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

2. Status of Galactic Cosmic-ray Observation
　 Observables:
◎ 1-ry nucleus(p,He,C, …)
◎ 2-ry nucleus(Li,Be,B, …)
◎ ultra heavy (Z　30)
◎ anti-proton, positron
◎ primary electron
◎ isotope(10Be, …,59Co, …)
◎ diffused gamma-rays
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

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

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

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

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

8. ：
(source) ● ～
: Kraichnan - type ●
: Kolmogorov- type ● :

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

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

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

12. z
line of sight γ y L l b
Earth x

13. Ⅲ-１］Proton-spectrum
Intensity at solar system

14. Relative proton intensity

15. Ⅲ-２］γ- ray production cross section
① 　　　　　　　　　　　　 ~ 1 GeV
：　　Bugg et al. (1964)
② 　10 ~ 300 GeV
：　　Jaeger et al. (1975)
③　 400 ~ 2000 GeV
：　　Neuhofer et al. (1972)