After a successful core-collapse supernova a neutrino-driven wind develops from the nascent neutron star. Neutrino-driven winds are a possible astrophysical site for the synthesis of the lighter heavy elements (26 < Z < 47) which are associated to the r-process and at least one additional process. Despite the fast process in the last years the astrophysical and nuclear physics uncertainties are still relatively large. We study the impact of the astrophysical uncertainties on the nucleosynthesis in the wind and have a special focus on the formation of 92,94Mo and 96,98Ru. The Mo and Ru p-isotopes have raised interest because their nucleosynthesis origin in the solar system is a long lasting mystery. We present the necessary conditions for the synthesis of 92,94Mo and 96,98Ru and show whether the wind can explain their solar system abundances. Moreover, we show that (alpha,n) reactions are critical to redistribute matter in neutron-rich winds. In the absence of experiments most (alpha,n) reaction rates are calculated with statistical models, and thus contain some uncertainties. Our results show that (alpha,n) rate uncertainties are crucial for the abundances. Since the nucleosynthesis path is close to stability, individual critical reactions can be measured with new radioactive beam facilities in the near future.