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宇宙線スペクトルと GeV-TeV diffuse-g emission

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Presentation on theme: "宇宙線スペクトルと GeV-TeV diffuse-g emission"— Presentation transcript:

1 宇宙線スペクトルと GeV-TeV diffuse-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 Particle physics & Cosmology
(II) Comparison between γ’s, e∓’s, p’s and other CRs - ◎ consistent or not ? ◎ 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 ?    Particle physics & Cosmology

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

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

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

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9 ii) cross-section production cross-section

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

11 iii) normalization cosmic-ray density renormalized at SS

12 1) energy spectra for 1-ry components
normalized CR density at SS Q ∝ R-g D ∝ vRa a = 0.3, g = ? or a = 0.6, g = ?

13 contribution of CR’s other than proton

14 2) secondary-to-primary ratios 

15 3) antiproton-to-proton ratio 

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

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

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

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21 diffuse-g emission in GeV-TeV region
[1] extra-galactic g ’s  [2] hadron-induced g ’s   [3] electron-induced g ’s  

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28 (preliminary)


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