Diffuse?-rays and antiprotons

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Diffuse?-rays and antiprotons
Toru ShibataAoyama-Gakuin Univ.
(14/Sep/2007)
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--- Is there any signal of novel source in?痴
and/or p痴 ? ---
(and in e痴)
(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, . . . , )
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? consistent or not ?
? if not,
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1) emissivity at r
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P p, He, . . . Fe
S ?, p
Astrop. Phys 2005 for p-p
?
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Astrop. Phys in press for p-p
p
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2) intensity at SS
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straightforward for gamma-rays
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cross-section for gamma-rays in p-p collision
Astrop. Phys. 23(2005)510
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cross-section for antiprotons in p-p collision
Astrop. Phys. in press
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p-p collision
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rapidity distribution by ISR
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1) Energy spectra for 1-ry components
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2) secondary-to-primary ratio
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3) radionuclide abundance ratios
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Summary of Galactic parameters in our model
expected from CR data nowadays available
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diffusive g 睦ays (energy spectrum)
Astrop. Phys. 27(2007)411
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Boer, W. 2005 CERN COURIER 45, 17
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Stecker, Hunter, Kniffen, arXiv0705.4311
astro-ph29, May 2007
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longitudinal distribution
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latitudinal distribution
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popular versions of empirical propagation model
with no Galactic wind
plain diffusion diffusion reacceleration (Va ? 0)
diffusion coefficient spectrum of turbulence source spectrum features problems D ﾟR0.5 Kraichnan q R-2.2 q(R) steepens at lt 40 GV, break of D(R) at 4 GV, too high anisotropy at gt 10 TeV D ﾟR0.3 Kolmogorov q R-2.4 q(R) flattens at lt 3 GV, too low antiproton flux ?
flux of antiprotons model parameters obtained
from B/C ratio
Sina et al. 2001
Ptuskin Rapp.Talk at 29th ICRR
problem in antiproton spectrum
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Tang Ng (1983)
Duperray et al. (2003)
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Tang Ng (1983)
Duperray et al. (2003)
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Summary
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Thank you