This simulation shows how to evolve a stable, single neutron star. It uses a TOV solution as initial data and follows the initial (numerical) perturbations, writing the maximum density to disk. What can be seen is that the star oscillates for a few cycles (only very slightly because the solution is stationary and the induced numerical perturbation is small), before numerical errors due to the lack of resolution spoil the results. The size of this simulation is intentionally kept as small as possible, thus the resolution is about as low possible without loosing any confidence in at least quantitatively correct results. It is intended to be used as quick example in lectures, workshops or summer schools where both time and computational power are typically scarce.
|Thornlist||ET Proca release (ET_2019_03)|
|approx. memory||0.25 GB|
|approx. runtime||2.5 hrs using 1 CPU|