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動的な太陽大気モデルの系譜 磁気大気の活動性の起源 加藤 成晃（NAOJ） 太陽と恒星の物理学 2011/12/26-28 1

動的な太陽大気モデルの系譜 磁気大気の活動性の起源 加藤 成晃（NAOJ） 太陽と恒星の物理学 2011/12/26-28 Ca II H Okamoto et al. (2007) 1

概要 動的な太陽大気モデリングの系譜 今後の太陽大気モデリングの課題 新しい試みの紹介 太陽と恒星の物理学 2011/12/26-28 2

Toward Realistic 太陽と恒星の物理学 2011/12/26-28 Photo-ionization Modelings of Solar Atmosphere Collisional excitation Radiative cooling Ionization EOS Lines Continuum Opacity LTE + Non-LTE Radiative Transfer field lines from corona Heat conduction along Magneto-convection 10 6 K - - ✓ z [Mm] ✓ - 10 5 K ✓ 2 ✓ 1 0 6000 K - - Schrijver 2001 3

Toward Realistic Lines 太陽と恒星の物理学 2011/12/26-28 EOS Radiative cooling Magneto-convection Modelings of Solar Atmosphere Collisional excitation Ionization Photo-ionization Continuum LTE + Non-LTE Heat conduction along Radiative Transfer field lines from corona Opacity Basic equations 10 6 K - - ✓ z [Mm] ✓ - 10 5 K ✓ 2 ✓ 1 0 6000 K - - Solar “ingredients”: Schrijver 2001 3

What physics need to be Radiation in strong lines from H, Ca, Mg, He (Non-LTE 6-12 levels per element) and in many weak non-Maxwellian distribution functions need kinetic modelling Need to solve rate equation for Hydrogen ionization Plasma Chromosphere is mostly neutral (multi-fluid) Reconnection, high Alfven velocity (Shor time-scale) included in numerical Non-locality, Frequency integration, and Scattering Radiation transfer lines (many frequency bins) MHD Energy flow from convection zone to corona Conduction (Short time-scale) Shock dissipation (High spatial resolution) Energy balance simulations? 2-D/3-D domain ranging from convection zone to corona Can we do this? ✓ ✓ ✓ • In principle, yes ✓ • 20 km resolution, 50 Mm box, NLTE H+Ca+He +Mg: 6 million years on 5000 CPUs for one hour of solar time ✓ • In practice, no ✓ ✓ ✓ by M. Carlsson ✓

石川 岡本 勝川 太陽と恒星の物理学 2011/12/26-28 Current understanding of the dynamics in Quiet Region Corona Chromosphere Photosphere Convection zone Conventional picture 5

太陽と恒星の物理学 2011/12/26-28 Current understanding of the dynamics in Quiet Region Canopy Magnetic Canopy β =1 Sub-canopy Sub-magnetic τ 500 =1 Convection zone Modern picture 6

Magneto-convection simulation “fly” movie by Mats Carlsson & Bob Stein (Stagger code) G-band 7

Magneto-convection simulation “fly” movie by Mats Carlsson & Bob Stein (Stagger code) G-band B-field 7

Magneto-convection simulation “fly” movie by Mats Carlsson & Bob Stein (Stagger code) Height where tau=1 G-band B-field 7

Magneto-convection simulation “fly” movie by Mats Carlsson & Bob Stein (Stagger code) Height where tau=1 G-band B-field 7

3-D Dynamical Modeling of Network/Internetwork Region M. Carlsson by using BIFROST (Gudiksen et al. 2011) 太陽と恒星の物理学 2011/12/26-28 8

3-D Dynamical Modeling of Network/Internetwork Region M. Carlsson by using BIFROST (Gudiksen et al. 2011) 太陽と恒星の物理学 2011/12/26-28 8

3-D Dynamical Modeling of Network/Internetwork Region M. Carlsson by using BIFROST (Gudiksen et al. 2011) 太陽と恒星の物理学 2011/12/26-28 8

