EOS EOS
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1 EOS EOS
2
3 SN1987A Crab nebula (SN1054) A.K.Mann "Shadow of a Star" From
4 重力崩壊型超新星爆発 中性子星 ブラックホールの誕生 重元素の起源 rプロセス 爆発的元素合成 銀河の進化 宇宙線 ガンマ線バースト 重力波 爆発メカニズムの解明 重力崩壊 コアバウンス 3 10 Explosion Dynamics Trapping, heating 2 10 ν νν ν Pt, Au ν ν SUBAR U Mass number Origin of Elements r-process, ν-process Super-Kamiokande ν ν ν Dense Matter Astronomy Probe inside
5 Fe core ρ c ~10 10 g/cm 3 T c ~1 MeV ν ν- ρ c ~10 12 g/cm 3 T c ~2 MeV ν ν ν ν 1000 km ρ c ~3x10 14 g/cm 3 T c ~5 MeV ν ν ν ρ c ~4x10 14 g/cm 3 T c ~10 MeV ν ν ν Shockwave NS ~ 10 km NS T~0 MeV Y e <0.1
6 M Fe ~M NS ~ 1.4M solar, R Fe ~10 4 km R NS ~10 km ΔE Grav = GM 2 GM 2 ~ erg R Fe R NS E exp ~ erg E ν ~ erg Macrophysics Microphysics
7 多次元流体力学計算 超新星爆発多次元流体計算の例 2D calc with rotation Shen-EOS 超新星爆発残骸 形状, 元素合成, 偏光 中性子星キック 非対称性 球対称:1D (非)軸対称:2D, 3D 回転, 磁場 流体力学的不安定性 対流, 組成混合 Jun Wang 2002 Jan Kotake et al. ApJ 595 (2003) 304
8 / ν ν f(t,x,y,z,p x,p y,p z ) 6+1 ν ν ν ( ) / /
9 / ν ν f(t,x,y,z,p x,p y,p z ) 6+1 ν ν f(e ν f ν (E ν ) ν ( ) 1.0 ρ c =10 14 g/cm 3 & 0.8 bounce ρ c =10 12 / / ρ c = g/cm MeV 100 MeV 1000 E ν [MeV] ν energy
10 9 SciDAC Review Spring 2006
11 ν (ρ, T, Y e ) : ε, p, S, µ n, µ p, X i, m *, ρ ν
12 : σ ~ A 2 ν / : e - + p ν + n e - + A ν + A e + + n ν + p : ν i + N ν i + N ν i + A ν i + A ν i + e ν i + e : e - + e + ν e + ν e γ ν i + ν i N + N N + N + ν i ν i i=e, µ, τ
13 Lattimer-Swesty EOS (1991) Skyrme-Hartree-Fock approach Relativistic EOS (Shen-Oyamatsu-Toki-Sumiyoshi, 1998) Relativistic Mean Field approach Hyperon EOS (Ishizuka-Ohnishi, 2006) Variational Approach (Kanzawa-Takano, 2005~) - 3D Skyrme Hartree-Fock EOS (Newton, Stone Mezzacappa, 2007) A=460 A=1400 (n b =0.08 fm -3, T=2.5 MeV, Y p =0.3) Fuller, Fowler & Newman, Bruenn (1989) Langanke-Pinedo (45<A<112) T. Otsuka & T. Suzuki, Fujita-RCNP Reddy, Horowitz, Yamada-Toki,
14
15 EOS n,p,e ρ ρ0 21pSA T=0 EOS
16 Approaches to obtain the EOS approach starts from ingredients Theory/Model empirical the parametrized EOS nuclear mass, size,... Phenomenological effective NN int. nuclear mass, size,... Liquid-Drop Model Droplet Model Thomas-Fermi Theory... Skyrme HF RMF AMD... many-body bare NN int. (AV18, Bonn, Paris,...) NN scattering,... Variational Calc. DBHF...
