Recent developments in TeV astronomy have boosted our study of particle acceleration in supernova remnants significantly. I will first discuss the Fermi acceleration mechanism and the difference between diffusive shock acceleration and stochastic particle acceleration model. The talk will then focus on observations and theoretical modeling of SNR RX J1713.7-3946. There are two competing scenarios for the TeV emission from this remnant. In the leptonic model, the TeV emission is produced by TeV electrons via the inverse Compton scattering of the Cosmic Microwave Background Radiation. In the hadronic model, the TeV photons are produced by TeV protons via inelastic collisions with the background ions and the consequence generation and decay of neutral pions. I will discuss these two models and show how future observational and theoretical developments may distinguish them.