NBIA Seminar: Silvia Manconi

The observation of few-degree extended gamma-ray halos around Galactic pulsars has opened a new window to investigate the acceleration and propagation of cosmic rays in our Galaxy. Currently, there is a generic consensus that these gamma-ray structures, observed from GeV to multi TeV energies, are the result of inverse Compton scattering of electrons and positrons accelerated at the pulsar’s wind termination shock and propagating diffusively in the turbulent interstellar medium. However, many aspects remain unclear: How are these halos formed? Are they a general property of Galactic pulsars? What are the consequences for cosmic-ray acceleration and propagation in our Galaxy at large? In this talk I will review our current understanding of these objects, the most recent theoretical and observational developments, and conclude by outlining some perspectives to shed light on the open questions in the near future.