MG11 
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Abstract

The final fate of binary neutron star systems: What happens after the merger? The final fate of binary neutron star systems: What happens after the merger?

The merger of two neutron stars usually produces a remnant with a mass significantly above the single (nonrotating) neutron star maximum mass. In some cases, the remnant will be stabilized against collapse by rapid, differential rotation. MHD-driven angular momentum transport eventually leads to the collapse of the remnant's core, resulting in a black hole surrounded by a massive accreting torus. In this talk, I present simulations of this process using numerical relativistic MHD. I discuss numerical issues involved in simulating the remnant before and after the appearance of the black hole. The plausibility of generating short-duration gamma-ray bursts through this scenario is also discussed.

A new code for evolving relativistic fluid spacetimes

I present a new code for solving the coupled Einstein-hydrodynamics equations to evolve relativistic, self-gravitating fluids. The Einstein field equations are solved on one grid using pseudospectral methods, while the fluids are evolved on another grid by finite differencing. I discuss implementation details, such as the communication between the grids and the treatment of stellar surfaces, and present code tests. Applications to compact binaries are discussed.