DARK MATTER CANDIDATES IN LEFT-RIGHT SYMMETRIC MODELS

2011 ◽  
Vol 20 (08) ◽  
pp. 1389-1397 ◽  
Author(s):  
WAN-LEI GUO ◽  
YUE-LIANG WU ◽  
YU-FENG ZHOU
Keyword(s):  
Dark Matter ◽  
Gamma Rays ◽  
Cosmic Ray ◽  
High Energy ◽  
Muon Flux ◽  
Symmetric Model ◽  
Internal Bremsstrahlung ◽  
Energy Gamma ◽  
Charged Leptons ◽  
Bremsstrahlung Process

We discuss an extended left-right symmetric model in which the decay of DM particle is induced by tiny soft charge-conjugation violating interactions, and calculate the spectra for cosmic-ray positrons, neutrinos and gamma-rays. The DM signals in the flux of high energy neutrinos can be significantly enhanced, as the triplets couple to both charged leptons and neutrinos. The predicted neutrino-induced muon flux can be several times larger than the case in which DM particle only directly decays into charged leptons. In addition, the charged components of the triplet give extra contributions to the high energy gamma-rays through internal bremsstrahlung process.

Diffuse Gamma Rays of Galactic and Extragalactic Origin: Preliminary Results from EGRET

1996 ◽  
Vol 168 ◽  
pp. 279-288
Author(s):  
P. Sreekumar ◽  
D.A. Kniffen
Keyword(s):  
Gamma Rays ◽  
Gamma Ray ◽  
Cosmic Ray ◽  
High Energy ◽  
Emission Model ◽  
Diffuse Emission ◽  
Interstellar Gas ◽  
Cosmic Ray Interactions ◽  
Galactic Model ◽  
Energy Gamma

The all-sky survey in high energy gamma rays (E>30 MeV) carried out by the Energetic Gamma Ray Experiment Telescope (EGRET) aboard the Compton Gamma Ray Observatory provides for the first time an opportunity to examine in detail diffuse gamma-ray emission of extra-galactic origin. The observed diffuse emission at high galactic latitudes is generally assumed to have a galactic component arising from cosmic-ray interactions with the local interstellar gas and radiation, in addition to an isotropic component presumably of extragalactic origin. The galactic component can be estimated from a model of the interstellar medium and cosmic-ray distribution. Since the derived extragalactic spectrum depends very much on the success of our galactic model, the consistency of the galactic diffuse emission model is examined both spectrally and spatially with existing EGRET observations. In conjunction with this model, EGRET observations of the high latitude emission are used to examine the flux and spectrum of the residual extragalactic emission. This residual emission could be either truly diffuse in origin or could arise from accumulated emission from unresolved sources particularly in the light of EGRET observations showing the presence of numerous gamma-ray bright active galactic nuclei.

scholarly journals SEARCH FOR DARK MATTER WITH GAMMA-RAYS: A REVIEW

2013 ◽  
Vol 53 (A) ◽  
pp. 545-549 ◽  
Author(s):  
Aldo Morselli
Keyword(s):  
Dark Matter ◽  
Energy Range ◽  
Gamma Rays ◽  
Gamma Ray ◽  
High Energy ◽  
Space Telescope ◽  
High Energy Gamma ◽  
Astrophysical Objects ◽  
Energy Gamma

Successfully launched in June 2008, the Fermi Gamma-ray Space Telescope, formerly named GLAST, has been observing the high-energy gamma-ray sky with unprecedented sensitivity in<br />the 20MeV ÷ 300 GeV energy range and electrons + positrons in the 7 GeV ÷ 1TeV range, opening a new observational window on a wide variety of astrophysical objects.

SEARCH FOR BURST SIGNALS FROM POINT SOURCES

2005 ◽  
Vol 20 (29) ◽  
pp. 6962-6964
Author(s):  
◽  
P. LE COULTRE
Keyword(s):  
Gamma Rays ◽  
Time Windows ◽  
High Energy ◽  
Muon Flux ◽  
Point Sources ◽  
Source Position ◽  
High Energy Gamma ◽  
Sky Survey ◽  
Energy Gamma ◽  
Underground Muon

A sky survey for flaring point sources emitting high energy gamma rays has been performed with the L 3+ C underground muon spectrometer at LEP, CERN. Data were collected from mid July to October 1999 and from April to November 2000. No signal excesses in any direction have been found with muons above 20, 30, 50 and 100 GeV within one day and longer time windows. The steady muon flux sensitivity is of the order of a few times 10-9 cm-2 s-1 for muon energies above 20 GeV, and between 2 × 10-11 and 5 × 10-10 cm -2 s -1 for muon energies above 20 GeV depending on the source position.

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