Diffuse {gamma} rays and p flux from dark matter annihilation: A model for consistent results with EGRET and cosmic ray data

Journal Article · Fri Aug 15 00:00:00 EDT 2008 · Physical Review. D, Particles Fields

DOI:https://doi.org/10.1103/PHYSREVD.78.043001· OSTI ID:21250444

Xiaojun, Bi ^[1]; Juan, Zhang; Qiang, Yuan ^[1]

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1. Key laboratory of particle astrophysics, IHEP, Chinese Academy of Sciences, Beijing 100049 (China)

In this work we develop a new propagation model for the Galactic cosmic rays based on the GALPROP code, including contributions from dark matter annihilation. Its predictions of the Galactic diffuse {gamma}-ray spectra are compatible with the EGRET data in all sky regions. It also gives consistent results about the diffuse {gamma} ray longitude and latitude distributions. The B/C, {sup 10}Be/{sup 9}Be, proton, electron and antiproton spectra are in agreement with cosmic ray measurements as well. In this model we have taken a universal proton spectrum throughout the Galaxy without introducing large fluctuation, considering the proton energy loss is negligible. The dark matter annihilation signals are boosted after taking the contributions from subhalos into account. Another interesting feature of this model is that it gives a better description of the diffuse {gamma} rays when taking the source distribution compatible with supernova remnants data, which is different from previous studies.

• OSTI ID: 21250444
• Journal Information: Physical Review. D, Particles Fields, Vol. 78, Issue 4; Other Information: DOI: 10.1103/PhysRevD.78.043001; (c) 2008 The American Physical Society; Country of input: International Atomic Energy Agency (IAEA); ISSN 0556-2821
• Country of Publication: United States
• Language: English

Related Subjects

79 ASTROPHYSICS
COSMOLOGY AND ASTRONOMY
99 GENERAL AND MISCELLANEOUS//MATHEMATICS, COMPUTING, AND INFORMATION SCIENCE
ANNIHILATION
ANTIPROTONS
BERYLLIUM 10
BERYLLIUM 9
COSMIC RADIATION
DISTRIBUTION
ELECTRONS
ENERGY LOSSES
FLUCTUATIONS
FORECASTING
GALAXIES
GAMMA RADIATION
GAMMA SPECTRA
ISOTOPE RATIO
NONLUMINOUS MATTER
PROTON SPECTRA
SIMULATION
SUPERNOVA REMNANTS
WAVE PROPAGATION