  Events GW170817 and GRB 170817A provide the best confirmation so far that
compact binary mergers where at least one of the companions is a neutron star
(NS) can be the progenitors of short gamma-ray bursts (sGRBs). An open question
for GW170817 remains the values and impact of the initial NS spins. The initial
spins could possibly affect the remnant black hole (BH) mass and spin, the
remnant disk and the formation and lifetime of a jet and its luminosity. Here
we summarize our general relativistic magnetohydrodynamic simulations of
spinning, NS binaries undergoing merger and delayed collapse to a BH. The
binaries consist of two identical NSs, modeled as $\Gamma=2$ polytropes, in
quasicircular orbit, each with spins $\chi_{\rm{NS}}=-0.053,\,0,\,0.24$, or
$0.36$. The stars are endowed initially with a dipolar magnetic field extending
from the interior into the exterior, as in a radio pulsar. Following merger,
the redistribution of angular momentum by magnetic braking and magnetic
turbulent viscosity in the hypermassive neutron star (HMNS) remnant, along with
the loss of angular momentum due to gravitational radiation, induce the
formation of a massive, nearly uniformly rotating inner core surrounded by a
magnetized Keplerian disk-like envelope. The HMNS eventually collapses to a BH,
with spin $a/M_{\rm BH} \simeq 0.78$ independent of the initial spin of the
NSs, surrounded by a magnetized accretion disk. The larger the initial NS spin
the heavier the disk. After $\Delta t\sim 3000-4000 M \sim 45-60(M_{\rm
NS}/1.625M_\odot)\rm ms$ following merger, a mildly relativistic jet is
launched. The lifetime of the jet [$\Delta t\sim 100-140(M_{\rm
NS}/1.625M_\odot)\rm ms$] and its outgoing Poynting luminosity [$L_{\rm EM}\sim
10^{51.5\pm 1}\rm erg/s$] are consistent with typical sGRBs, as well as with
the Blandford--Znajek mechanism for launching jets and their associated
Poynting luminosities.
