-. --- 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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--- Is there any signal of novel source inγ’s and/or p’s ?---Diffuseγ-rays and antiprotons
Toru ShibataAoyama-Gakuin Univ.
Estimation ofGalactic parameters
--- Is there any signal of novel source inγ’sand/or p’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, . . . , )
(II) Comparison betweenγ’s,p’s, e+’sand other CRs
● how about the uncertainty in calculations ?
● how about the data quality in ⊿E,σ ?
● how much enhanced from those expected ?
● how about an astronomical origin ?
● how about an extragalactic contribution ?
● how about . . . . . ?
◎consistent or not ?
key inputs for the numerical approach toγ’sand p’s:
renormalized at SS
ApJ 2004, 2006, 2007
1) emissivity at r
P ≡ p, He, . . . Fe;
S ≡γ, p
Astrop. Phys 2005 for p-p
Astrop. Phys in press for p-p
structure function for
2) intensity at SS
: straightforward for gamma-rays
cross-section for gamma-rays in p-p collision
Astrop. Phys. 23(2005)510
cross-section for antiprotons in p-p collision
Astrop. Phys. in press
1) Energy spectra for 1-ry components
possibly reacceleration occurs
with a= 1/3, and
10 g cm-2
2) secondary-to-primary ratio
◎, normalized to
: halo thickness
3) radionuclide abundance ratios
How about γ’s and p’s?
compatible or imcompatible ?
Summary of Galactic parameters in our model
expected from CR data nowadays available
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
longitudinal distribution May 2007
latitudinal distribution May 2007
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
novel source ? Galactic wind
2) Revised EGRET data (E, l,b-dist) arein harmony with
CR data, both in shape and absolute value forE< 10GeV
=>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)
Thank you Galactic wind