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      Smooth equations of state for high-accuracy simulations of neutron star binaries

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          Abstract

          High-accuracy numerical simulations of merging neutron stars play an important role in testing and calibrating the waveform models used by gravitational wave observatories. Obtaining high-accuracy waveforms at a reasonable computational cost, however, remains a significant challenge. One issue is that high-order convergence of the solution requires the use of smooth evolution variables, while many of the equations of state used to model the neutron star matter have discontinuities, typically in the first derivative of the pressure. Spectral formulations of the equation of state have been proposed as a potential solution to this problem. Here, we report on the numerical implementation of spectral equations of state in the Spectral Einstein Code. We show that, in our code, spectral equations of state allow for high-accuracy simulations at a lower computational cost than commonly used `piecewise polytrope' equations state. We also demonstrate that not all spectral equations of state are equally useful: different choices for the low-density part of the equation of state can significantly impact the cost and accuracy of simulations. As a result, simulations of neutron star mergers present us with a trade-off between the cost of simulations and the physical realism of the chosen equation of state.

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          Cavefish Study Supports Controversial Evolutionary Mechanism

          E Pennisi (2013)
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            Author and article information

            Journal
            14 August 2019
            Article
            1908.05277
            e788c479-ee87-4e84-a37e-f97a2f86fd37

            http://arxiv.org/licenses/nonexclusive-distrib/1.0/

            History
            Custom metadata
            Submitted to PRD, 13p, 7 figures, 3 tables
            gr-qc astro-ph.HE

            General relativity & Quantum cosmology,High energy astrophysical phenomena

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