Production spectrum of gamma rays in interstellar space through neutral pion decay

1981 ◽  
Vol 76 (1) ◽  
pp. 213-233 ◽  
Author(s):  
S. A. Stephens ◽  
G. D. Badhwar
Keyword(s):  
Gamma Rays ◽  
Neutral Pion ◽  
Interstellar Space ◽  
Pion Decay ◽  
Production Spectrum

scholarly journals Neutral pion decay intoνν¯in dense Skyrmion matter

2005 ◽  
Vol 71 (11) ◽  
Author(s):  
Alexander C. Kalloniatis ◽  
Jonathan D. Carroll ◽  
Byung-Yoon Park
Keyword(s):  
Neutral Pion ◽  
Pion Decay ◽  
Skyrmion Matter

Gamma rays from pion decay - Evidence for long-term trapping of particles in solar flares

1992 ◽  
Vol 396 ◽  
pp. L111 ◽  
Author(s):  
Natalie Mandzhavidze ◽  
Reuven Ramaty
Keyword(s):  
Gamma Rays ◽  
Solar Flares ◽  
Pion Decay

LOOKING FOR NEW SCALARS IN THE NEUTRAL PION DECAY

1991 ◽  
Vol 06 (02) ◽  
pp. 143-149
Author(s):  
M.I. DOBROLIUBOV
Keyword(s):  
Neutral Pion ◽  
Branching Ratio ◽  
Point Of View ◽  
Experimental Point ◽  
Pion Decay ◽  
Strong Enhancement

We found a strong enhancement of the rate of the decay of π0-meson into scalar and pseudoscalar bosons as compared with its decay into two photons. The branching ratio of this mode can be as large as BR(π0→S+P)≃10−6–10−5, which is very interesting from the experimental point of view.

THE CR CONNECTION(S): UHE NEUTRINOS AND PHOTONS FROM UHECR SOURCES

2009 ◽  
Vol 18 (10) ◽  
pp. 1571-1575
Author(s):  
ANDREW TAYLOR
Keyword(s):  
Radiation Field ◽  
Pion Production ◽  
Neutral Pion ◽  
Neutrino Flux ◽  
Photon Flux ◽  
Pion Decay ◽  
Cosmic Radio ◽  
Microwave Background ◽  
Radio Background ◽  
Nearby Source

During their acceleration, both UHECR nuclei and UHECR protons may interact with the radiation field present in the accelerator region leading to photo-disintegration and photo-pion production interactions respectively. This leads to a close connection between the degree of disintegration of UHECR nuclei and the UHE neutrino flux produced by a source. Upon escaping the accelerator, UHECR protons go on to generate a secondary UHE photon flux through photo-pion interactions with the cosmic microwave background (CMB) photons, These secondary UHE photons produced (via neutral pion decay) will themselves also interact with the cosmic radio background (CRB) photons. This leads to a second connection between UHE photons and nearby source of UHECR protons. We hear investigate both these connections to draw conclusions on what we can learn about UHECR sources.

The neutral-pion decay and the gamma radiation from our galaxy

1971 ◽  
Vol 2 (1) ◽  
pp. 77-92 ◽  
Author(s):  
G. Cavallo ◽  
R. J. Gould
Keyword(s):  
Gamma Radiation ◽  
Neutral Pion ◽  
Pion Decay

scholarly journals Connection between Neutral Pion Decay and Proton Compton Scattering

1960 ◽  
Vol 117 (3) ◽  
pp. 854-858 ◽  
Author(s):  
Maurice Jacob ◽  
Jon Mathews
Keyword(s):  
Compton Scattering ◽  
Neutral Pion ◽  
Pion Decay

Neutral pion decay

1958 ◽  
Vol 9 (3) ◽  
pp. 451-460 ◽  
Author(s):  
M. L. Goldberger ◽  
S. B. Treiman
Keyword(s):  
Neutral Pion ◽  
Pion Decay

Search for a light photino in neutral pion decay

1987 ◽  
Vol 192 (1-2) ◽  
pp. 135-137 ◽  
Author(s):  
M.I. Dobroliubov ◽  
A.Yu. Ignatiev ◽  
V.A. Matveev
Keyword(s):  
Neutral Pion ◽  
Pion Decay

scholarly journals Gamma Rays from Galaxy Clusters

1981 ◽  
Vol 94 ◽  
pp. 333-334
Author(s):  
M. Giler ◽  
J. Wdowczyk ◽  
A. W. Wolfendale
Keyword(s):  
Diffusion Coefficient ◽  
Cosmic Rays ◽  
Recent Work ◽  
Galaxy Clusters ◽  
Gamma Rays ◽  
Virgo Cluster ◽  
Clusters Of Galaxies ◽  
Production Spectrum ◽  
Γ Rays ◽  
Energy Dependent

In our recent work we have shown that a good model for the highest energy cosmic rays is one where they are generated in clusters of galaxies with a relatively flat production spectrum and then propagate with an energy dependent diffusion coefficient. There is evidence for a similar flat production spectrum (γ ≃ 2.1) for both protons and electrons in our own Galaxy. Here we assume that the spectrum for clusters (specifically the VIRGO cluster) is independent of energy and an evaluation is made of the likely flux of γ-rays.

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