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Based on stellar evolution simulations, we demonstrate that rapidly accretingwhite dwarfs in close binary systems are an astrophysical site for theintermediate neutron-capture process. During recurrent and very strong He-shellflashes in the stable H-burning accretion regime H-rich material enters theHe-shell flash convection zone. $^{12}$C(p,$\gamma)^{13}$N reactions releaseenough energy to potentially impact convection, and i process is activatedthrough the $^{13}$C($\alpha$,n)$^{16}$O reaction. The H-ingestion flash maynot cause a split of the convection zone as it was seen in simulations ofHe-shell flashes in post-AGB and low-Z AGB stars. We estimate that for theproduction of first-peak heavy elements this site can be of similar importancefor galactic chemical evolution as the s-process production by low-mass AGBstars. The He-shell flashes result in the expansion and, ultimately, ejectionof the accreted and then i-process enriched material, via super-Eddingtonluminosity winds or Roche-lobe overflow. The white dwarf models do not retainany significant amount of the accreted mass, with a He retention efficiency of$\leq 10\%$ depending on mass and convective boundary mixing assumptions. Thismakes the evolutionary path of such systems to supernova Ia explosion highlyunlikely.

i-process nucleosynthesis and mass retention efficiency in He-shell flash evolution of rapidly accreting white dwarfs