17 SN-EOS for supernova simulations Empirical J.M. Lattimer, F.D. Swesty NPA535(1991). Phenomenological (RMF-TM1) H. Shen, H. Toki, K. Oyamatsu, K. Sumiyoshi, NPA637(1998), PTP100(1998). many-body (AV18) under construction (21pSA-11) H. Kanzawa, K. Oyamatsu, K. Sumiyoshi, M. Takano, NPA791(2007) Mukherjee, Pandharipande, Phys. Rev. C 75, (2007).
18 The Nuclear EOS for Supernova Simulations! based on the Realistic Nuclear Potential! H. Kanzawa a, K. Oyamatsu b, K. Sumiyoshi c and M. Takano a! a Waseda Univ., b Aichi Shukutoku Univ., c Numazu CT! 1) The uniform EOS: AV18+UIX,! Vatiational many-body calculations! 2) The Thomas-Fermi calculations for atomic nuclei reproduce their empirical data.! NPA791 (2007) 232! 3) The SN-EOS is under construction!
19 Hix (Proc. Nuclei in the Cosmos X to be published) Protoneutron star size 20% 200ms Shock location 20% lepton, entropy gradient g/cm 3 BH neutrino 21pSA9,10
20 (flux, spectra) : (40M solar ) Sumiyoshi et al., PRL (2006) ν ν Shen EOS ν 50 ν cf. Hyperon WW95: 40M solar ν 40 ν e ν e ν µ < E ν > [MeV] ν e ν e 10 Hyperon- 0.7 Shen- 1.3 ν time after bounce [sec] 1.5 Sumiyoshi, Yamada & Suzuki ApJ (2007) Sumiyoshi et al. (2008) in preparation
21 (Prakash) 0.5 ρ0 ρ0 GDR ρ0 2-3 ρ0 Heavy Ion Collision Bao et al., Phys. Rep.(2008) in press.(arxiv: ) ρ > 2-3 ρ0 Hyperon, Meson Condensate, Qurak Matter (
22 T=0 w n, x w 0 + K 0 18n 0 2 n n x 2 S 0 + L 3n 0 n n 0 ds( n) L = 3n 0 dn n=n0 S 0 = S( n ) 0
23 L, K0 EOS K. Oyamatsu and K. Iida, PTP 109, , 2003.
24 Efforts being done Estimate L value from global behavior of nuclear mass and size in nuclear chart with Prof. Iida (Kouchi U.), Drs. Kohama(RIKEN), Koura(JAEA), Abu-Ibrahim(Cairo U.) For nuclear size, we need to directly compare calculations and cross section measurements. Kurotama (Black sphere) model(21asb7) Glauber calculation of cross sections Preliminary result from nuclear mass L value is relatively large. (closer to EOS C than to EOS G)
25 (Shen EOS) Wigner-Seitz cell free n, p, α Thomas-Fermi
26
27 arxiv: v1 (astro-ph)
28 RMF calculation by Maruyama, Chiba, Tatsumi 12$&2($&*30&3*"$(%#(425"*!!"#$%&'()*+,-"$(%#(./(0"--! Pasta structures appear.! Y p =0.5! Y p =0.1!!!
29 QMD calculations by Sonoda, Watanabe, Sato, Takiwaki, Yasuoka, Ebisuzaki Pasta phases at zero temperature Cooling of Hot nuclear matter(~10 MeV) down to 0.1 MeV Snapshots calculated for model 2 Sphere Rod Slab 0.100! ! ! 0 Red!Proton Blue!Neutron! 0 =0.168 fm -3 "Nuclear density#! Rod-like Bubbles 0.490! 0 Spherical Bubbles 0.575! 0 14
30 Shen EOS table size log10 (T(MeV) ) 31 grids log10(yp) grids log10(ρb (g/cm3)) grids ,904 data points
31 EOS L / GDR K0 Heavy ion collision Nuclear Statistical Equilibrium Hartree-Fock RMF
32 hyperons, meson condensate, quark matter,...
