2-7 June 2019
Simon Fraser University
America/Vancouver timezone
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Masses of neutron-rich Ga isotopes for the formation of the 1st r-process abundance peak in neutron star merger

5 Jun 2019, 14:15
15m
DAC FT I (Simon Fraser University)

DAC FT I

Simon Fraser University

Oral (Non-Student) / Orale (non-étudiant(e)) Nuclear Physics / Physique nucléaire (DNP-DPN) W2-8 Nuclear Astrophysics II (DNP) | Astrophysique nucléaire II (DPN)

Speaker

Dr Moritz Pascal Reiter (JLU, TRIUMF)

Description

Since the discovery of the GW170817 binary neutron star merger and the associated kilonova, it became clear that such an event can indeed produce heavy elements up to the lanthanide region and recent work has been focussed on understanding the formation of the 2nd and 3rd r-process abundance peaks as well as the lanthanide region. However nuclear data in these regions is scares. The situation is advantages for the 1st abundance peak, which is more in reach of current radioactive beam (RIB) facilities. However beams of these neutron-rich isotopes around the closed neutron shell at N=50 suffer from strong isobaric background, making high precision measurements challenging. To overcome the strong background an isobar separator based on the Multiple-Reflection Time-Of-Flight Mass Spectrometry (MR-TOF-MS) technique has been installed at TRIUMF’s Ion Trap for Atomic and Nuclear science (TITAN), similar to other ion trap on-line facilities. The MR-TOF-MS enables high precision mass measurements of very short-lived nuclides that are weakly produced.

With mass measurements of neutron-rich Ga isotopes at TITAN, we determine one of the last missing experimental properties to model the formation of the A=84 abundance maximum of the 1st r-process peak under conditions prevalent in the ejecta of the blue kilonova of the GW170817 binary neutron star merger. Performing large-scale nuclear reaction calculations with two state of the art reaction codes, we can perform a detailed investigation on how the abundance maxima at A=80 and A=84 of the 1st r-process abundance peak are formed. This indicates that binary neutron star mergers may not have the potential to be the dominant source of light r-process elements.

Primary author

Dr Moritz Pascal Reiter (JLU, TRIUMF)

Co-authors

Dr Andree Sieverding (GSI, TU-Darmstadt) Anna Kwiatkowski (TRIUMF) Brian Kootte C. Andreoiu (Simon Fraser University) C. SCHEIDENBERGER (GSI Helmholtzzentrum fu ̈r Schwerionenforschung, D-64291 Darmstadt, Germany) Dr Christine Hornung (GSI, JLU-Giessen) Dr D Welch (NSCL) ELEANOR DUNLING (TRIUMF) Erich Leistenschneider (TRIUMF) Gabriel Martínez Pinedo (GSI Darmstadt) Gerald Gwinner (University of Manitoba) Hendrik Schatz (National Superconducting Cyclotron Laboratory) Iris Dillmann Jens Dilling (triumf/UBC) Dr Jonas Lippuner (Los Alamos National Lab, JINA) Dr Luke Roberts (NSCL) Michael Wieser (University of Calgary) Prof. Robert Thompson (University of Calgary, Canada) Dr Samuel Ayet San Andres (GSI, JLU-Giessen) Stefan Paul (TRIUMF) Mr Stylianos Nikas (GSI, TU-Darmstadt) Thomas Brunner (McGill University) Timo Dickel (GSI) Dr Wolfgang Plass (GSI, JLU-Giessen) Yang Lan (TRIUMF)

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