörster, Gockel らの活躍

9 Millikan s Experiment ( ) 高山を利用した宇宙線研究の始まり 米国最高峰 Mt. Whitney(4418m), Muir Lake(3540m) (The experiment maybe belonged to very first experiment to do so at high altitude, mountain laboratories.)

10 Robert Millikan noticed that the rays must come from the universe, not from the Earth origin; cosmic rays 電荷に単位があることを見出したミリカン ( 米国 ) が高山の湖に装置を沈めてその強度を測定した かれは異なる高度で同じ実験を繰り返した その結果強度の減衰が完全に空気の厚みによる ことを見出し これらの放射線は地球外から飛来しているという認識に到達した そして宇宙線という名前を与えた 1940 年この名前にヘスが同意したのでそれ以来 宇宙線と呼ばれている 発見から 28 年が経過していた

11

12 Mount Whitney 4418m Lake Muir feet (4540m)

13 Mt. Whitney からの写真

14 宇宙線研究 素粒子の研究 ミクロの世界 Study of microscopic world 宇宙の研究 マクロの世界 Study of macroscopic world

15 2. Study of elementary particles by cosmic rays(Ⅰ) 宇宙線を使った素粒子研究 ( ) 1932 Anderson discovered Positrons ( 陽電子の発見 ) 反物質の発見 1937 Nedermyer discovered muons ( ミュー粒子の発見 ) 透過度が高い 1942 Sakata, Inoue, Tanigawa ( 二中間子論の提唱 ) 1947 Lattes, Occhialini, Powell discovered pions at Mt. Chacaltaya ( パイ中間子の発見 ) 湯川中間子 1948 Accelerator experiment started.. Many cosmic ray physicists moved to the field of high energy experiment 1948 Yukawa Nobel prize by the prediction of pi-meson ( パイ中間子の予言 ) 1950 Powell Nobel prize by the development of emulsion technique ( 原子核乾板開発と中間子の発見 )

16 Mt. Chacaltaya 5,250m in Bolivia

17 2 Study of elementary particles by cosmic rays(Ⅱ) 地道な宇宙線による素粒子研究は続いた 1966 Search for quarks in cosmic rays 1970 Niu Discovery of charmed particles in cosmic rays 1974 Proposal of the bag theory on the Quark クォーク閉じ込め理論又は袋理論の提案 1980 Search for proton decay and monopole GUT 1987 Discovery of neutrinos by Super Nova explosion 2002 Koshiba Nobel prize Present Search for dark matters in the universe 今も宇宙線中の新素粒子の探査は続いている

18 3. 宇宙線による宇宙の研究 - Where are cosmic rays accelerated? - 要約すると 宇宙線による宇宙の研究 ( ) 宇宙線がどこで作られているのかを理解すること どこでイオンが宇宙線と呼ばれる高エネルギー粒子に加速されているのかを調べる 粒子加速過程の研究をしている Studying particle acceleration processes in various parts of the universe.

19 宇宙線のエネルギー分布 太陽起源 ~1/m 2 sec 衝撃波加速 ~ 1/m 2 year フロンティア領域 ~ 1/km 2 year Energy frontier 12 桁

20 flare Protons are accelerated beyond 56 GeV 太陽起源宇宙線 Forbush found solar particles

21 Space weather forecast from ISS

22 宇宙線のエネルギー分布 (knee 領域 ) Knee 領域の宇宙線は 超新星残骸で作られているという有力な仮説が 1977 年ころ提唱された このような高いエネルギーの宇宙線は空気シャワーを利用して測定する 電磁石では測れない

23 空気シャワーの概念図 air shower

24 チェレンコフ光を測定約 1 万 ~10 万個の電子 by Mori

25 超新星残骸での高エネルギー電子加速の証拠 SRN with resolved shells (2009) Latest addition: SN 1006 expands in uniform environment above the Galactic plane kev X-rays VHE -rays smoothed X-ray contours B? Flux: 1% Crab H.E.S.S. prelim.

26 超新星残骸起源説 hypothesis SNR origin 超新星残骸 SN1006 からの TeV カ ンマ線の観測成功は電子がこの超新星残骸で 100TeV まで加速されているとする あすか X 線衛星の観測結果 (Koyama et al.) を証明した TeVγ 線は衝撃波加速理論に従って加速されていると考えられる しかしこれですべてが解決したわけではない (The discovery of TeV gamma-rays from the SNR 1006 confirmed a prediction by ASKA X-ray group that electrons are accelerated up to 100 TeV in the shock front of the Super Nova Remnant.)

