Inflation has proven to be a useful framework for understanding many aspects of the early universe, but ideally, one would like to compute the inflationary potential rather than postulating one. In models such as the KKLMMT model, where inflation is embedded in a string model with the extra dimensions stabilized, the potential is in principle computable in some regions of parameter space. At first glance, the simplest such models inescapably have an eta parameter that is much too large, but I will show how string effects can alleviate this problem. In particular, I will review the effect of D-brane interactions on the superpotential, and give some remarks about the largely unexplored Kahler corrections.