「 Cosmic-rays and diffused gamma-rays 」

Is the diffused γ-ray data in harmony with the cosmic-ray data ? 「Cosmic-rays and diffused gamma-rays」 Aoyama-gakuin University T. Shibata

Status of Galactic Cosmic-ray Observation physics: origin, source, accel. limit path length, anisotropy r-process, s-process, source spectrum 2-ry products + novel sources nearby source C.R. life time, accel. period C.R. density, gas density, novel source Observables: ◎ 1-ry nucleus(p,He,C, …) ◎ 2-ry nucleus(Li,Be,B, …) ◎ ultra heavy (Z30) ◎ anti-proton, positron ◎ primary electron ◎ isotope(10Be, …,59Co, …) ◎ diffused gamma-rays

( 一定 ) 2hh 2hg ( 一定 ) ( 一定 ) Ginzburg-Ptuskinの銀河モデル（１９７６、１９９０） Dh : 拡散係数 halo nh : ガス密度 Dg : 拡散係数 disk ng : ガス密度 ( a fewkpc?) ～ (300pc) ～ Dh : 拡散係数　 halo nh ガス密度　 : 2R (30kpc) ～

Propagation of Cosmic-rays in Our Galaxy ×：source r0(r0,z0) ●：solar systemr(r 10kpc,z 0)

● Boundaryless Galaxy : r |z| →∞ →∞ Ⅰ］Our Model ● Gas density : ● Diffusion coefficient : with ● Source density : with

Ⅱ］Important parameters ● average scale height : Longitudinal dist. of diff. γ ● average scale height : Latitudinal dist. of diff. γ

: : ● : ： (source) ● ～ : Kraichnan - type ● : Kolmogorov- type

( ) average path length ● ( ) for R = 1 GVat G.C. : 銀河中心でのガス密度 for : 拡散係数のscale height

( ) ● : life time of unstable nuclei ( ) for R = 1 GVat G.C. for : 拡散係数のscale height for

Ⅲ］Gamma-raySpectrum ∫ ∫ Proton density γ ray prod. prob.

z line of sight γ 0 y L l b Earth x

Intensity at solar system Ⅲ-１］Proton-spectrum

Relative proton intensity

Ⅲ-２］γ- ray production cross section ① ~ 1 GeV ：　　Bugg et al. (1964) ：　　Jaeger et al. (1975) ②10 ~ 300 GeV ：　　Neuhofer et al. (1972) ③400 ~ 2000 GeV

「 Cosmic-rays and diffused gamma-rays 」