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We discovered two transient events in the Kepler field with light curves thatstrongly suggest they are type II-P supernovae. Using the fast cadence of theKepler observations we precisely estimate the rise time to maximum for KSN2011aand KSN2011d as 10.5$\pm 0.4$ and 13.3$\pm 0.4$ rest-frame days respectively.Based on fits to idealized analytic models, we find the progenitor radius ofKSN2011a (280$\pm 20$ R$_\odot$) to be significantly smaller than that forKSN2011d (490$\pm 20$ R$_\odot$) but both have similar explosion energies of2.0$\pm 0.3\times 10^{51}$ erg.  The rising light curve of KSN2011d is an excellent match to that predicted bysimple models of exploding red supergiants (RSG). However, the early rise ofKSN2011a is faster than the models predict possibly due to the supernovashockwave moving into pre-existing wind or mass-loss from the RSG. A mass lossrate of $10^{-4}$ M$_\odot$ yr$^{-1}$ from the RSG can explain the fast risewithout impacting the optical flux at maximum light or the shape of thepost-maximum light curve.  No shock breakout emission is seen in KSN2011a, but this is likely due to thecircumstellar interaction suspected in the fast rising light curve. The earlylight curve of KSN2011d does show excess emission consistent with modelpredictions of a shock breakout. This is the first optical detection of a shockbreakout from a type II-P supernova.

Shock Breakout and Early Light Curves of Type II-P Supernovae Observed with Kepler