The origin of the elements and other implications of gravitational wave detection for nuclear physics
Résumé
The neutron-star collision revealed by the event GW170817 gave us a first glimpse of a possible birthplace of most of our heavy elements. The multi-messenger nature of this historical event combined gravitational waves, a gamma-ray burst and optical astronomy of a “kilonova”, bringing the first observations of rapid neutron capture (r process) nucleosynthesis after 60 years of speculation. Modeling the r process requires a prodigious amount of nuclear-physics ingredients: practically all the quantum state and interaction properties of virtually all neutron-rich nuclides, many of which may never be produced in the laboratory! Another essential contribution of nuclear physics to neutron stars (and their eventual coalescence) is the equation of state (EoS) that defines their structure and composition. The EoS, combined with the knowledge of nuclear binding energies, determines the elemental profile of the outer crust of a neutron star and the relationship between its radius and mass. In addition, the EoS determines the form of the gravitational wave signal. This article combines a tutorial presentation and bibliography with recent results that link nuclear mass spectrometry to gravitational waves via neutron stars.Key words: Gravitational waves / Nuclear binding energy / Nuclear equation of state / r-process nucleosynthesis / Chemical elements
Mots clés
Gravitational waves
Nuclear binding energy
Nuclear equation of state
r-process nucleosynthesis
Chemical elements
nucleus: mass
nucleus: binding energy
gamma ray: burst
n: capture
gravitational radiation
neutron star
nuclear physics
equation of state
nucleosynthesis
coalescence
structure
nuclide
optical
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