The minimal two DM components with SUSY

Huh, Ji-Haeng; Kim, Jihn E.; Kyae, Bumseok

doi:10.48550/arxiv.0812.5004

Cited by 2 publications

(3 citation statements)

References 4 publications

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“…The most popular DM candidate is the lightest supersymmetric particle (LSP) in the minimal supersymmetric standard model (MSSM). The MSSM LSP has been proposed to explain the e ± excesses [31][32][33][34][35][36][37][38][39][40][41][42][43][44][45][46][47][48] However the MSSM also has problem. The LSP is a linear combination of photino, zino and higgsino.…”

Section: Theoretical Models For Dark Mattermentioning

confidence: 99%

“…Although astrophysics calculations of background e ± spectrum in our galaxy have errors due to model parameters [3][4][5][6], within reasonable ranges it is not possible to eliminate the excesses in the energy range from 10 GeV to 1 TeV. The e ± excesses in cosmic ray have generated much excitement in particle physics community because dark matter (DM), which contributes about 23% energy density of our universe with properties different than those of the standard model (SM) particles, can provide a nature explanation [14][15][16][17][18][19][20][21][22][23][24] [25] [26][27][28][29][30] [ [31][32][33][34][35][36][37][38][39][40][41][42][43][44][45][46][47][48] [ [49][50][51] [ [52][53][54] [ [ [79][80]...…”

Section: Introductionmentioning

confidence: 99%

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A Brief Review on Dark Matter Annihilation Explanation for $e^\pm$ Excesses in Cosmic Ray

2009

Preprint

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Recently data from PAMELA, ATIC, FERMI-LAT and HESS show that there are e ± excesses in the cosmic ray energy spectrum. PAMELA observed excesses only in e + , but not in anti-proton spectrum. ATIC, FERMI-LAT and HESS observed excesses in e + + e − spectrum, but the detailed shapes are different which requires future experimental observations to pin down the correct data set. Nevertheless a lot of efforts have been made to explain the observed e ± excesses, and also why PAMELA only observed excesses in e + but not in antiproton. In this brief review we discuss one of the most popular mechanisms to explain the data, the dark matter annihilation. It has long been known that about 23% of our universe is made of relic dark matter. If the relic dark matter was thermally produced, the annihilation rate is constrained resulting in the need of a large boost factor to explain the data. We will discuss in detail how a large boost factor can be obtained by the Sommerfeld and Briet-Wigner enhancement mechanisms. Some implications for particle physics model buildings will also be discussed.

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Section: Theoretical Models For Dark Mattermentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

A Brief Review on Dark Matter Annihilation Explanation for $e^\pm$ Excesses in Cosmic Ray

2009

Preprint

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“…In many dark matter models, the dark matter particles are their own anti-particles (Majorana fermions), and can annihilate with each other. There are several possible DM annihilation scenarios: (i) DM particles annihilate to standard model particle pairs, such as gauge bosons, quarks, and lepton pairs 138,141,202,203,204,205 ; (ii) DM particles annihilate via virtual internal bremsstrahlung processes to produce e + e − γ 206 ; (iii) DM particles annihilate to new mediating particle pairs, which then decay to e + e − and other standard model particles 207,208,209 212,138,213,141,27,207,214,215,216,217,218,206,219,220,221,222,223,224,225,226,227,228,229,230,231,232,233,234,235,236,237,238,239,240,241,242,…”

Section: Dark Matter Models For the E ± Excessmentioning

confidence: 99%

Electron/Positron Excesses in the Cosmic Ray Spectrum and Possible Interpretations

Fan

Zhang

Chang

2010

Int. J. Mod. Phys. D

101

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The data collected by ATIC, PPB-BETS, FERMI-LAT and HESS all indicate that there is an electron/positron excess in the cosmic ray energy spectrum above ∼ 100 GeV, although different instrumental teams do not agree on the detailed spectral shape. PAMELA also reported a clear excess feature of the positron fraction above several GeV, but no excess in anti-protons. Here we review the observational status and theoretical models of this interesting observational feature. We pay special attention to various physical interpretations proposed in the literature, including modified supernova remnant models for the e ± background, new astrophysical sources, and new physics (the dark matter models). We suggest that although most models can make a case to interpret the data, with the current observational constraints the dark matter interpretations, especially those invoking annihilation, require much more exotic assumptions than some astrophysical interpretations. Future observations may present some "smoking-gun" observational tests to differentiate among different models and to identify the correct interpretation to the phenomenon.

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The minimal two DM components with SUSY

Abstract: We present the dark matter extension of the minimal supersymmetric standard model by one more stable fermion N toward explaining the recent rising high energy positron spectrum of the PAMELA data. The needed coupling can arise in the flipped-SU(5) GUT.

Cited by 2 publications

References 4 publications

A Brief Review on Dark Matter Annihilation Explanation for $e^\pm$ Excesses in Cosmic Ray

A Brief Review on Dark Matter Annihilation Explanation for $e^\pm$ Excesses in Cosmic Ray

Electron/Positron Excesses in the Cosmic Ray Spectrum and Possible Interpretations

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