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Diffuseγ-rays and antiprotons

-. --- 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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  1. - --- Is there any signal of novel source inγ’s and/or p’s ?--- Diffuseγ-rays and antiprotons Toru ShibataAoyama-Gakuin Univ. (14/Sep/2007)

  2. 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, . . . , )

  3. - (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,

  4. - 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

  5. emissivity atr structure function for 2) intensity at SS

  6. but slightly cumbersome for antiprotons : straightforward for gamma-rays

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

  8. cross-section for antiprotons in p-p collision Astrop. Phys. in press - p-p collision

  9. rapidity distribution by ISR

  10. normalized CR density atSS Q∝R-g D∝vRa 2.7-2.8 1) Energy spectra for 1-ry components

  11. 180 mbarn possibly reacceleration occurs with a= 1/3, and 10 g cm-2 or 2) secondary-to-primary ratio

  12. ◎, normalized to : halo thickness isotope spread Galactic plane 3) radionuclide abundance ratios

  13. ◎ ◎ ◎ ◎ - How about γ’s and p’s? compatible or imcompatible ? ◎ Summary of Galactic parameters in our model expected from CR data nowadays available

  14. 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

  15. Boer, W. 2005 CERN COURIER 45, 17

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

  17. longitudinal distribution

  18. latitudinal distribution

  19. 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

  20. novel source ?

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

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

  23. 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

  24. Thank you

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