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advective-reactive nucleosynthesis

Convective-reactive i-process nucleosynthesis of heavy elements in a rapidly accreting white dwarf (WD). In general, convective zones within the interior of stars modify their evolution and modulate nuclear reactions. Here, hydrogen is ingested into a helium burning convective shell, which triggers a nuclear carbon reaction and produces neutron densities sufficiently high to promote i-process nucleosynthesis. Visualizations show the fractional volume of the material in the stable layer, at a time 500 minutes after the start of the simulation.

Methods: PPMstar code