|Speaker:||Carmelo Evoli (DESY)|
|Title:||Modeling cosmic-ray propagation in the Galaxy|
|Date (JST):||Mon, Nov 02, 2015, 13:30 - 14:30|
|Place:||Seminar Room A|
At GeV-TeV energies the propagation of cosmic rays (CRs) in our Galaxy is diffusive. Current models of galactic propagation are based on a simplified approach for which diffusion is constant and isotropic. In fact, diffusion transport must be described as in-homogenous and anisotropic and experimental data have now reached an accuracy that allows to study such effects. In my talk, I will present some of the consequences of adopting realistic diffusion models for the propagation of galactic CRs, and I will show how these models allow a better understanding of local observations and diffusion emissions within an unified framework.
Whether or not an exotic component, as the fugitive Dark Matter (DM), contributes to the observed fluxes, is one of the most important open problem in Cosmology. Antiprotons play a key role in this context, since weakly interacting massive particle annihilations can be a copious source of antiprotons, and the antiproton flux from conventional astrophysical sources is predicted with fair accuracy and makes for a potentially very good signal/background ratio. In the second part of my talk, I will focus on antiprotons as a tool to set constraints on DM models. In particular, I will discuss the uncertainties associated to the propagation in the Galaxy both for standard astrophysical and DM originated antiprotons.