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The recent observations of GW170817 and its electromagnetic (EM) counterpartsshow that double neutron star mergers could lead to rich and bright EMemissions. Recent numerical simulations suggest that neutron star and neutronstar/black hole (NS-NS/BH) mergers would leave behind a central remnantsurrounded by a mildly isotropic ejecta. The central remnant could launch acollimated jet and when the jet propagating through the ejecta, a mildlyrelativistic cocoon would be formed and the interaction between the cocoon andthe ambient medium would accelerate electrons via external shock in a wideangle. So that the merger-nova photons (i.e., thermal emission from the ejecta)would be scattered into higher frequency via inverse compton (IC) process whenthey propagating through the cocoon shocked region. We find that the ICscattered component peaks at X-ray band and it will reach its peak luminosityin order of days (simultaneously with the merger-nova emission). With currentX-ray detectors, such a late X-ray component could be detected out to 200 Mpc,depending on the merger remnant properties. It could serve as an importantelectromagnetic counterpart of gravitational wave signals from NS-NS/BHmergers. Nevertheless, simultaneous detection of such a late X-ray signal andthe merger-nova signal could shed light on the cocoon properties and theconcrete structure of the jet.

Inverse compton scattered merger-nova: late X-ray counterpart of gravitational wave signals from NS-NS/BH mergers