  Models invoking magnetic reconnection as the particle acceleration mechanism
within relativistic jets often adopt a gradual energy dissipation profile
within the jet. However, such a profile has yet to be reproduced in
first-principles simulations. Here, we perform a suite of 3D general
relativistic magnetohydrodynamic simulations of post-neutron star merger disks
with an initially purely toroidal magnetic field. We explore the variations in
both the microphysics (e.g., nuclear recombination, neutrino emission) and
system parameters (e.g., disk mass). In all our simulations, we find the
formation of magnetically striped jets. The stripes result from the reversals
in the poloidal magnetic flux polarity generated in the accretion disk. The
simulations display large variations in the distributions of stripe duration,
$\tau$, and power, $\langle P_{\Phi} \rangle$. We find that more massive disks
produce more powerful stripes, the most powerful of which reaches $\langle
P_{\Phi} \rangle \sim 10^{49}$~erg~s$^{-1}$ at $\tau \sim 20$~ms. The power and
variability that result from the magnetic reconnection of the stripes agree
with those inferred in short duration gamma-ray bursts. We find that the
dissipation profile of the cumulative energy is roughly a power-law in both
radial distance, $z$, and $\tau$, with the slope in the range, $\sim 1.7-3$;
more massive disks display larger slopes.
