XMM-Newton observations of the low-mass X-ray binary EXO 0748-676 in quiescence

TL;DR

This study monitors the cooling of a neutron star in a low-mass X-ray binary over 19 months using XMM-Newton, revealing thermal evolution consistent with standard cooling models and constraining neutron star properties.

Contribution

First long-term X-ray spectral monitoring of EXO 0748-676 in quiescence, providing insights into neutron star cooling and constraining its mass, radius, and distance.

Findings

Neutron star crust temperature decreased by 10% over 19 months.

Thermal luminosity declined by 40%, indicating cooling.

Results support a medium-mass neutron star with standard cooling mechanisms.

Abstract

The neutron star low-mass X-ray binary EXO 0748-676 started a transition from outburst to quiescence in August 2008, after more than 24 years of continuous accretion. The return of the source to quiescence has been monitored extensively by several X-ray observatories. Here, we report on four XMM-Newton observations elapsing a period of more than 19 months and starting in November 2008. The X-ray spectra show a soft thermal component which we fit with a neutron star atmosphere model. Only in the first observation do we find a significant second component above ~ 3 keV accounting for ~ 7 % of the total flux, which could indicate residual accretion. The thermal bolometric flux and the temperature of the neutron star crust decrease steadily by 40 and 10 % respectively between the first and the fourth observation. At the time of the last observation, June 2010, we obtain a thermal bolometric luminosity of 5.6 x 10$^{33}$ (d/7.1 kpc)$^2$ erg s$^{-1}$ and a temperature of the neutron star crust of 109 eV. The cooling curve is consistent with a relatively hot, medium-mass neutron star, cooling by standard mechanisms. From the spectral fits to a neutron star atmosphere model we infer limits for the mass and the radius of the neutron star. We find that in order to achieve self-consistency for the NS mass between the different methods, the value of the distance is constrained to be <~6 kpc. For this value of the distance, the derived mass and radius contours are consistent with a number of EoSs with nucleons and hyperons.