Mainz 2022 – scientific programme
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HK: Fachverband Physik der Hadronen und Kerne
HK 34: Invited Talks IV
HK 34.2: Invited Talk
Wednesday, March 30, 2022, 11:30–12:00, HK-H1
Electromagnetic Counterparts of Neutron Star Mergers: Signatures of Heavy r-Process Nucleosynthesis — •Andreas Flörs1, Luke Shingles1, and Gabriel Martínez-Pinedo1,2 — 1GSI, Darmstadt, Germany — 2TU Darmstadt, Darmstadt, Germany
It has long since been established that observable actinides in the universe originate from the r-process. In 2017, the electromagnetic counterpart to the gravitational wave detection of two merging neutron stars was observed. From the light curve alone it was possible to characterize two ejecta components: one that contains low-Ye material such as lanthanides and possibly actinides, and a high-Ye component with low lanthanide abundances. The dividing characteristic between the two components is the opacity of the material: lanthanides have a ∼100 times higher opacity than iron-group material. The opacity of actinides is expected to be on a similar level as that of the lanthanides, or, possibly, even higher.
To identify specific elements, spectroscopic information is required. However, so far no clear detection of individual lanthanides or actinides has been made in the only observed neutron star merger. A great challenge for spectroscopic modeling of kilonovae using radiative transfer codes is the almost non-existent atomic data currently available for lanthanides and actinides. I will present converged and, where possible, calibrated atomic structure calculations from Zr to U. I will then use this collection of atomic data to show how we can use radiative transfer simulations to identify signatures or place constraints on the amount of heavy r-process material synthesized in kilonovae.