THE DISCOVERY BY FERMI LAT OF GEV GAMMA-RAYS FROM CLASSICAL NOVAE ILLUSTRATES THE IMPORTANCE OF SHOCKS AND RELATIVISTIC PARTICLE ACCELERATION IN THESE EVENTS. THE CORRELATION BETWEEN OPTICAL AND GAMMA-RAY LIGHT CURVES IN ASASSN-16MA SHOWS THAT THE SHOCKS CAN BE RADIATIVE I.E. THE POST-SHOCK COOLING TIMESCALE IS MUCH SHORTER THAN THE FLOW TIME. USING 2D/3D HYDRODYNAMIC SIMULATIONS WE WILL EXPLORE THE IMPACT OF THE NON-LINEAR THIN SHELL INSTABILITY ON THE GEOMETRY OF THE SHOCK FRONT THE THERMODYNAMIC CONDITIONS OF THE POSTSHOCK GAS AND THE RESULTING THERMAL/NON-THERMAL EMISSION. THE DISTRIBUTION OF SHOCK OBLIQUITY RELATIVE TO THE UPSTREAM MAGNETIC FIELD WILL BE COMBINED WITH HYBRID PIC SIMULATIONS TO QUANTIFY THE ION ACCELERATION EFFICIENCY AND COMPARE TO LAT-DETECTED NOVAE.