  We investigate the shapes of \gamma-ray pulsar light curves using 3D pulsar
magnetosphere models of finite conductivity. These models, covering the entire
spectrum of solutions between vacuum and force-free magnetospheres, for the
first time afford mapping the GeV emission of more realistic, dissipative
pulsar magnetospheres. To this end we generate model light curves following two
different approaches: (a) We employ the emission patterns of the slot and outer
gap models in the field geometries of magnetospheres with different
conductivity \sigma. (b) We define realistic trajectories of radiating
particles in magnetospheres of different \sigma and compute their Lorentz
factor under the influence of magnetospheric electric fields and curvature
radiation-reaction; with these at hand we then calculate the emitted radiation
intensity. The light curves resulting from these prescriptions are quite
sensitive to the value of \sigma, especially in the second approach. While
still not self-consistent, these results are a step forward in understanding
the physics of pulsar \gamma-radiation.
