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 Pb and help constrain the low density EOS. As the sensitivity of gravitational wave detectors improve, we expect to observe many more events. We are looking forward to exciting advances and surprises!
- Authors:
-
- Indiana Univ., Bloomington, IN (United States)
- Publication Date:
- Research Org.:
- Indiana Univ., Bloomington, IN (United States); Michigan State Univ., East Lansing, MI (United States)
- Sponsoring Org.:
- USDOE Office of Science (SC)
- OSTI Identifier:
- 1800670
- Alternate Identifier(s):
- OSTI ID: 1572741
- Grant/Contract Number:
- FG02-87ER40365; SC0018083
- Resource Type:
- Accepted Manuscript
- Journal Name:
- Annals of Physics
- Additional Journal Information:
- Journal Volume: 411; Journal Issue: C; Journal ID: ISSN 0003-4916
- Publisher:
- Elsevier
- Country of Publication:
- United States
- Language:
- English
- Subject:
- 79 ASTRONOMY AND ASTROPHYSICS; Physics; Dense matte; rNeutron stars; Gravitational waves
Citation Formats
Horowitz, C. J. 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. 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. Sun .
"Neutron rich matter in the laboratory and in the heavens after GW170817". United States. https://doi.org/10.1016/j.aop.2019.167992. https://www.osti.gov/servlets/purl/1800670.
@article{osti_1800670,
title = {Neutron rich matter in the laboratory and in the heavens after GW170817},
author = {Horowitz, C. J.},
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 Pb and help constrain the low density EOS. As the sensitivity of gravitational wave detectors improve, we expect to observe many more events. We are looking forward to exciting advances and surprises!},
doi = {10.1016/j.aop.2019.167992},
journal = {Annals of Physics},
number = C,
volume = 411,
place = {United States},
year = {Sun Dec 01 00:00:00 EST 2019},
month = {Sun Dec 01 00:00:00 EST 2019}
}
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