Astrophysics: Radioactive glow as a smoking gun

  title={Astrophysics: Radioactive glow as a smoking gun},
  author={Stephan Rosswog},
The observation of infrared emission following a short γ-ray burst lends support to the hypothesis that mergers of compact binary systems cause such bursts and produce the heaviest nuclei in the cosmos. See Letter p.547 Hubble Space Telescope observations of the location of the short-duration γ-ray burst SGRBH 130603B, which was detected by the Burst Alert Telescope on NASA's Swift satellite on 3 June 2013, provide support for the favoured model for the origin of such bursts — the merger of… 
Electric Field-Induced "Tentillar" Bridging of a Droplet Twin.
Experimental investigations with high-speed imaging reveal that two unequal sized oppositely charged droplets suspended in an insulating oil can come in contact in an asymmetric manner under an
Multimessenger Detection Rates and Distributions of Binary Neutron Star Mergers and Their Cosmological Implications
Gravitational wave (GW) events, produced by the coalescence of binary neutron stars (BNSs), can be treated as the standard sirens to probe the expansion history of the universe, if their redshifts
Modeling of neutron-star mergers: a review while awaiting gravitational-wave detection
review some recent results on simulations of mergers of binary neutron stars, highlighting some of the several significant advances published in the literature in the years 2013 to 2015.


A ‘kilonova’ associated with the short-duration γ-ray burst GRB 130603B
Optical and near-infrared observations provide strong evidence that compact-object mergers are the progenitors of short-duration γ-ray bursts and the sites of significant production of r-process elements, and suggest that kilonovae offer an alternative, unbeamed electromagnetic signature of the most promising sources for direct detection of gravitational waves.
Electromagnetic counterparts of compact object mergers powered by the radioactive decay of r‐process nuclei
The most promising astrophysical sources of kHz gravitational waves (GWs) are the inspiral and merger of binary neutron star(NS)/black hole systems. Maximizing the scientific return of a GW detection
Transient Events from Neutron Star Mergers
Mergers of neutron stars (NS + NS) or neutron stars and stellar-mass black holes (NS + BH) eject a small fraction of matter with a subrelativistic velocity. Upon rapid decompression, nuclear-density
The multimessenger picture of compact object encounters: binary mergers versus dynamical collisions
We explore the multi-messenger signatures of encounters between two neutron stars (ns 2 ) and between a neutron star and a stellar-mass black hole (nsbh). We focus on the dierences between
Mergers of Neutron Star-Black Hole Binaries with Small Mass Ratios: Nucleosynthesis, Gamma-Ray Bursts, and Electromagnetic Transients
We discuss simulations of the coalescence of black hole-neutron star binary systems with black hole masses between 14 and 20 M☉. The calculations use a three-dimensional smoothed particle
R-process nucleosynthesis in dynamically ejected matter of neutron star mergers
Although the rapid neutron-capture process, or r-process, is fundamentally important for explaining the origin of approximately half of the stable nuclei with A > 60, the astrophysical site of this
r-Process in Neutron Star Mergers.
Sufficient material is ejected to explain the amount of r-process nuclei in the Galaxy by decompression of neutron star material, and the calculated abundances fit the observed solar r-pattern excellently for nuclei that include and are heavier than the A approximately 130 peak.
On the astrophysical robustness of the neutron star merger r-process
In this study we explore nucleosynthesis in the dynamic ejecta of compact binary mergers. We are particularly interested in the question how sensitive the resulting abundance patterns are to the
We investigate systematically the dynamical mass ejection, r-process nucleosynthesis, and properties of electromagnetic counterparts of neutron-star (NS) mergers in dependence on the uncertain
Mass ejection in neutron star mergers
We present the results of 3D Newtonian SPH simulations of the merger of a neutron star binary. The microscopic properties of matter are described by the physical equation of state of Lattimer and