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

Striped Jets in Post Neutron Star Merger Systems