太陽と恒星の物理学 2011/12/26-28 Comparison between Models and Observations RMHD Model atmosphere Detailed Radiation transfer Simulated intensity Inversion Reconstructed Observations atmosphere 9

太陽と恒星の物理学 2011/12/26-28 勝川 Ca II H-line formation in 1-D Non-LTE Model atmosphere by Carlsson & Stein 1992, 1994, 1995, 1997 10

太陽と恒星の物理学 2011/12/26-28 Ca II H-line formation in 1-D Non-LTE Model atmosphere by Carlsson & Stein 1992, 1994, 1995, 1997 10

太陽と恒星の物理学 2011/12/26-28 Current issues for modeling of Solar atmosphere What’s minimum temperature? Heating Total heating rate ad-hoc heating rate Total Radiative heating rate Compression work Cooling Leenaarts et al. 2011 Martinez-Sykora, De Pontieu, Hansteen 2012 11

Chromosphere/Corona heating “Energy flows” 太陽と恒星の物理学 2011/12/26-28 Dissipation Propagation Excitation 12

Discovery of Excitation of Slow-modes YK, Steiner, Steffen, Suematsu (2011) by using CO 5 BOLD white contour: Magnetic field line, Arrows: velocity White & Black curve: Optical surface 太陽と恒星の物理学 2011/12/26-28 T gas N x =400 N z =165 13

太陽と恒星の物理学 2011/12/26-28 YK, Steiner, Steffen, Suematsu (2011) EXCITATION OF SLOW-MODE & SHOCK Downflow Upflow -10 -5 0 5 10 V z [km s -1 ] time = 12.5 min time = 13.8 min time = 15.1 min time = 16.4 min 200 0 -200 z [km] -400 core -600 -800 -1000 -1200 4000 4400 4800 5200 4000 4400 4800 5200 4000 4400 4800 5200 4000 4400 4800 5200 (a) x [km] x [km] x [km] x [km] <V z > skin [km s -1 ] <V z > core [km s -1 ] 200 shock downflow 0 upflow -200 skin skin downdraft -400 z [km] < ! > core = 1 -600 < " > core = 1 -800 Spatially averaged vertical Spatially averaged vertical -1000 velocity in the skin region velocity in the core region -1200 12 13 14 15 16 17 18 12 13 14 15 16 17 18 (b) Time [min] Time [min] 14

太陽と恒星の物理学 2011/12/26-28 wave Downdrafts YK, Steiner, Steffen, Suematsu (2011) EXCITATION OF SLOW-MODE & SHOCK Magnetic pumping Downflows Shock Downflow Upflow -10 -5 0 5 10 V z [km s -1 ] time = 12.5 min time = 13.8 min time = 15.1 min time = 16.4 min 200 0 -200 z [km] -400 -600 -800 -1000 -1200 4000 4400 4800 5200 4000 4400 4800 5200 4000 4400 4800 5200 4000 4400 4800 5200 (a) x [km] x [km] x [km] x [km] <V z > skin [km s -1 ] <V z > core [km s -1 ] 200 shock downflow 0 upflow -200 downdraft -400 z [km] < ! > core = 1 -600 < " > core = 1 -800 Spatially averaged vertical Spatially averaged vertical -1000 velocity in the skin region velocity in the core region -1200 12 13 14 15 16 17 18 12 13 14 15 16 17 18 (b) Time [min] Time [min] 14

まとめ 動的な太陽大気モデリングにはRMHDが必要不可欠！ 磁気大気：Canopyなどの複雑な磁場構造によって大気構造が決まっている Ca II H-lineの放射メカニズムには衝撃波からの複雑な寄与がある 実用的なRMHD計算技術の開発が必要 Opacity table/Realistic EOS 高速化 定常一次元”平行平板”大気モデルについて ただし「動的な太陽大気モデル」から「定常一次元的な大気モデル」を再構 築することは、太陽と恒星の理論と観測の両方の面で重要かも知れない。 太陽と恒星の物理学 2011/12/26-28 15