Carmelo Evoli

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We study the compatibility of Alpha Magnetic Spectrometer (AMS-02) data on the cosmic-ray (CR) positron fraction with data on the CR electron and positron spectra provided by PAMELA and Fermi LAT. We do that in terms of a novel propagation model in which sources are distributed in spiral arm patterns in agreement with astrophysical observations. While(More)
We construct realistic maps of the expected neutrino and γ-ray emissions above the TeV originated from the hadronic scattering of cosmic rays (CR) with the interstellar medium (ISM). Differently from previous works, where a uniform CR density was assumed, we estimate the spatial distribution of primary nuclei by means of numerical simulations considering(More)
In the last months several ballon and satellite experiments improved significantly our knowledge of cosmic ray (CR) spectra at high energy. In particular CREAM allowed to measure B/C, C/O and N/O ratios up to 1 TeV/n and PAMELA the p̄/p ratio up to 100 GeV with unprecedented accuracy. These measurements offer a valuable probe of CR propagation properties.(More)
We use our numerical code, DRAGON, to study the implications and the impact of recent CREAM and PAMELA data on our knowledge of the propagation properties of cosmic ray nuclei with energy & 1 GeV/n in the Galaxy. We will show that B/C (as well as N/O and C/O) and p̄/p data (especially including recent PAMELA results) can consistently be matched within a(More)
We discuss the Li abundance evolution within a hierarchical model of Galaxy formation which correctly reproduces the [Fe/H] distribution of metal-poor halo stars. Contrary to previous findings, we find that neither the level (Li/H= 6 × 10) nor the flatness of the Li distribution with [Fe/H] can be reproduced under the most favourable conditions by any model(More)
We investigate the atomic (HI) and molecular (H2) Hydrogen content of normal galaxies by combining observational studies linking galaxy stellar and gas budgets to their host dark matter (DM) properties, with a physically grounded galaxy formation model. This enables us to analyse empirical relationships between the virial, stellar, and gaseous masses of(More)
Multichannel cosmic ray spectra and the large scale cosmic ray anisotropy can hardly be made compatible in the framework of conventional isotropic and homogeneous propagation models. These models also have problems explaining the longitude distribution and the radial emissivity gradient of the γ-ray Galactic interstellar emission. We argue here that(More)
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