Beta particles from r-process decay heat and ionize kilonova ejecta non-locally, so transport and detailed atomic data change the predicted temperature and ionization state.
A kilonova as the electromagnetic counterpart to a gravitational-wave source
5 Pith papers cite this work. Polarity classification is still indexing.
5
Pith papers citing it
abstract
Gravitational waves were discovered with the detection of binary black hole mergers and they should also be detectable from lower mass neutron star mergers. These are predicted to eject material rich in heavy radioactive isotopes that can power an electromagnetic signal called a kilonova. The gravitational wave source GW170817 arose from a binary neutron star merger in the nearby Universe with a relatively well confined sky position and distance estimate. Here we report observations and physical modelling of a rapidly fading electromagnetic transient in the galaxy NGC4993, which is spatially coincident with GW170817 and a weak short gamma-ray burst. The transient has physical parameters broadly matching the theoretical predictions of blue kilonovae from neutron star mergers. The emitted electromagnetic radiation can be explained with an ejected mass of 0.04 +/- 0.01 Msol, with an opacity of kappa <= 0.5 cm2/gm at a velocity of 0.2 +/- 0.1c. The power source is constrained to have a power law slope of beta = -1.2 +/- 0.3, consistent with radioactive powering from r-process nuclides. We identify line features in the spectra that are consistent with light r-process elements (90 < A < 140). As it fades, the transient rapidly becomes red, and emission may have contribution by a higher opacity, lanthanide-rich ejecta component. This indicates that neutron star mergers produce gravitational waves, radioactively powered kilonovae, and are a nucleosynthetic source of the r-process elements.
citation-role summary
background 3
citation-polarity summary
roles
background 3representative citing papers
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.
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.
The Einstein Telescope will enable gravitational-wave observations up to cosmological distances, opening avenues for discoveries in astrophysics, cosmology, and fundamental physics.
Overview of synergies between SKA radio observations and gamma-ray facilities for studying transient, variable, and steady GeV-TeV sources.
citing papers explorer
-
Beta-Particle Transport and Thermalization in Kilonova Ejecta with Detailed Atomic Microphysics
Beta particles from r-process decay heat and ionize kilonova ejecta non-locally, so transport and detailed atomic data change the predicted temperature and ionization state.
-
A magnetar formation in binary neutron star merger
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.
-
Effects of magnetically driven shocks on nucleosynthesis and kilonovae from neutron star mergers
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.
-
Science Case for the Einstein Telescope
The Einstein Telescope will enable gravitational-wave observations up to cosmological distances, opening avenues for discoveries in astrophysics, cosmology, and fundamental physics.
-
SKAO and Gamma-Ray Synergies
Overview of synergies between SKA radio observations and gamma-ray facilities for studying transient, variable, and steady GeV-TeV sources.