  Pulsars emit pulsed emission across the entire electromagnetic spectrum and
their light curve phenomenology is strongly dependent on energy. This is also
true for the gamma-ray waveband. Continued detections by Fermi Large Area
Telescope in the GeV band and ground-based Cherenkov telescopes in the TeV band
(e.g., Crab and Vela above 1 TeV) raise important questions about our
understanding of the electrodynamics and local environment of pulsar
magnetospheres. We model energy-dependent light curves (as a function of
geometry, e.g., pulsar inclination and observer angle) in the curvature
radiation domain using a full emission code. We will discuss our refined
calculation of the curvature radius of the particle trajectory and the effect
thereof on the expected light curve shapes, as well as the origin of the light
curve peaks in the magnetosphere. Our modelling should aid in differentiating
between different emission mechanisms, as well as constraining the emission
geometry by comparing our predictions to multi-wavelength data.
