Rapid Cooling of the Neutron Star in the Quiescent Super-Eddington Transient XTE J1701-462

TL;DR

This study observes the rapid cooling of a neutron star's crust after a super-Eddington outburst, revealing a highly conductive crust and providing insights into neutron star thermal evolution.

Contribution

It provides the first detailed measurement of neutron star crust cooling timescale following a super-Eddington outburst, indicating high crust conductivity.

Findings

Crust cooling timescale of ~120 days

Crust is highly conductive

Surface temperature ~125 eV at equilibrium

Abstract

We present Rossi X-Ray Timing Explorer and Swift observations made during the final three weeks of the 2006-2007 outburst of the super-Eddington neutron star (NS) transient XTE J1701-462, as well as Chandra and XMM-Newton observations covering the first ~800 days of the subsequent quiescent phase. The source transitioned quickly from active accretion to quiescence, with the luminosity dropping by over 3 orders of magnitude in ~13 days. The spectra obtained during quiescence exhibit both a thermal component, presumed to originate in emission from the NS surface, and a non-thermal component of uncertain origin, which has shown large and irregular variability. We interpret the observed decay of the inferred effective surface temperature of the NS in quiescence as the cooling of the NS crust after having been heated and brought out of thermal equilibrium with the core during the outburst. The interpretation of the data is complicated by an apparent temporary increase in temperature ~220 days into quiescence, possibly due to an additional spurt of accretion. We derive an exponential decay timescale of ~120 (+30/-20) days for the inferred temperature (excluding observations affected by the temporary increase). This short timescale indicates a highly conductive NS crust. Further observations are needed to confirm whether the crust is still slowly cooling or has already reached thermal equilibrium with the core at a surface temperature of ~125 eV. The latter would imply a high equilibrium bolometric thermal luminosity of ~5x10^{33} erg/s for an assumed distance of 8.8 kpc.