Constraining the nuclear equation of state via gravitational-wave radiation of short gamma-ray burst remnants

Abstract

The observed internal plateau of X-ray emission in some short GRBs suggests the formation of a remnant supra-massive magnetar following a double neutron star (NS) merger. In this paper, we assume that the rotational energy is lost mainly via gravitational wave (GW) radiation instead of magnetic dipole (MD) radiation, and present further constraints on the NS nuclear equation of state (EoS) via mass quadrupole deformation and r-mode fluid oscillations of the magnetar. We present two short GRBs with measured redshifts, 101219A and 160821B, whose X-ray light curves exhibit an internal plateau. This suggests that a supra-massive NS may survive as the central engine. By considering twelve NS EoSs, within the mass quadrupole deformation scenario we find that the GM1, DD2, and DDME2 models give an $M_{\mathrm{p}}$ band falling within the 2$\sigma$ region of the proto-magnetar mass distribution for $\epsilon =0.01$. This is consistent with the constraints from the MD radiation dominated model of rotational energy loss. However, for an r-mode fluid oscillation model with $\alpha =0.1$ the data suggest that the NS EOS is close to the Shen and APR models, which is obviously different from the MD radiation dominated and mass quadrupole deformation cases.

7 pages, 1 table, and 4 figures. ApJ in press, matched the published version

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• The evolution effects of radius and moment of inertia for rapidly rotating neutron stars
• Gravitational-wave evolution of newborn magnetars with different deformed structure