Cocoon cooling emission in neutron star mergers

In the gravitational wave event GW170817, there was a & SIM;10 h gap before electromagnetic (EM) observations, without detection of the cocoon. The cocoon is heated by a short gamma-ray burst (sGRB) jet propagating through the ejecta of a neutron star (NS) merger, and a part of the cocoon escapes the ejecta with an opening angle of 20 & DEG;-30 & DEG;. Here, we model the cocoon and calculate its EM emission. Our 2D hydrodynamic simulations suggest that the density and energy distributions, after entering homologous expansion, are well-fitted with power-law functions, in each of the relativistic and non-relativistic parts of the escaped cocoon. Modelling these features, we calculate the cooling emission analytically. We find that the cocoon outshines the r-process kilonova/macronova at early times (10-10(3) s), peaking at UV bands. The relativistic velocity of the cocoon's photosphere is measurable with instruments such as Swift, ULTRASAT, and LSST. We also imply that energetic cocoons, including failed jets, might be detected as X-ray flashes. Our model clarifies the physics and parameter dependence, covering a wide variety of central engines and ejecta of NS mergers and sGRBs in the multimessenger era.

Automated summary

In the GW170817 gravitational wave event, a 10-hour gap without detection of the cocoon was observed before electromagnetic observations. The cocoon is formed by a short gamma-ray burst jet passing through the ejecta of a neutron star merger. Our simulations and calculations show that the cocoon emits strong UV radiation, outshining the r-process kilonova/macronova at early times. The relativistic velocity of the cocoon can be measured, and energetic cocoons may be detected as X-ray flashes.