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Spectral Function Approach

Spectral Function Approach. 作田　誠　（岡山大学理）、 2012 年 12 月 18 日 @JPARC 理論研究会 1. 準弾性散乱断面積 2. NC QE+ 励起状態（ γ 線） : 超新星爆発、陽子崩壊、ニュートリノ振動実験 3. まとめ　. 1. Uniform Fermi-Gas and Spectral Function for Various Nuclei.

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Spectral Function Approach

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  1. Spectral Function Approach 作田　誠　（岡山大学理）、2012年12月18日 @JPARC 理論研究会 1. 準弾性散乱断面積 2. NC QE+励起状態（γ線）: • 超新星爆発、陽子崩壊、ニュートリノ振動実験 3. まとめ　

  2. 1. Uniform Fermi-Gas and Spectral Function for Various Nuclei Spectral Functions P(p,E) for various nuclei, eg.16O, are estimated by Benhar et al. using e-N data and the calculation. P(p,E) : Probability of removing a nucleon of momentum p from ground state leaving the residual nucleus with excitation energy E. E (MeV) Fermi momemtum 30% 40. 20. Fermi Gas model 0. 100. 200. P (MeV/c) p

  3. Electron-nucleus scattering • Benhar, MS et al., PRD72,’05;H.Nakamura,MS et al.,PRC76, 065208 (2007). 単色E=880 MeVのニュートリノを酸素に当てて、32度のニュートリノのエネルギーを測れるとすると（相対的な大きさを除き）同様なスペクトルが見えるはず。原子核効果を含むVector current 部分の精密な検証が可能。 準弾性 16O(e,e’), Ee=880MeV, q=32° 実験データ 準弾性(SP)+MAID(SP) 準弾性(FG)+MAID(FG) 準弾性(SP)+Paschos(SP) 境界 D共鳴 エネルギー移行w=Ee-Ee’ (MeV)

  4. Results from NuInt-Quantitative comparison of calculation and data- Quasi-Elastic is understood to 10% for E=700MeV-2000MeV (and Q2>0.2 (GeV/c)2) Reference=Relativistic Fermi-Gas model (Smith-Moniz) Spectral Function S(p,E): validated by JLAB E97-001 Final state interaction: validated by JLAB E97-001 1p (D) production Sato-Lee,Lalakulich Understood to 20-30%? DIS (Kumano et al.) New data H,D,C(e,e’) at Low Q2 are coming soon. これで解決と思っていたが、2009年から新たな問題。

  5. MiniBooNE異常(2009)から混乱状態 • 実験が核子(p,n)を見ているか、2Nに感じているか、何も見ていないか。 • MEC, 2p2h, FSI の議論が始まった。 • NuInt2011 (March 7-11,2011) もこの議論のみ。 • 原子核物理で20年未解決の問題。2年かかるだろう。 • Nieves et al., PRC83,045501,2011 • Meucci et al., PRL107,172501,2011 • Amaro et al.,PRD84,033004,2011 • ………

  6. 2. Importance ofg rays in NC n-O or n-C interactions This process is very important to both Supernova (SN) physics and neutrino oscillation experiments. 1) SN Detection • Supernova neutrino bursts in Our Galaxy: The events containing g rays from NC n-O (n-C) interactions comprise 5-10% of the total events. They will give us flux (Temperature), independent of the neutrino oscillations. • Supernova Relic Neutrino (SRN) detection: Though we are about to reach the sensitivity to SRN, the g-rays from Atmospheric NC n-O (n-C) interactions at high energy may make serious background in 5-20 MeV region. 2) Neutrino Oscilation Experiments at Beam Dump or LBNE • BD: KARMEN experiment measured the 15.1MeV g rays from NC n-C reactions at 29.8MeV. No experiments exist for oxygen at low energy. • LBNE: The number of g-ray events from NC n-A interaction is independent of neutrino oscillations.

  7. arXiv:1110.0679[nucl-th] • To appear in Phys.Rev.Lett.

  8. En>200MeV: NC QE process producing g-raysn+O n+n+15O*, n+p+15N*- -Ejiri, PRC48,1442 (1993). 30MeV 1p1/2 26.8 25.5 25MeV 1p3/2 24.8 1s1/2 30MeV proton neutron 29.0 20MeV 28.0 7.34 7.03 8.18 7.55 7.01 6.45 6.90 6.20 25MeV 5.83 6.73 5.69 6.59 5.11 4.92 Sp=4.63 6.09 1p1/2 15MeV 3.95 20MeV 5.17 2.31 4.63 s1/2 s1/2 7.03 1p3/2 6.45 7.55 15MeV 6.20 10.8 5.83 13.2 g.s. 10.2 14N+n 10MeV 5.69 14C+p 5.11 14O+n 1s1/2 4.92 3.95 10MeV 2.31 9.93 P3/2 proton neutron 6.18 P3/2 7.30 6.32 P3/2 5.30 14N+p 5.27 5MeV 5.18 5MeV 0 0 15O 15N

  9. まとめ • QE, QE+γ線放射の簡単な記述の紹介をした • まずは、共通のモデル--Web • Sato-Lee モデルを基本にする。 • それにSpectral Function 加える。 • DIS は熊野さんのモデル。 • 2p-2h　－未解決

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