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宇宙線スペクトルと GeV-TeV diffuse - g emission

宇宙線スペクトルと GeV-TeV diffuse - g emission. 柴田　　徹 ( 青学大理工 ). 09/Jan/’10. -. --- Is there any signal of novel source in γ’s, e ∓ ’s and p’s ? ---. (I) Internal consistency in CR observables:. ◎ 1-ry rich components (p, He, . . . Fe). ◎ 1-ry poor components (ultra-heavy elements).

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宇宙線スペクトルと GeV-TeV diffuse - g emission

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  1. 宇宙線スペクトルとGeV-TeVdiffuse-g emission 柴田　　徹 (青学大理工) 09/Jan/’10

  2. - --- Is there any signal of novel source in γ’s, e∓’s and p’s ?--- (I) Internal consistency in CR observables: ◎1-ry rich components (p, He, . . . Fe) ◎1-ry poor components (ultra-heavy elements) ◎1-ry (poor) electron components ◎2-ry stable components (Li, Be, B, . . . , ) ◎2-ry unstable components (10Be, 26Al, . . . , ) modeling check of CR propagation estimation of Galactic parameters Astrophysics

  3. - (II) Comparison betweenγ’s, e∓’s, p’s and other CRs ● how about the uncertainty in calculations ? ● how about the data quality in ⊿E,σ? N ● how much enhanced from those expected ? ● how about an astronomical origin ? ● how about an extragalactic contribution ? ● how about . . . . . ? ◎consistent or not ? ◎if not, Particle physics & Cosmology

  4. - key inputs for the numerical approach to γ’sand p’s: 1) emissivity at r from astronomical origin - P ≡ p, He, . . . Fe; e S ≡ γ, p cosmic-raydensity renormalized at SS gas density, or photon density production cross-section

  5. 2) intensity at SS emissivity atr’ structure function for Astronomical origin or cosmological one ?

  6. i) ISM, ISRF gas density, or photon density

  7. ii) cross-section production cross-section

  8. cross-section for g-rays in p-p collision Astrop. Phys. 23(2005)510

  9. iii) normalization cosmic-raydensity renormalized at SS

  10. normalized CR density atSS 1) energy spectra for 1-ry components Q∝R-g D∝vRa 2.7-2.8 a= 0.3, g = 2.4-2.5 ? or a = 0.6, g = 2.1-2.2 ?

  11. contribution of CR’s other than proton

  12. 2) secondary-to-primary ratios

  13. 3) antiproton-to-proton ratio

  14. ◎, normalized to : halo thickness isotope spread Galactic plane 4) radionuclide abundance ratios note 15-20% uncertainty in s-frag.

  15. ◎ ◎ ◎ - How about γ’s and p’s? compatible or incompatible ? ◎ Summary of Galactic parameters in our model expected from CR data nowadays available ◎

  16. difficulty in electron components total energy-loss of electrons in ISM and ISRF: ISM ISRF

  17. diffuse-g emissionin GeV-TeV region [1] extra-galactic g’s [2] hadron-induced g’s [3] electron-induced g’s

  18. (preliminary)

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