Uncertainties of Cosmic Ray Spectra and Detectability of Antiproton mSUGRA

We studied the variation of e + and ¯ p top of the atmosphere spectra due to the parameters uncertainties of the Milky Way geometry, propagation models and cross sections. We used the B/C data and Galprop code for the propagation analysis. We also derived the uncertainty bands for subFe/Fe ratio, H, He, antiproton to proton ratio and the positron charge fraction. Finally, we considered a neutralino induced component in the antiproton flux in the mSUGRA framework. PAMELA expectations for positrons and antiprotons are calculated. We studied in details the possibility to disentangle an eventual supersymmetric component in the antiproton spectra in a clumpy halo scenario. We computed the minimal and the maximal values of the clumpiness factors needed to disentangle the signal from the background without violating present data. The main result of this work is that, assuming as the background the best fit for the DC model, PAMELA will be able to disentangle an eventual supersymmetric signal even for small clumpiness factors. Lower values of the background will expand the allowed mSUGRA parameter space but for higher clumpiness factors. Higher values of the background will reduce the allowed mSUGRA parameter space but for smaller clumpiness factors.