Abstract
The merger of a binary neutron star (BNS) system can lead to different final states depending on the total mass of the binary system and the equation of state (EOS). One of the possible outcomes of the merger is a long-lived (lifetime > 10 ms), compact and differentially rotating remnant. The Komatsu, Eriguchi and Hachisu (1989) differential rotation law (KEH) has been used almost exclusively in the literature to describe such configurations, despite the tension with corresponding rotational profiles reported from numerical simulations. New rotation laws suggested by Uryu et al. (2017) aspire to ease this tension and provide more realistic choices to describe the rotational profiles of BNS merger remnants. We recently started constructing equilibrium models with one of the new rotation laws proposed and comparing their physical properties to the KEH rotation law counterpart models. In addition, building on earlier work, the accuracy of the IWM-CFC conformal flatness approximation with the new differential rotation law was confirmed.
Highlights
Differential rotation in relativistic stars has drawn a steady research interest because it is relevant in phenomena such as binary neutron star (BNS) mergers that can provide information through gravitational and electromagnetic waves observations for the behaviour of matter at high densities, i.e., the equation of state (EOS)
M of the BNS is greater than the maximum mass of a cold, uniformly rotating neutron star, Mmax,rot, the compact remnant that is formed during the merger can survive for several tens of milliseconds supported by differential rotation and thermal pressure
In [8], we found that the versatility of the new Uryu+ rotation law allowed for the construction of equilibrium solutions with a rotational profile much closer to the one observed for merger remnants in numerical simulations, while at the same time dwelling in the realm of type A solutions [18]
Summary
Differential rotation in relativistic stars has drawn a steady research interest because it is relevant in phenomena such as binary neutron star (BNS) mergers that can provide information through gravitational and electromagnetic waves observations for the behaviour of matter at high densities, i.e., the equation of state (EOS). Several aspects of the merger remnant are neglected in order to obtain idealized models of its structure. Enriching these initial idealized models by adding gradually, selected realistic components of the binary coalescence problem ensures that this method can still provide useful insights
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