Microsoft PowerPoint - 太陽黒点と磁場.pptx
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1 太陽黒点と磁場 一本潔京都大学 太陽 恒星研究会 ー 28 於 : 東大本郷 太陽物理学と恒星物理学の相互交流と将来的展望
2 内容 1. Global properties of sunspots 2. Fine structures 3. Model 4. Summary
3 1. Global properties of sunspots umbra pore penumbra SoHO/MDI (2001) 1989/09/07 Sunspots often appear as a group or a pair aligned in E-W direction Developed sunspots consist of umbra and penumbra
4 Two historic discoveries on sunspot Sunspot magnetic field, G.Hale 1908 ApJ, その後 磁場 が太陽物理のキーワードに Evershed effect, J.Evershed 1909 umbra Limb side: Red shift 記念切手 ( インド 2009) Disk center side Blue shift penumbra Horizontal outflow 1~2km/s 100 年来の謎 黒点とガスダイナミクスの密接な関係
5 黒点のサイズ : 3500 ~ 60000km with penumbra < 7000km without penumbra (pore) Largest sunspot ever observed (Mitaka sketch) ~130,000km A ~ 0.5% of solar disk
6 寿命 : Larger sunspot has longer life; (Gnevyshev-Waldmeier 則 ) e.g. 80~90day for 60,000km, 2~3day for 10,000km 明るさ : brightness (in vis.) temperature umbra: I QS, K penumbra: I QS, ~ 5600K Sunspot is dark But, still brighter than a tungsten lamp (~3700K) 磁場の強度 : Typical: 1500 ~ 4000G Max. record: 6100G (1942 Feb 28) (Livingstone etal 2006)
7 黒点のサイズ 磁場と明るさ brightness vs. size brightness vs. field strength 1.56 m continuum intensity 1.56 m continuum 1.56 m continuum intensity Larger sunspots tend to be darker and have a stronger magnetic field. Umbral diameter [arcsec] Solanki, 2002 Triangles - Kopp & Rabin (1992), filled square - Solanki et al. (1992), 3 stars - Ruedi et al. (1995b) Field strength [G] Livingston 2002, Sol.Phys. darkest part in umbra at FeI1.56 m
8 Global structure of sunspot magnetic field and flow Bz Magnetic fields umbra penumbra Br Evershed flow 1 ~ 2 km/s Azimuth v // B A century-long puzzle (till ~1990) -- Why can sunspots be maintained? -- Mathew etal 2003
9 黒点磁場の測定 スペクトル線のゼーマン効果 Zeeman effect of spectral line SOT/Spectro-polarimeter I Q FeI6301.5A FeI6302.5A g = 1.67 g = 2.5 U V
10 Stokes profiles: Zeeman effect I Q プロファイルのフィッティング 磁場の 3 成分 視線速度 U V
11 Suntpot magnetic field Field strength Field inclination 0 ~ 4000 Gauss -90 o ~ +90 o
12 2. Fine structures
13 Sunspots are rich in fine scale structures. 黒点の寿命 ~2 週間 >> 微細構造の寿命 ~1 時間 黒点は静的平衡状態ではなく動的平衡状態. Hinode FG/SOT
14
15 高分解能でみた磁場速度場 磁場の太陽面法線からの傾き ドップラーシフト 半暗部の磁場は放射状に水平な磁場とより立った磁場が交互に並んでいる エバーシェッド流は水平な磁場に沿って流れていた
16 Stokes-V at A +100mA (sign reversed) = 2.9o -100mA +100mA
17 Stokes-V at A +277mA (sign reversed) Dark patches: Upflow with the same polarity of the sunspot -277mA White patches: Downflow with the opposite polarity to the sunspot +277mA
18 V (+365mA) - V (-276mA) DC 2.9o
