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Novel Sources in Cosmic Rays: Observables and Propagation Estimation in Galactic Parameters

Explore signals of novel sources in cosmic rays through internal consistency checks, comparison of different cosmic ray components, and modeling checks of cosmic ray propagation, estimating Galactic parameters. Analyze uncertainties, data quality, astronomical and extragalactic origins, and key inputs for numerical approach. Delve into energy spectra, secondary-to-primary ratios, antiproton-to-proton ratios, and difficulty in electron components’ energy loss, in relation to GeV-TeV diffuse gamma-ray emission and other cosmic ray phenomena.

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Novel Sources in Cosmic Rays: Observables and Propagation Estimation in Galactic Parameters

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  1. 宇宙線スペクトルとGeV-TeVdiffuse-g emission 柴田　　徹 (青学大理工) 09/Jan/’10

  2. - --- Is there any signal of novel source in γ’s, e∓’s and p’s ?--- (I) Internal consistency in CR observables: ◎1-ry rich components (p, He, . . . Fe) ◎1-ry poor components (ultra-heavy elements) ◎1-ry (poor) electron components ◎2-ry stable components (Li, Be, B, . . . , ) ◎2-ry unstable components (10Be, 26Al, . . . , ) modeling check of CR propagation estimation of Galactic parameters Astrophysics

  3. - (II) Comparison betweenγ’s, e∓’s, p’s and 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, Particle physics & Cosmology

  4. - key inputs for the numerical approach to γ’sand p’s: 1) emissivity at r from astronomical origin - P ≡ p, He, . . . Fe; e S ≡ γ, p cosmic-raydensity renormalized at SS gas density, or photon density production cross-section

  5. 2) intensity at SS emissivity atr’ structure function for Astronomical origin or cosmological one ?

  6. i) ISM, ISRF gas density, or photon density

  7. ii) cross-section production cross-section

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

  9. iii) normalization cosmic-raydensity renormalized at SS

  10. normalized CR density atSS 1) energy spectra for 1-ry components Q∝R-g D∝vRa 2.7-2.8 a= 0.3, g = 2.4-2.5 ? or a = 0.6, g = 2.1-2.2 ?

  11. contribution of CR’s other than proton

  12. 2) secondary-to-primary ratios

  13. 3) antiproton-to-proton ratio

  14. ◎, normalized to : halo thickness isotope spread Galactic plane 4) radionuclide abundance ratios note 15-20% uncertainty in s-frag.

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

  16. difficulty in electron components total energy-loss of electrons in ISM and ISRF: ISM ISRF

  17. diffuse-g emissionin GeV-TeV region [1] extra-galactic g’s [2] hadron-induced g’s [3] electron-induced g’s

  18. (preliminary)

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