Abstract
We present numerical models of dissipative 3D pulsar magnetospheres which are then used to model pulsar γ-ray light-curves (LC). Using a variety of prescriptions to relate the current density J to the fields E, B we produce families of solutions covering the entire spectrum between the vacuum retarded dipole (VRD) and the force-free solutions. These solutions provide also the distribution of electric fields, E∥ parallel to the magnetic field B, which accelerate the radiating particles. Using these detailed dissipative magnetospheric models we generate model LCs following two different approaches: (a) We define realistic trajectories of radiating particles in these dissipative magnetospheres and we compute their Lorentz factor under the influence of both the electric field E∥ and radiation-reaction effects; with these at hand we then calculate the radiation intensity as a function of pulsar phase to produce realistic LCs. (b) We use the standard emission arrangements of slot and outer gap models in the magnetic field geometries of our dissipative magnetospheres to improve the LCs based on the VRD geometry used to date.
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