A general framework for incorporating arbitrary nonequilibrium corrections into linear non-radial relativistic stellar perturbations without specifying constitutive relations.
Origin of the heavy elements in binary neutron-star mergers from a gravitational wave event
11 Pith papers cite this work. Polarity classification is still indexing.
11
Pith papers citing it
abstract
The cosmic origin of the elements heavier than iron has long been uncertain. Theoretical modelling shows that the matter that is expelled in the violent merger of two neutron stars can assemble into heavy elements such as gold and platinum in a process known as rapid neutron capture (r-process) nucleosynthesis. The radioactive decay of isotopes of the heavy elements is predicted to power a distinctive thermal glow (a 'kilonova'). The discovery of an electromagnetic counterpart to the gravitational-wave source GW170817 represents the first opportunity to detect and scrutinize a sample of freshly synthesized r-process elements. Here we report models that predict the detailed electromagnetic emission of kilonovae and enable the mass, velocity and composition of ejecta to be derived from the observations. We compare the models to the optical and infrared radiation associated with GW170817 event to argue that the observed source is a kilonova. We infer the presence of two distinct components of ejecta, one composed primarily of light (atomic mass number less than 140) and one of heavy (atomic mass number greater than 140) r-process elements. Inferring the ejected mass and a merger rate from GW170817 implies that such mergers are a dominant mode of r-process production in the Universe.
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UNVERDICTED 11roles
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Relativistic transport model for beta-particles in homologously expanding kilonova ejecta, incorporating per-species atomic data, shows non-local deposition and escape lower thermalization efficiency with analytic prescriptions supplied for light-curve codes.
Simulations show magnetar giant flares produce nuclei near r-process peaks whose decays create bright MeV gamma-ray lines from 88Kr and 92Sr with fluxes above 10^-8 erg cm^-2 s^-1.
High-resolution GR neutrino-radiation MHD simulation of 1.35-1.35 Msun BNS merger shows KHI-driven B-field amplification to magnetar levels (~10^50 erg, factor >=316) in 3 ms post-merger.
In neutron star merger ejecta simulations, coupling in-situ nuclear networks with composition-dependent thermalization and frequency-dependent opacities changes nucleosynthesis yields, delays and reddens early emission, and produces brighter, bluer kilonovae than simplified analytic prescriptions.
Magnetically driven shocks from neutron star merger remnants can reheat ejecta to nuclear statistical equilibrium, alter r-process yields, and produce observable changes in kilonova color and light curves.
Improved Monte Carlo neutrino transport in BNS merger simulations that includes inelastic electron scattering and refined pair processes produces lower heavy-lepton neutrino energies/luminosities and 50% higher ejecta mass.
Monte Carlo simulation of post-merger remnant shows pair annihilation rates greatly increased in cold low-density regions and inelastic electron scattering important for heavy-lepton neutrino thermalization, processes not included in prior merger simulations.
The paper proposes a high-redshift (z>2) origin for GRB 061201 by combining afterglow constraints with deep JWST near-infrared imaging of a faint candidate host.
The Einstein Telescope will enable gravitational-wave observations up to cosmological distances, opening avenues for discoveries in astrophysics, cosmology, and fundamental physics.
Review summarizing the role of dense-matter equation of state, weak interactions, and r-process nucleosynthesis in binary neutron star mergers and their multimessenger observables.
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