27 4. From recent topics and highlights of cosmic ray studies 最高エネルギー宇宙線の謎 人類が到達できる最高のエネルギーである すなわちエネルギー フロンティアーである 何か big surprise が隠されているかもしれないという 期待感がそこにはある 日本の AGASA データが それを示唆している

28 1x10 18 ev の宇宙線まで arm に閉じ込められる

29 P=300Hρ P=300Hρ P= H 3 µgauss ρ 500pc = cm P= ev

30 最高エネルギー宇宙線はどこからやってくるのか? 源は銀河内? 源は銀河外?

31 An interesting historical stories (extra) Enrico Fermi suggested to Rossi, probably cosmic rays will be not involved in the galactic arm, due to the limit of the magnetic field, so cut-off of the cosmic rays in the energy spectrum must be observed. This is the origin of Fermi Rossi the air shower experiment by Bruno Rossi (Prof. Oda told me it)

32 最高エネルギー宇宙線の謎 GZK cut-off はあるのか? Auger は GZK cut-off をみつけたのか? 3 実験の絶対値 ( エネルギースケール / フラックス ) のずれの理由は?

33 The LHCf experiment CERN では LHC という大型加速器が 11 月に稼動する そのエネルギーは実験室系で ev に相当する このエネルギー領域で核相互作用のモデルを Calibration( 更正 ) して ev 領域の宇宙線実験の解釈に役立てようという実験が行われる (At CERN, the LHC machine is almost going to start in this November. With use of this high energy, the LHC collaboration will get the pion cross-section emitted at very forward region and calibrate the MC codes that are used in the determination of energy of each shower.)

34 The LHCf Collaboration (31 人 ) K.Fukui, Y.Itow, T.Mase, K.Masuda, Y.Matsubara, H.Menjo, T.Sako, K.Taki, H.Watanabe Solar-Terrestrial Environment Laboratory, Nagoya University, Japan K.Yoshida K.Kasahara, M.Mizuishi, Y.Shimizu, S.Torii Shibaura Institute of Technology, Japan Waseda University, Japan T.Tamura Kanagawa University, Japan Y.Muraki Konan University M.Haguenauer Ecole Polytechnique, France W.C.Turner LBNL, Berkeley, USA O.Adriani, L.Bonechi, M.Bongi, R.D Alessandro, M.Grandi, P.Papini, S.Ricciarini, G.Castellini INFN, Univ. di Firenze, Italy A.Tricomi INFN, Univ. di Catania, Italy J.Velasco, A.Faus IFIC, Centro Mixto CSIC-UVEG, Spain D.Macina, A-L.Perrot CERN, Switzerland

35 まとめ Summary 最高エネルギー宇宙線の研究はエネルギーフロンティアの領域であり big surprise が隠れている可能性が大きい しかし当面は各実験間の矛盾を解く必要がある これらは加速器や Auger 実験と異なる TA 実験等で確認されるであろう その後は巨大な北 Auger 計画や EUSO 計画で break through があるかどうか 探求が進むであろう 宇宙線の長期変動と気候に与える影響という大変興味ある分野もあるが 時間の関係で割愛した The highest energy region of cosmic rays belong to the energy frontier. Therefore a big surprise may hidden there. At the moment, we must resolve the discrepancy between each experimental result, being based on the LHCf experiment or different experimental method like TA. However after that, the region must be investigated by using more large detectors like North Auger and EUSO projects.

36 まとめ 宇宙線は発見されて百年になるが まだその成因については 十分理解されたとは言えないのが現状である 宇宙線研究は今後も続くであろう 月面は非常に宇宙線観測にむいた場所である

37 逆コンプトン効果の概念図 inverse Compton effect

38 The position of shower maximum Knapp et al, Astroparticle Physics, 19(2003) 77 LHCf UA7 Fe incidence

39 衝突の両 side に測定器を置く Detector I Tungsten Scintillator Scintillating fibers INTERACTION POINT Detector II Tungsten Scintillator Silicon strips 140 m 140 m Beam line 1. Redundancy 2. Background rejection (especially beam-gas) 3. Physics single diffractive/double diffractive

40 Examples of simulated events for and n

41 Detector location Y Chamber

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