Diffuse rays and antiprotons
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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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Diffuseγ-rays and antiprotons

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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)


Diffuse rays and antiprotons

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, . . . , )


Diffuse rays and antiprotons

-

(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,


Diffuse rays and antiprotons

-

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


Diffuse rays and antiprotons

emissivity atr

structure function for

2) intensity at SS


Diffuse rays and antiprotons

but slightly cumbersome for antiprotons

: straightforward for gamma-rays


Diffuse rays and antiprotons

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

Astrop. Phys. 23(2005)510


Diffuse rays and antiprotons

cross-section for antiprotons in p-p collision

Astrop. Phys. in press

-

p-p collision


Diffuse rays and antiprotons

rapidity distribution by ISR


Diffuse rays and antiprotons

normalized CR density atSS

Q∝R-g

D∝vRa

2.7-2.8

1) Energy spectra for 1-ry components


Diffuse rays and antiprotons

180 mbarn

possibly reacceleration occurs

with a= 1/3, and

10 g cm-2

or

2) secondary-to-primary ratio


Diffuse rays and antiprotons

◎, normalized to

: halo thickness

isotope spread

Galactic plane

3) radionuclide abundance ratios


Diffuse rays and antiprotons

-

How about γ’s and p’s?

compatible or imcompatible ?

Summary of Galactic parameters in our model

expected from CR data nowadays available


Diffuse rays and antiprotons

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


Diffuse rays and antiprotons

Boer, W. 2005

CERN COURIER

45, 17


Diffuse rays and antiprotons

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


Diffuse rays and antiprotons

longitudinal distribution


Diffuse rays and antiprotons

latitudinal distribution


Diffuse rays and antiprotons

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


Diffuse rays and antiprotons

novel source ?


Diffuse rays and antiprotons

Tang & Ng (1983)

Duperray et al. (2003)


Diffuse rays and antiprotons

Tang & Ng (1983)

Duperray et al. (2003)


Diffuse rays and antiprotons

  • Diffusion + reacceleration with α=1/3

  • consistent with CR data (1-ry, 2-ry, isotope, e- ? )

=>

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


Diffuse rays and antiprotons

Thank you


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