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Cosmic Ray Transport in our Galaxy and Starburst Galaxies and Secondary Emission
Cosmic rays are energetic charged particles and these particles are injected into the interstellar medium (ISM) by plausible sources such as supernova remnants. After acceleration in these sources they also undergo reacceleration, spallation and radiative processes during their transport in our Galaxy. The secondary nuclei produced via spallation (Li, Be, B etc) are tracers for the cosmic ray transport in our Galaxy. Using the observed ratio of these secondary nuclei with the primary cosmic rays we constrain the model parameters for cosmic ray transport in our Galaxy. This model is very useful to interpret the observed cosmic ray flux on Earth as well as fluxes of cosmic ray positrons and antiprotons. The recent results by the DAMPE satellite have measured some features in the cosmic ray proton spectrum in TeV energy range which indicates more than one population of cosmic ray sources resides in our Galaxy.
In this talk I will describe these processes and how the current observations of cosmic rays and secondary particles by DAMPE, AMS, PAMELA, IceCube and Cherenkov gamma ray detectors are helping us to understand the origin of cosmic rays. I will also update how the scenario changes in the starburst galaxies where not only the intensity of cosmic rays is higher but also dense gas regions are available for interactions.