WE WILL DEVELOP THE MODEL FOR GAMMA-RAY EMISSION FROM PULSARS OBSERVED BY FERMI. THE MODEL WILL BE BASED ON THE 3DMAGNETOSPHERIC SOLUTIONS WHICH INCLUDE THE BACKREACTION OF CURRENTS ON THE STRUCTURE OF THE FIELD. RECENT MODELING INDICATES THAT THE CHARACTERISTIC DOUBLE-PEAK LIGHT CURVES CAN BE EXPLAINED BY EMISSION FROM THE STRONG EQUATORIAL CURRENT SHEET THAT SEPARATES FIELD LINES FROM THE OPPOSITE HEMISPHERES NEAR THE LIGHT CYLINDER. WE WILL USE RESISTIVE FORCE-FREE AND RELATIVISTIC MHD MODELS TO PROVIDE THE BACKGROUND FIELD STRUCTURE AND PLASMA BEAMING REQUIRED TO CALCULATE DIRECTION OF EMISSION. WE WILL ALSO CALCULATE PHASE-RESOLVED GAMMA RAY SPECTRA FROM DISSIPATING CURRENT SHEETS OBTAINED FROM KINETIC SIMULATIONS OF THE MAGNETOSPHERE.