33 EOS T, ρ, Yp Mega Grids nucastrodata.org, bigbangonline.org
1401_HPCI-lecture4.SNEOS.pptx
極限物質の性質を決めるには? 超新星 : 状態方程式データテーブル 中性子星と超新星の状態方程式 中性子星 密度のみの関数 ほぼ中性子物質 ゼロ温度 冷えた中性子星 多くの状態方程式 原子核実験 中性子星質量 半径 超新星 密度だけでなく 電子の割合が変わる 有限温度 超新星爆発時 少ないデータテーブル 数値シミュレーション 中性子星合体にも 極限状態での物質の性質 状態方程式 (Equation
PowerPoint Presentation
2010 KEK (Japan) (Japan) (Japan) Cheoun, Myun -ki Soongsil (Korea) Ryu,, Chung-Yoe Soongsil (Korea) 1. S.Reddy, M.Prakash and J.M. Lattimer, P.R.D58 #013009 (1998) Magnetar : ~ 10 15 G ~ 10 17 19 G (?)
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@ 2011.12.26 τ weak 1 σ weak n target v relative 8 10 8 sec ( T 10MeV ) 2 ( σ weak 4G2 F h2 c 2 π T 2, n target ρ m u, v relative c ( τ dyn 1 0.4msec Gρ ) 1/2 ρ 10 14 g/cm 3 ) 1 ρ 10 14 g/cm 3 (T 10MeV,
EOS and Collision Dynamics Energy of nuclear matter E(ρ, δ)/a = E(ρ, )/A + E sym (ρ)δ 2 δ = (ρ n ρ p )/ρ 1 6 E(ρ, ) (Symmetric matter ρ n = ρ p ) E sy
Nuclear collision dynamics and the equation of state We want to measure EOS. Measure T, P and ρ of matter... Prepare matter in the state we want to measure HI collisions What are taking place in collisions?
ニュートリノ駆動型 超新星爆発シミュレーション ３Ｄと２Ｄの比較
2016/01/05 宇宙の歴史をひもとく地下素粒子原子核研究 第二回超新星ニュートリノ研究会 ニュートリノ観測による超新星爆発メカニズムの探求 滝脇知也 ( 理化学研究所 ) 1 2 Three phases of supernovae Presupernova phase Burst phase Accretion phase Cooling phase Kato+2015 吉田敬さん石徹白さん
W 1983 W ± Z cm 10 cm 50 MeV TAC - ADC ADC [ (µs)] = [] (2.08 ± 0.36) 10 6 s 3 χ µ + µ 8 = (1.20 ± 0.1) 10 5 (Ge
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22 2 24 W 1983 W ± Z 0 3 10 cm 10 cm 50 MeV TAC - ADC 65000 18 ADC [ (µs)] = 0.0207[] 0.0151 (2.08 ± 0.36) 10 6 s 3 χ 2 2 1 20 µ + µ 8 = (1.20 ± 0.1) 10 5 (GeV) 2 G µ ( hc) 3 1 1 7 1.1.............................
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超新星爆発メカニズムの現状 固武慶 ( 国立天文台 ) 超新星爆発とニュートリノ原子核反応 阪大 RCNP 研究会 2007 年 2 月 目次及び時刻表 第 1 章 Introduction (~5 分 ) 第 2 章超新星の物理 (~5 分 ) (standard supernova scenario) 第 3 章超新星爆発メカニズム最前線 (~30 分 ) Asymmetry と爆発メカニズム
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天体プラズマにおける粒子加速機構 無衝突系粒子シミュレーション 星野真弘理学系研究科 地惑惑星科学専攻 内容 ** PIC (Particle In Cell) シミュレーション ** プラズマ輸送係数の研究 (MHD では現象論的に扱う粘性 電気抵抗 熱伝導に関わる物理 ) 非熱的プラズマ ( 局所的熱平衡ではない物理 ) 電子とイオンのエネルギー分配 宇宙での高エネルギー粒子の観測 数値チェレンコフ問題
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数値相対論シミュレーション 関口雄一郎 ( 京都大学基礎物理学研究所 ) 内容 数値相対論の概要 最近の研究成果 - アニメーションを中心にー 数値相対論とは? John von Neumann 非線形問題の解法として 高速電子計算機を用いる時代が必ず到来する 数値相対論のターゲット 強重力場の動的変動を伴う現象 ブラックホール形成の瞬間 大質量星の重力崩壊 コンパクト天体連星の合体, etc 重力波放出現象
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