Diffuseγ-rays and antiprotons

Diffuseγ-rays and antiprotons

Toru ShibataAoyama-Gakuin Univ.

(14/Sep/2007)

--- Is there any signal of novel source inγ’s and/or p’s ? ----

(I) Internal consistency in CR observables:

◎ 1-ry rich components (p, He, . . . Fe)

◎ 1-ry poor components (ultra-heavy elements)

◎ 2-ry stable components (Li, Be, B, . . . , )

◎ 2-ry unstable components (10Be, 26Al, . . . , )

◎ 1-ry electron components

(and in e+’s)

Modeling check of CR propagation

Estimation of Galactic parameters

--- Is there any signal of novel source inγ’s and/or p’s ? ----

◎ consistent or not ?

(II) Comparison between γ’s, p’s, e+’s and other CRs-

◎ 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 . . . . . ? 　　　

-1) emissivity at r

P ≡ p, He, . . . Fe ;

key inputs for the numerical approach toγ’s and p’s:-

S ≡γ, p

cosmic-ray density renormalized at SS

gas density

production cross-section

ApJ 2004, 2006, 2007

Astrop. Phys 2005 for p-p γ

Astrop. Phys in press for p-p -p

2) intensity at SS

emissivity at r

structure function for

　　　　　　　　　　 : straightforward for gamma-rays

but slightly cumbersome for antiprotons

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

cross-section for antiprotons in p-p collision

p-p collision-

Astrop. Phys. in press

rapidity distr

ibution by IS

R

normalized CR density at SS

1) Energy spectra for 1-ry components

D 　∝　 vR

Q 　∝　 R-

2.7-2.8

2) secondary-to-primary ratio

180 mbarn

10 g cm-2or

possibly reacceleration occurswith = 1/3, and

Galactic plane

: halo thickness

isotope spread

◎ 　 　　 , normalized to

3) radionuclide abundance ratios

Summary of Galactic parameters in our model expected from CR data nowadays available

◎

◎

◎

◎

◎

-How about γ’s and p’s ?compatible or imcompatible ?

diffusive –rays (energy spectrum)

＝ 180 mbarn;

reacceleration with = 1/3,

the intensity is not affected bythe choices of these parametersas long as 1-ry-CR-fluxes at SSare normalized at 100 GeV/n

from spatial dist.

Astrop. Phys. 27(2007)411

Boer, W. 2005 CERN COURIER45, 17

Stecker, Hunter, & Kniffen, arXiv:0705.4311 [astro-ph]29, May 2007

longitudinal distr

ibution

latitudinal distr

ibution

popular versions of empirical propagation model with no Galactic wind

plain diffusion diffusion + reacceleration (Va ≠ 0)

diffusion coefficient spectrum of turbulence source spectrum

features

problems

D ~ βR0.5

Kraichnan q ~ R-2.2

q(R) steepens at < 40 GV, break of D(R) at 4 GV, too high anisotropy at > 10 TeV

D ~ βR0.3

Kolmogorov q ~ R-2.4

q(R) flattens at < 3 GV,

too low antiproton flux ?

Sina et al. 2001

flux of antiprotons; model parameters obtained from B/C ratio

Ptuskin Rapp.Talk at 2

9th IC

RR

problem in

antiproton sp

ectru

m

novel source ?

Tang & Ng (1983) Duperray et al. (2003)

Tang & Ng (1983) Duperray et al. (2003)

Summary

2) Revised EGRET data (E, l, b-dist) are in harmony with CR data, both in shape and absolute value for E < 10GeV

γ ～=> constraint for WIMPS (await GALST data)

3) BESS p data -

=> consistent with CR data for > 1GeV but not yet clear for < 1GeV (signal of PBH ?)

～

～

(await BESS-PPB, AMS02, PAMELA)

1) Diffusion + reacceleration with α=1/3 consistent with CR data (1-ry, 2-ry, isotope, e- ? )=>

Thank you