p‐Process modeling of some rare but stable proton‐rich nuclei requires knowledge of a variety of neutron, charged particle, and photonuclear reaction rates at temperatures of 2 to 3×109°K. Detailed balance is usually invoked to obtain the stellar photonuclear rates, in spite of a number of well‐known constraints. In this work we attempt to calculate directly the stellar rates for (&ggr;,n) and (&ggr;,&agr;) reactions on151Eu. These are compared with stellar rates obtained from detailed balance, using the same input parameters for the stellar (n,&ggr;) and (&agr;,&ggr;) reactions on150Eu and147Pm, respectively. The two methods yielded somewhat different results, which will be discussed along with some sensitivity studies.