Speaker
Description
I will show that Fermi data provide crucial information that guides us to yield meaningful constraints on the macroscopic parameters of our global dissipative pulsar magnetosphere models. Our FIDO (Force-Free Inside, Dissipative Outside) models indicate that the dissipative regions lie outside the light cylinder near the equatorial current sheet. Our models reproduce the light-curve phenomenology while a detailed comparison of the model spectral properties with those observed by Fermi reveals the dependence of the macroscopic conductivity parameter on the spin-down power. We further exploit these important results by building self-consistent 3D global kinetic particle-in-cell (PIC) models, which, eventually, provide the dependence of the macroscopic parameter behavior (e.g. conductivity) on the microphysical properties (e.g. particle multiplicities). Our PIC models provide field structures and particle distributions that are not only consistent with each other but also able to reproduce a broad range of the observed gamma-ray phenomenology (light curves and spectral properties) of both young and millisecond pulsars. The convergent results of our macroscopic and kinetic models and their agreement with the Fermi data provide a unique insight into the understanding of the physical mechanisms behind the high-energy emission in pulsar magnetospheres.
