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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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l values of the changes of the lication of the The dominant es, respectively, alculations and ttribute ±15 % BESS ’97 fluxes the overlapping solar activities ose to the minors and by the by BESS. (’95+’97) specme a distinctive rly is the dom-



provides crucial ar modulation, e input source 2 n be calculated 1 Bottino 3 2 Bergstrom helium spectra 3 Biebar 4 roduction. The 4 Mitsui λ(R,β) 5 m also has clear 5 Mitsui λ(R) 1 tonic (and un-3 ys. 10 -1 10 1 10 theoretical calKinetic Energy (GeV) n model [25,26] Figure 2. Compilation of observed p/p ¯ flux ratios at top of atmosphere, compared with model he propagation Data from Buffington et al. (1981), Golden FIG. 3. BESS ’95+’97 (solar minimum) antiproton fluxes calculations for secondary and primary p¯ production. Z n

o p qsrut Salamon et al. (1990, PBAR), Streitmatter et al. et al. (1979), Bogomolov et al. (1979, 1987, 1990), length) are deat the top of the atmosphere together with previous data. (1990, LEAP), Boezio et al. (1997, CAPRICE94), Bergström et al. (2000, CAPRICE98), Mitchell y nuclei such as The error-bars represent the quadratic sums of the statistical et al. (1996, IMAX), Hof et al. (1996, MASS91), Orito et al. (2000 BESS, 95&97), Maeno et al. (2000, BESS). The theoretical calculations of the p/p ¯ ratio are from Moskalenko et al. (1998, on that the difand systematic errors. The curves are recent calculations of MSR-1, MSR-2), Webber and Potgieter (1989, W&P), and Simon et al. (1998, SMR). Possible v wy.the z|{'secondary }d~u€.x‚Rƒ5p¯„l  …  w ˆ † 1 ‡ ' ‰  w 5 ƒ e Š ; ƒ \ ‹ . ƒ  Œ 4   } ' { . Ž

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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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11.05 / 8

Prob

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0.1986

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9.641 ± 0.29

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E [GeV]

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3.5

0.4096

a

5.695 ± 0.1187

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0.5063 ± 0.03259

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2

E [GeV]

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