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T. M. Braje, R. W. Romani (Stanford University)
We have developed a Monte Carlo simulation code to accurately model pulsar surface and magnetospheric emissions. In these simulations, we include several rapid rotation effects which we have shown to be important in the accurate modeling of millisecond pulsar light curves and spectra. We also incorporate more subtle (e.g. relativistic Kerr effects, magnetospheric resonant scattering) effects which could be measurable in high signal-to-noise observations. We include non-magnetic model atmosphere calculations (Fe, H, solar abundance) that are angle-dependent and include the effects of limb-darkening. We discuss applications to SAX J1808.4-3658 and RX J1856.5-3754.