We present 3D global kinetic pulsar magnetosphere models, where the charged particle trajectories and the corresponding electromagnetic fields are treated self-consistently. For our study, we have developed a cartesian 3D relativistic particle-in-cell code that incorporates the radiation reaction forces. We describe our code and discuss the related technical issues, treatments, and assumptions. Injecting particles up to large distances in the magnetosphere, we apply arbitrarily low to high particle injection rates and get an entire spectrum of solutions from close to the Vacuum-Retarded-Dipole to close to the Force-Free solution, respectively. For high particle injection rates (close to FF solutions) significant accelerating electric field components are confined only near the equatorial current sheet outside the light-cylinder. A judicious interpretation of our models allows the calculation of the particle emission and consequently the derivation of the corresponding realistic high-energy sky-maps and spectra. Using model parameters that cover the entire range of spin-down powers of Fermi young and millisecond pulsars, we compare the corresponding model γ-ray light-curves, cutoff energies, and total γ-ray luminosities with those observed by Fermi to discover a dependence of the particle injection-rate, F, on the spin-down power,Ė, indicating an increase of F withĖ. Our models guided by Fermi observations 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 γ-ray phenomenology of both young and millisecond pulsars.

Based on the Fermi observational data we reveal meaningful constraints for the dependence of the macroscopic conductivity (σ) of dissipative pulsar magnetosphere models on the corresponding spindown rate,Ė. Our models are refinements of the FIDO (Force-Free Inside, Dissipative Outside) models whose dissipative regions are restricted on the equatorial current-sheet outside the light-cylinder. Taking into account the observed cutoff-energies of all the Fermi -pulsars and assuming that a) the corresponding γ−ray pulsed emission is due to curvature radiation at the radiation-reaction-limit regime and b) this emission is produced at the equatorial current-sheet near the light-cylinder, we show that the Fermi -data provide clear indications about the corresponding accelerating electric-field components. A direct comparison between the Fermi cutoff-energies and the model ones reveals that σ increases withĖ for highĖ-values while it saturates for low ones. This comparison indicates also that the corresponding gap-width increases toward lowĖ-values. Assuming the Goldreich-Julian flux for the emitting particles we calculate the total γ−ray luminosity (L γ ). A comparison between the dependence of the Fermi L γ -values and the model ones onĖ indicates an increase of the emitting particle multiplicity withĖ. Our modeling guided by the Fermi -data alone, enhances our understanding of the physical mechanisms behind the high energy emission in pulsar magnetospheres.