Cosmic Ray-Turbulence Interplay in the Galaxy

Data: 
19/06/2019 - 14:00 - 15:00
Local: 
Auditório "Prof. Dr. Paulo Benevides Soares", Bloco G

Cosmic Ray-Turbulence Interplay in the Galaxy

Reinaldo Santos de Lima

IAG/USP

 

The proper understanding of cosmic ray (CR) transport is crucial for interpreting and modeling most of high-energy phenomena in our Galaxy. In the context of CR acceleration in supernova shocks, the efficiency of the diffusive shock acceleration mechanism relies on the ability of either the CR generated instabilities or the magnetohydrodynamic (MHD) turbulence to confine the CRs in the acceleration region via resonant scattering. At the same time, for the acceleration of CRs up to energies ~ 10^15 eV, the magnetic field in the pre-shock region has to be amplified to intensities much higher than those of the interstellar medium. One mechanism proposed for this amplification is the turbulence generated by the interaction of the CRs precursor with the density inhomogeneities of the interstellar medium. Far from the acceleration sites, both the large-scale MHD turbulence present in the interstellar medium and the turbulence locally generated through CR instabilities are important for controlling the CR propagation. In this seminar, I will present an overview about the basic CR-MHD turbulence interaction mechanisms. I will also discuss some results my collaborators and I obtained modeling the processes aforementioned using numerical simulations.