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We perform magnetohydrodynamic simulations in full general relativity (GRMHD) of a binary black hole-neutron star (BHNS) on a quasicircular orbit that undergoes merger. The binary mass ratio is 3: 1, the black hole initial spin parameter a/m=0. 75 (m is the black hole Christodoulou mass) aligned with the orbital angular momentum, and the neutron star is an irrotational \ =2 polytrope. About two orbits prior to merger (at time t={t₁}), we seed the neutron star with a dynamically weak interior dipole magnetic field that extends into the stellar exterior. At t={t₁}, the exterior has a low-density atmosphere with a constant plasma parameter \ \ {P\ ₆₀ₒ}/{P\ ₌₀₆}. Varying β at tB in the exterior from 0. 1 to 0. 01, we find that at a time \ 4000M\ 100 ({M\ ₍ₒ}/1. 4{M\ }) \\;\ ms (M is the total (ADM) mass) following the onset of accretion of tidally disrupted debris, magnetic winding above the remnant black hole poles builds up the magnetic field sufficiently to launch a mildly relativistic, collimated outflow¿an incipient jet. The duration of the accretion and the lifetime of the jet is \ t\ 0. 5 ({M\ ₍ₒ}/1. 4{M\ }) s. Our simulations furnish the first explicit examples in GRMHD that show that a jet can emerge following a BHNS merger.
Paschalidis et al. (Mon,) studied this question.