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) ◎ 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

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

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

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

i) ISM, ISRF gas density, or photon density

ii) cross-section production cross-section

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

iii) normalization cosmic-ray density renormalized at SS

1) energy spectra for 1-ry components normalized CR density at SS 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 ?

contribution of CR’s other than proton

2) secondary-to-primary ratios　

3) antiproton-to-proton ratio　

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

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

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

diffuse-g emission in GeV-TeV region [1] extra-galactic g ’s　 [2] hadron-induced g ’s 　 [3] electron-induced g ’s 　

(preliminary)