Equilibrium sequences of differentially rotating stars with post-merger-like rotational profiles

ABSTRACT We present equilibrium sequences of rotating relativistic stars, constructed with a new rotation law that was proposed by Uryū et al. (2017). choose rotational parameters motivated simulations binary neutron star merger remnants, but otherwise adopt cold, N = 1 polytropic EOS, in order to perform detailed comparison published used the Komatsu, Eriguchi and Hachisu (1989) law. find small influence choice on mass models somewhat larger their radius. The versatility allows us construct have similar profile axial ratio as observed for while at same time being quasi-spherical. More specifically, we sequence variations different degrees differential identify type A C solutions, corresponding types classification Ansorg, Gondek-Rosińska Villain (2009). While our are highly accurate solutions fully general structure equations, demonstrate relevant remnants IWM-CFC approximation still maintains an acceptable accuracy.