Speaker
Description
Recent advances in realistic descriptions of pulsar magnetosphere with regions of finite conductivity allow for the predictions of the gamma-ray intensity over the observer sky in the form of a sky map. Such models incorporate trends of conductivity $\sigma$ with spin-down power $\dot E$, cut-off energies $\epsilon_{\rm cut}$ with $\dot E$, and the gamma-ray luminosity $L_\gamma$ with $\epsilon_{\rm cut}$, magnetic field $B$, and $\dot E$, thereby eliminating model free parameters. On the other hand, the radio luminosity $L_\nu$ requires three model free parameters the overall multiplicative factor $f_\nu$ and the exponents of the period $P$ and period derivative $\dot P$ with $\alpha_\nu$ and $\beta_\nu$, respectively. We perform Markov Chain Monte Carlo simulations to search the parameter space in order to establish the most likely values of the model free parameters in the case of millisecond pulsars (MSP). We then perform a simulation of young pulsars (YP) assuming magnetic field decay. We present preliminary results of both MSPs and YPs from the Galactic Disk.
We express our gratitude for the generous support of the National Science Foundation under grant AST-1616632 and the Michigan Space Grant Consortium under grant NNX15AJ20H.
