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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
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- --- 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
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Particle physics & Cosmology
(II) Comparison between γ’s, e∓’s, p’s and other CRs - ◎ consistent or not ? ◎ if not, ● how much enhanced from those expected ? ● how about an astronomical origin ? ● how about an extragalactic contribution ? ● how about the uncertainty in calculations ? ● how about the data quality in ⊿E, σ ? N ● how about ? Particle physics & Cosmology
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key inputs for the numerical approach to γ’s and p’s: -
1) emissivity at r from astronomical origin - P ≡ p, He, Fe ; e S ≡ γ, p cosmic-ray density renormalized at SS gas density, or photon density production cross-section
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Astronomical origin or cosmological one ?
2) intensity at SS emissivity at r’ Astronomical origin or cosmological one ? structure function for
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i) ISM, ISRF gas density, or photon density
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ii) cross-section production cross-section
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cross-section for g-rays in p-p collision
Astrop. Phys. 23(2005)510
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iii) normalization cosmic-ray density renormalized at SS
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1) energy spectra for 1-ry components
normalized CR density at SS Q ∝ R-g D ∝ vRa a = 0.3, g = ? or a = 0.6, g = ?
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contribution of CR’s other than proton
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2) secondary-to-primary ratios
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3) antiproton-to-proton ratio
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4) radionuclide abundance ratios
Galactic plane : halo thickness isotope spread ◎ , normalized to note 15-20% uncertainty in s-frag.
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Summary of Galactic parameters in our model
expected from CR data nowadays available ◎ ◎ ◎ ◎ ◎ - How about γ’s and p’s ? compatible or incompatible ?
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difficulty in electron components
total energy-loss of electrons in ISM and ISRF: ISM ISRF
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diffuse-g emission in GeV-TeV region
[1] extra-galactic g ’s [2] hadron-induced g ’s [3] electron-induced g ’s
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(preliminary)
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