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Rapidly accreting white dwarfs (RAWDs) have been proposed as contributors tothe chemical evolution of heavy elements in the Galaxy. Here, we test thisscenario for the first time and determine the contribution of RAWDs to thesolar composition of first-peak neutron-capture elements. We add themetallicity-dependent contribution of RAWDs to the one-zone galactic chemicalevolution code OMEGA according to RAWD rates from binary stellar populationmodels combined with metallicity-dependent $i$-process stellar yieldscalculated following the models of Denissenkov et al. (2017). With thisapproach we find that the contribution of RAWDs to the evolution of heavyelements in the Galaxy could be responsible for a significant fraction of thesolar composition of Kr, Rb, Sr, Y, Zr, Nb, and Mo ranging from $2$ to $45\%$depending on the element, the enrichment history of the Galactic gas, and thetotal mass ejected per RAWD. This contribution could explain the missing solarLighter Element Primary Process for some elements (e.g., Sr, Y, and Zr). We donot overproduce any isotope relative to the solar composition, but $^{96}$Zr isproduced in a similar amount. The $i$ process produces efficiently the Mostable isotopes $^{95}$Mo and $^{97}$Mo. When nuclear reaction rateuncertainties are combined with our GCE uncertainties, the upper limits for thepredicted RAWD contribution increase by a factor of $1.5-2$ for Rb, Sr, Y, andZr, and by 3.8 and 2.4 for Nb and Mo, respectively. We discuss the implicationof the RAWD stellar evolution properties on the single degenerate Type Iasupernova scenario.

i-Process Contribution of Rapidly Accreting White Dwarfs to the Solar Composition of First-Peak Neutron-Capture Elements