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use as essential inputs recently measured proton spectra [23,31,32], which are significantly (by a factor 1.4 to 1.6) lower than previous data in the energy range (10 to 50 GeV) relevant to the p¯ production. These calculations reproduce our spectrum at the peak 10
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3.
Indirect search for Supersymmetric Dark Matter
Observations and cosmology indicate that the Universe may include a large amount of unknown dark matter (DM). It should be composed of non-baryonic Weakly Interacting Massive Particles (WIMP). A good WIMP candidate being the Lightest Supersymmetric Particle in R-parity conserving SUSY models. AMS offers a unique opportunity to study simultaneously SUSY dark matter in three decay channels from the neutralino annihilation: e+ , p¯ and γ. Positron Flux: In recent works[2] e+ production by annihilating neutralinos χ01 in the galactic halo has been simulated according to several models, varying 7 free parameters of the MSSM. In each model the e+ interstellar flux has been calculated by means of a standard diffusion model. Two models assuming mχ being 336 GeV and 130.3 GeV respectively have been investigated by means of DARKSUSY[11]. The e+ signal from χ annihilation was boosted by factors 11.7 and 54.6 to fit the HEAT data, the simulated primary positron fluxes have been
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Energy resolution σ [%] E
χ2 / ndf
11.05 / 8
Prob
7 6
0.1986
a
9.641 ± 0.29
b
2.413 ± 0.05821
5 4 3 2 1 0 10
10
2
E [GeV]
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σ ( θ) [ ]
åù åù
8.248 / 8
Prob
4
3.5
0.4096
a
5.695 ± 0.1187
b
0.5063 ± 0.03259
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10
2
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