Abstract
The detection of gravitational waves and electromagnetic signals from the neutron star merger GW170817 has provided evidence that these astrophysical events are sites where the r-process nucleosynthesis operates. The electromagnetic signal, commonly known as kilonova, is powered by the radioactive decay of freshly synthesized nuclei. However, its luminosity, colour and spectra depend on the atomic opacities of the produced elements. In particular, opacities of lanthanides and actinides elements, due to their large density of bound–bound transitions, are fundamental. The current work focuses on atomic structure calculations for lanthanide and actinide ions, which are important in kilonovae modelling of ejecta spectra. Calculations for Nd III and U III, two representative rare-earth ions, were achieved. Our aim is to provide valuable insights for future opacity calculations for all heavy elements. We noticed that the opacity of U III is about an order of magnitude greater than the opacity of Nd III due to a higher density of levels in the case of the actinide.
Highlights
IntroductionDepending on the neutron density reached in the astrophysical environment, one distinguishes between the s-process (s for slow) and r-process (r for rapid)
Laboratory for Instrumentation, Biomedical Engineering and Radiation Physics (LIBPhys-UNL), Department of Physics, NOVA School of Science and Technology, NOVA University Lisbon, 2829-516 Caparica, Portugal; GSI Helmholtzzentrum für Schwerionenforschung, Planckstraße 1, 64291 Darmstadt, Germany; Institut für Kernphysik (Theoriezentrum), Fachbereich Physik, Technische Universität Darmstadt, Schlossgartenstraße 2, 64298 Darmstadt, Germany
While it has been known for a long time that the s-process operates on the asymptotic giant branch (AGB) stars, only recently have we been able to identify one of the astrophysical sites where the r-process operates [1]
Summary
Depending on the neutron density reached in the astrophysical environment, one distinguishes between the s-process (s for slow) and r-process (r for rapid) While it has been known for a long time that the s-process operates on the asymptotic giant branch (AGB) stars, only recently have we been able to identify one of the astrophysical sites where the r-process operates [1]. This has been made possible by the observation of a kilonova associated with the collision of two neutron stars.
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