Speaker
Description
The first observation of a kilonova (or macronova) in the aftermath of
a gravitational wave signal has confirmed neutron star mergers (NSMs) as
a major source of heavy r-process nuclei in the universe. However, some
observational data of r-process elements in the galaxy seemingly cannot be
explained if NSMs are assumed to be the only r-process site. Theoreti-
cal models show that the heaviest r-process nuclei can possibly be produced
also in other astrophysical scenarios, such as magneto-rotationally driven su-
pernovae (MRSNe) or disks forming around collapsars. Distinguishing these
scenarios by means of their nucleosynthetic signatures proves extremely chal-
lenging, since the properties of the neutron-rich nuclei involved are unknown,
in addition to the uncertainties in hydrodynamical conditions of the ejecta.
Most models, however, agree that the ejecta from NSMs include com-
ponents that are neutron-rich enough for fission cycling, while simulated
outflows from MRSNe are generally less neutron-rich. This talk aims to
outline possible differences in abundance patterns originating from this dif-
ference and to discuss uncertainties in nucleosynthesis calculations.