  In this work, we study the merger of two neutron stars with a gravitational
mass of 1.4 M_sol each, employing the Shen-Horowitz-Teige equation of state.
This equation of state is a corner case, allowing the formation of a stable
neutron star with the given total baryonic mass of 3.03 M_sol. We investigate
in unprecedented detail the structure of the remnant, in particular the mass
distribution, the thermal structure, and the rotation profile. We also compute
fluid trajectories both inside the remnant and those relevant for the formation
of the disk. We find a peanut-shaped fluid flow inside the remnant following a
strong m=2 perturbation. Moreover, the flow is locally compressive, causing the
appearance of dynamic hot spots. Further, we introduce new diagnostic measures
that are easy to implement in numeric simulations and that allow to quantify
mass and compactness of merger remnants in a well-defined way. As in previous
studies of supra- and hypermassive stars, we find a remnant with a slowly
rotating core and an outer envelope rotating at nearly Keplerian velocity. We
compute a Tolman-Oppenheimer-Volkoff star model which agrees well with that of
the remnant in the core, while the latter possesses extensive outer layers
rotating close to Kepler velocity. Finally, we extract the gravitational wave
signal and discuss the detectability with modern observatories. This study has
implications for the interpretation of gravitational wave detections from the
post-merger phase, and is relevant for short gamma-ray burst models.