19 Inclination of mag. Field DC 2.9o
20 Inclination of mag. Field DC 2.9 o 上昇流と下降流が水平チャンネルの両端に エバーシェッド流要素のわき出しと沈み込みが見えた
21 Continuum image DC 2.9o
22 Continuum image 上昇流と輝点のよい一致. エバーシェッド流は表面に熱を運んでいる DC 2.9 o
23 黒点の磁場構造とエバーシェッド流 umbra Rising hot gas (overturning?) cooling Supersonic downflow 半暗部の筋構造とエバーシェッド流は傾いた強い磁場の中でおこる熱対流現象の結果として理解できる. Scharmer 2009; Ichimoto etal 2009; Rempel etal 2009, Borrero 2008
24 Dynamics of the Evershed flow element Inward migration of bright grain Deflected into horizontal direction by Lorentz force Overturning convection Rising hot gas driven by vertical pressure force cooling Magnetic field line ~ 1 Supersonic downflow
25 Dynamics in sunspot chromosphere SOT CaII H Katsukawa et al. (2007) Ca II H movie FFT filtered (f>3mhz) Oscillation (umbral flush) & waves! Jets in penumbra! 28
26 解釈 : 半暗部磁場構造に起因した磁気リコネクション Vertical magnetic field lines Magnetic reconnection Penumbral filaments 29
27 暗部内輝点の磁場と速度場 磁場強度が弱く (Fe I 6302 で 17Gauss) 水平に傾いていて (0.6 ) 上昇流 (28m/s) を伴う H.Watanabe et al. (2008) 対流か振動これも表面に熱を運んでいる
28 3. Modeling
29 Global sunspot models We don t know the 3D structure of sunspot Mag.buoyancy Mag.tension ~ 1Mm Monolith interchange instability (Meyer etal 1977) Hypothesecal flow Cluster or Spaghetti Parker, 1979, ApJ, 230, 905 Sunspot cannot be in magnetohydrostatic, but be in a dynamic equilibrium.
30 Time distance 法による内部診断 (MDI/SoHO) (Zhao et al. 2001, NASA/ESA) 黒点直下の下降流 cluster model の傍証 35
31 MHD simulation (Rempel etal 2009, Science 325) driving the Evershed flow does not require physical processes that go beyond the combination of convection and anisotropy introduced by the magnetic field.
32 Simulation versus reality Simulation 12x12x8 km Resolution Non-grey Observation F. Wöger (NSO) Dunn telescope Courtesy Rempel 2011
33 Rempel 2011
34
35 Field structure in penumbra
36 黒点とタコクラインとの切断 冷却による下降流 対流の上昇流 ガス圧上昇磁場強度低下 磁束管の磁場強度 時間 40hr 対流によって磁場はぐちゃぐちゃになる 対流層下部との力学的な切断 対流と equipartition Schussler and Rempel, 2005, AA, 441, 337
37 4. Summary: 太陽黒点の基本 表面 構造は ひので 地上高分解能観測 および数値シミュレーションにより ここ数年飛躍的に理解が進 んだ その本質は強い磁場とガスの相互作用による磁気対流 現象である 黒点深部の構造も日震学と数値シミュレーションにより最近メス が入り始めたが ダイナモ領域に至る接続は謎である わからないこと 恒星からも学びたい課題 - 黒点のサイズの上限はどこにあるか - 黒点の成長 崩壊 消滅過程は何が決めているか - 活動サイクルの規則性と不規則性 - 活動経度の起源 発生緯度を決めているもの - 磁場の自由エネルギーの蓄積機構 複雑黒点の形成過程 - 電流系 中性 分子 の黒点ダイナミクスへの影響
38 Sunspots are not necessarily simple Hida DST Ishii etal, 1998, ApJ
39 Thank you!
- 3 Solar-B -
- 3 Solar-B - continuum - - - ( 3 ) Solar-B - ( ) ( ) (SoHO/MDI) Pore Penumbra (umbra) (= ) ( ) - - - 0.5km/s 3 (Advanced Stokes Polarimeter:ASP) (Lites al. 1998 ) - (pore ) - penumbra - SOT/EIS/XRT -
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