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-. --- Is there any signal of novel source inγ’s and/or p’s ? ---. Diffuseγ-rays and antiprotons. Toru Shibata Aoyama-Gakuin Univ. ( 14/Sep/2007 ). Modeling check of CR propagation. Estimation of Galactic parameters. -. --- Is there any signal of novel source in γ’s and/or p’s ? ---.

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Diffuse rays and antiprotons

-

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

Diffuseγ-rays and antiprotons

Toru ShibataAoyama-Gakuin Univ.

(14/Sep/2007)


Modeling check of CR propagation

Estimation ofGalactic parameters

-

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

(and ine+’s)

(I) Internal consistency in CR observables:

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

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

◎1-ry electron components

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

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


-

(II) Comparison betweenγ’s,p’s, e+’sand other CRs

● how about the uncertainty in calculations ?

● how about the data quality in ⊿E,σ ?

N

● how much enhanced from those expected ?

● how about an astronomical origin ?

● how about an extragalactic contribution ?

● how about . . . . . ?

◎consistent or not ?

◎if not,


-

key inputs for the numerical approach toγ’sand p’s:

cosmic-raydensity

renormalized at SS

gas density

ApJ 2004, 2006, 2007

production cross-section

1) emissivity at r

-

P ≡ p, He, . . . Fe;

S ≡γ, p

Astrop. Phys 2005 for p-p

γ

-

Astrop. Phys in press for p-p

p


emissivity atr

structure function for

2) intensity at SS


but slightly cumbersome for antiprotons

: straightforward for gamma-rays


cross-section for gamma-rays in p-p collision

Astrop. Phys. 23(2005)510


cross-section for antiprotons in p-p collision

Astrop. Phys. in press

-

p-p collision



normalized CR density atSS

Q∝R-g

D∝vRa

2.7-2.8

1) Energy spectra for 1-ry components


180 mbarn

possibly reacceleration occurs

with a= 1/3, and

10 g cm-2

or

2) secondary-to-primary ratio


, normalized to

: halo thickness

isotope spread

Galactic plane

3) radionuclide abundance ratios


-

How about γ’s and p’s?

compatible or imcompatible ?

Summary of Galactic parameters in our model

expected from CR data nowadays available


from spatial dist.

=180 mbarn;

reacceleration with

a=1/3,

the intensity is not affected by

the choices of these parameters

as long as 1-ry-CR-fluxes at SS

are normalized at 100 GeV/n

diffusive g–rays (energy spectrum)

Astrop. Phys. 27(2007)411


Boer, W. 2005

CERN COURIER

45, 17





popular versions of empirical propagation model with no Galactic wind

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

Sina et al. 2001

Ptuskin Rapp.Talk at 29th ICRR

problem in antiproton spectrum


novel source ? Galactic wind


Tang & Ng (1983) Galactic wind

Duperray et al. (2003)


Tang & Ng (1983) Galactic wind

Duperray et al. (2003)


=>

2) Revised EGRET data (E, l,b-dist) arein harmony with

CR data, both in shape and absolute value forE< 10GeV

γ

=>constraint for WIMPS

(await GALST data)

-

3) BESSp data

=> consistent with CR data for > 1GeV

but not yet clear for < 1GeV (signal of PBH ?)

(await BESS-PPB, AMS02, PAMELA)

Summary


Thank you Galactic wind


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