i-process nucleosynthesis and mass retention efficiency in He-shell flash evolution of rapidly accreting white dwarfs
Pavel Denissenkov (UVic), Falk Herwig (UVic), Umberto Battino (Basel),, Christian Ritter (UVic), Marco Pignatari (Hull), Samuel Jones (HIT), and Bill, Paxton (UCSB)

TL;DR
This study uses stellar evolution simulations to show that rapidly accreting white dwarfs can host the i-process during He-shell flashes, influencing galactic chemical evolution but unlikely leading to supernovae.
Contribution
It demonstrates the activation of the i-process in accreting white dwarfs during He-shell flashes and assesses their mass retention efficiency, impacting supernova progenitor models.
Findings
i-process activated during He-shell flashes in white dwarfs
White dwarfs have low mass retention efficiency (≤10%)
Accreted material is ejected, reducing supernova Ia likelihood
Abstract
Based on stellar evolution simulations, we demonstrate that rapidly accreting white dwarfs in close binary systems are an astrophysical site for the intermediate neutron-capture process. During recurrent and very strong He-shell flashes in the stable H-burning accretion regime H-rich material enters the He-shell flash convection zone. C(p,N reactions release enough energy to potentially impact convection, and i process is activated through the C(,n)O reaction. The H-ingestion flash may not cause a split of the convection zone as it was seen in simulations of He-shell flashes in post-AGB and low-Z AGB stars. We estimate that for the production of first-peak heavy elements this site can be of similar importance for galactic chemical evolution as the s-process production by low-mass AGB stars. The He-shell flashes result in the expansion and,…
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