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Title: Neutron rich matter in the laboratory and in the heavens after GW170817

Abstract

The historic observations of the neutron star merger GW170817 advanced our understanding of r-process nucleosynthesis and the equation of state (EOS) of neutron rich matter. Simple neutrino physics suggests that supernovae are not the site of the main r-process. Instead, the very red color of the kilonova associated with GW170817 shows that neutron star (NS) mergers are an important r-process site. We now need to measure the masses and beta decay half-lives of very neutron rich heavy nuclei so that we can more accurately predict the abundances of heavy elements that are produced. This can be done with new radioactive beam accelerators such as the Facility for Rare Isotope Beams (FRIB). GW170817 provided information on the deformability of NS and the equation of state of dense matter. The PREX II experiment will measure the neutron skin of {sup 208}Pb and help constrain the low density EOS. As the sensitivity of gravitational wave detectors improve, we expect to observe many more events. We look forward to exciting advances and surprises!.

Authors:
 [1]
  1. Center for Exploration of Energy and Matter and Department of Physics, Indiana University, Bloomington, IN, 47405 (United States)
Publication Date:
OSTI Identifier:
22852362
Resource Type:
Journal Article
Journal Name:
Annals of Physics (New York)
Additional Journal Information:
Journal Volume: 411; Other Information: © 2019 Elsevier Inc. All rights reserved.; Country of input: International Atomic Energy Agency (IAEA); Journal ID: ISSN 0003-4916
Country of Publication:
United States
Language:
English
Subject:
79 ASTROPHYSICS, COSMOLOGY AND ASTRONOMY; ACCELERATORS; BETA DECAY; EQUATIONS OF STATE; GRAVITATIONAL WAVE DETECTORS; GRAVITATIONAL WAVES; HALF-LIFE; LEAD 208; NEUTRINOS; NEUTRON STARS; NEUTRON-RICH ISOTOPES; NUCLEOSYNTHESIS; R PROCESS; SUPERNOVAE

Citation Formats

Horowitz, C.J., E-mail: horowit@indiana.edu. Neutron rich matter in the laboratory and in the heavens after GW170817. United States: N. p., 2019. Web. doi:10.1016/J.AOP.2019.167992.
Horowitz, C.J., E-mail: horowit@indiana.edu. Neutron rich matter in the laboratory and in the heavens after GW170817. United States. https://doi.org/10.1016/J.AOP.2019.167992
Horowitz, C.J., E-mail: horowit@indiana.edu. 2019. "Neutron rich matter in the laboratory and in the heavens after GW170817". United States. https://doi.org/10.1016/J.AOP.2019.167992.
@article{osti_22852362,
title = {Neutron rich matter in the laboratory and in the heavens after GW170817},
author = {Horowitz, C.J., E-mail: horowit@indiana.edu},
abstractNote = {The historic observations of the neutron star merger GW170817 advanced our understanding of r-process nucleosynthesis and the equation of state (EOS) of neutron rich matter. Simple neutrino physics suggests that supernovae are not the site of the main r-process. Instead, the very red color of the kilonova associated with GW170817 shows that neutron star (NS) mergers are an important r-process site. We now need to measure the masses and beta decay half-lives of very neutron rich heavy nuclei so that we can more accurately predict the abundances of heavy elements that are produced. This can be done with new radioactive beam accelerators such as the Facility for Rare Isotope Beams (FRIB). GW170817 provided information on the deformability of NS and the equation of state of dense matter. The PREX II experiment will measure the neutron skin of {sup 208}Pb and help constrain the low density EOS. As the sensitivity of gravitational wave detectors improve, we expect to observe many more events. We look forward to exciting advances and surprises!.},
doi = {10.1016/J.AOP.2019.167992},
url = {https://www.osti.gov/biblio/22852362}, journal = {Annals of Physics (New York)},
issn = {0003-4916},
number = ,
volume = 411,
place = {United States},
year = {2019},
month = {12}
}