Abstract
The merger of two neutron stars often results in a rapidly and differentially rotating hypermassive neutron star (HMNS). We show by numerical-relativity simulation that the magnetic-field profile around such HMNS is dynamically varied during its subsequent evolution, and as a result, electromagnetic radiation with a large luminosity ∼0.1B2R3Ω is emitted with baryons (B, R, and Ω are poloidal magnetic-field strength at stellar surface, stellar radius, and angular velocity of an HMNS). The predicted luminosity of electromagnetic radiation, which is primarily emitted along the magnetic-dipole direction, is ∼1047(B/1013 G)2(R/10 km)3(Ω/104 rad s−1) erg s−1, which is comparable to the luminosity of quasars.
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