Classifying first, second, and third peak r-process signatures via gamma-ray emission
ORAL
Abstract
The groundbreaking multimessenger observations of GW170817 provided evidence that binary neutron star mergers are a site of the r-process, which is responsible for the production of a fraction of the elements heavier than iron. Continued observational evidence is warranted to differentiate leading candidate sites.
In this work, we examine the time dependent gamma ray emission of the r-process using a radioactive decay network which includes both ground and isomeric nuclear states. We compare the results for the cases of a first, second and third peak r-process, noting significant differences in the integrated light curve as well as in the 1-100 KeV range. In addition, we find the influence of the isomeric nuclear states to be significant. We discuss the implications of these differences for observation of future multimessenger events.
In this work, we examine the time dependent gamma ray emission of the r-process using a radioactive decay network which includes both ground and isomeric nuclear states. We compare the results for the cases of a first, second and third peak r-process, noting significant differences in the integrated light curve as well as in the 1-100 KeV range. In addition, we find the influence of the isomeric nuclear states to be significant. We discuss the implications of these differences for observation of future multimessenger events.
*We acknowledge support from the Directed Asymmetric Network Graphs for Research (DANGR) initiative at Los Alamos National Laboratory (LANL). LANL is operated by Triad National Security, LLC, for the National Nuclear Security Administration of U.S. Department of Energy (Contract No. 89233218CNA000001).
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Publication: The content of this presentation is in preparation for publication.
Presenters
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Axel Gross
- Los Alamos National Laboratory (LANL)