2016ApJ...819..120L -
Astrophys. J., 819, 120 (2016/March-2)
Shock breakout driven by the remnant of a neutron star binary merger: an X-ray precursor of mergernova emission.
LI S.-Z. and YU Y.-W.
Abstract (from CDS):
A supra-massive neutron star (NS) spinning extremely rapidly could survive from a merger of an NS-NS binary. The spin-down of this remnant NS that is highly magnetized could power the isotropic merger ejecta to produce a bright mergernova emission in the ultraviolet/optical bands. Before the mergernova, the early interaction between the NS wind and the ejecta could drive a forward shock propagating outward into the ejecta. As a result, a remarkable amount of heat can be accumulated behind the shock front and the final escape of this heat could produce a shock breakout emission. We describe the dynamics and thermal emission of this shock with a semi-analytical model. It is found that a few hours after the merger, by leading the mergernova emission as a precursor, sharp and luminous breakout emission appears mainly in soft X-rays, with a luminosity of ∼1045 erg s–1. Therefore, the detection of such an X-ray precursor could provide evidence for identifying NS-powered mergernovae and distinguishing them from radioactivity-powered novae (i.e., kilonovae or macronovae). The discovery of NS-powered mergernovae could finally help to confirm the gravitational wave signals due to the mergers and the existence of supra-massive NSs.
Abstract Copyright:
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Journal keyword(s):
gamma-ray burst: general - stars: neutron - supernovae: general
Simbad objects:
3
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