Production of solar abundances for nuclei beyond Sr: The s- and r-process perspectives

Abstract

We present the status of nucleosynthesis beyond Sr, using up-to-date nuclear inputs for both the slow (s-process) and rapid (r-process) scenarios of neutron captures. It is now widely accepted that at least a crucial part of the r-process distribution is linked to neutron star merger (NSM) events. However, so far, we have found only a single direct observation of such a link, the kilonova GW170817. Its fast evolution could not provide strict constraints on the nucleosynthesis details, and in any case, there remain uncertainties in the local r-process abundance patterns, which are independent of the specific astrophysical site, being rooted in nuclear physics. We, therefore, estimate the contributions from the r-process to solar system (S.S.) abundances by adopting the largely site-independent waiting-point concept through a superposition of neutron density components normalized to the r-abundance peaks. Nuclear physics inputs for such calculations are understood only for the trans-Fe nuclei; hence, we restrict our computations to the Sr–Pr region. We then estimate the s-process contributions to that atomic mass range from recent models of asymptotic giant branch stars, for which uncertainties are known to be dominated by nuclear effects. The outcomes from the two independent approaches are then critically analyzed. Despite the remaining problems from both sides, they reveal a surprisingly good agreement, with limited local discrepancies. These few cases are then discussed. New measurements in ionized plasmas are suggested as a source of improvement, with emphasis on β-decays from unstable Cs isotopes. For heavier nuclei, difficulties grow as r-process progenitors lie far off experimental reach and poorly known branchings affect s-processing. This primarily concerns nuclei that are significantly long-lived in the laboratory and have uncertain decay rates in stars, e.g., Lu176 and Re187. New measurements are urgently needed for them, too.

Design of a novel ECR ion trap facility for nuclear physics and fundamental plasma processes studies

“…The recent activities of the PANDORA collaboration have been focused on the magnetic trap design [5] to be used in the experiments foreseen in 2025 and in the development of different tools for plasma diagnostics [7,11]. Advances in R&D activity are carried out along with theoretical models [15,16,17] and simulations [6,18,19] supporting the idea of the project.…”

How do nuclear isomers influence the gamma-ray bursts in binary neutron star mergers?

“…• We estimate the fraction of each element produced in merging neutron stars (see Table 1), based on Supplementary Table S1 in the Supplementary Material from Johnson (2019). A revised estimation is found in Busso et al (2022). • We calculate the quantity of baryons for each element, rescaled to the abundance of heavy elements baryons, assuming that neutron star collision produce mainly these heavy elements.…”

GEANT4 simulations for γ-ray detector array design for inplasma β-decays studies of nuclear astrophysics interest

“…Only few experimental evidences have been collected up to now mainly using as setups storage rings [2][3][4]. If confirmed, these evidences are expected to have a huge impact in the study of nuclear-astrophysics processes and cosmology (BBN, s-processing, Cosmo-chronometers, Early Solar System formation) [5][6][7][8][9]. The PANDORA (Plasma for Astrophysics, Nuclear Decay Observation and Radiation for Archaeometry) project [10], supported by the INFN, proposes a new experimental approach to measure the variation of the half-life of β-decaying nuclei in the magnetically confined ECR plasma, correlating the decaying rate with thermodynamic plasma properties.…”