diffuseγ-rays and antiprotons
DESCRIPTION
-. --- 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 ? ---. - PowerPoint PPT PresentationTRANSCRIPT
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Diffuseγ-rays and antiprotons
Toru ShibataAoyama-Gakuin Univ.
(14/Sep/2007)
--- Is there any signal of novel source inγ’s and/or p’s ? ----
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(I) Internal consistency in CR observables:
◎ 1-ry rich components (p, He, . . . Fe)
◎ 1-ry poor components (ultra-heavy elements)
◎ 2-ry stable components (Li, Be, B, . . . , )
◎ 2-ry unstable components (10Be, 26Al, . . . , )
◎ 1-ry electron components
(and in e+’s)
Modeling check of CR propagation
Estimation of Galactic parameters
--- Is there any signal of novel source inγ’s and/or p’s ? ----
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◎ consistent or not ?
(II) Comparison between γ’s, p’s, e+’s and other CRs-
◎ 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 . . . . . ?
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-1) emissivity at r
P ≡ p, He, . . . Fe ;
key inputs for the numerical approach toγ’s and p’s:-
S ≡γ, p
cosmic-ray density renormalized at SS
gas density
production cross-section
ApJ 2004, 2006, 2007
Astrop. Phys 2005 for p-p γ
Astrop. Phys in press for p-p -p
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2) intensity at SS
emissivity at r
structure function for
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: straightforward for gamma-rays
but slightly cumbersome for antiprotons
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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
p-p collision-
Astrop. Phys. in press
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rapidity distr
ibution by IS
R
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normalized CR density at SS
1) Energy spectra for 1-ry components
D ∝ vR
Q ∝ R-
2.7-2.8
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2) secondary-to-primary ratio
180 mbarn
10 g cm-2or
possibly reacceleration occurswith = 1/3, and
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Galactic plane
: halo thickness
isotope spread
◎ , normalized to
3) radionuclide abundance ratios
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Summary of Galactic parameters in our model expected from CR data nowadays available
◎
◎
◎
◎
◎
-How about γ’s and p’s ?compatible or imcompatible ?
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diffusive –rays (energy spectrum)
= 180 mbarn;
reacceleration with = 1/3,
the intensity is not affected bythe choices of these parametersas long as 1-ry-CR-fluxes at SSare normalized at 100 GeV/n
from spatial dist.
Astrop. Phys. 27(2007)411
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Boer, W. 2005 CERN COURIER45, 17
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Stecker, Hunter, & Kniffen, arXiv:0705.4311 [astro-ph]29, May 2007
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longitudinal distr
ibution
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latitudinal distr
ibution
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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 ~ βR0.5
Kraichnan q ~ R-2.2
q(R) steepens at < 40 GV, break of D(R) at 4 GV, too high anisotropy at > 10 TeV
D ~ βR0.3
Kolmogorov q ~ R-2.4
q(R) flattens at < 3 GV,
too low antiproton flux ?
Sina et al. 2001
flux of antiprotons; model parameters obtained from B/C ratio
Ptuskin Rapp.Talk at 2
9th IC
RR
problem in
antiproton sp
ectru
m
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novel source ?
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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
2) Revised EGRET data (E, l, b-dist) are in harmony with CR data, both in shape and absolute value for E < 10GeV
γ ~=> constraint for WIMPS (await GALST data)
3) BESS p data -
=> consistent with CR data for > 1GeV but not yet clear for < 1GeV (signal of PBH ?)
~
~
(await BESS-PPB, AMS02, PAMELA)
1) Diffusion + reacceleration with α=1/3 consistent with CR data (1-ry, 2-ry, isotope, e- ? )=>
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Thank you