The neutron star in HESS J1731-347: CCOs as laboratories to study the equation of state of superdense matter

TL;DR

This study analyzes the neutron star in HESS J1731-347 using new XMM-Newton data and atmosphere models, providing constraints on its physical parameters and implications for the equation of state of superdense matter.

Contribution

It presents improved spectral analysis of the CCO with atmosphere models, constrains its distance, mass, radius, and temperature, and discusses cooling scenarios relevant to superdense matter.

Findings

Atmosphere models fit the spectrum better than blackbody models.

Hydrogen atmosphere models suggest distances above 7-8 kpc, which are less plausible.

Carbon atmosphere models favor a distance of 3-6 kpc, consistent with Galactic spiral arms.

Abstract

Context: Central Compact Objects (CCOs) in supernova remnants are isolated thermally emitting neutron stars (NSs). They are most probably characterized by a magnetic field strength that is roughly two orders of magnitude lower than that of most of the radio and accreting pulsars. The thermal emission of CCOs can be modeled to obtain constraints on the physical parameters of the star such as its mass, radius, effective temperature, and chemical composition. Aims: The CCO in HESS, J1731-347 is one of the brightest objects of this class. We present our analysis of two new XMM-Newton observations of the source which increase the total exposure time of the by a factor of five compared to the analyses presented before. Methods: We use our numerical spectral models for carbon and hydrogen atmospheres to fit the spectrum of the CCO. From our fits, we derive constraints on the physical parameters of the emitting star. We also use the new data to derive new upper limits on pulsations and to confirm the absence of a long-term variability. Results: The analysis shows that atmosphere spectral models are clearly preferred by the fit over the blackbody function. Under the assumption that the X-ray emission is uniformly produced by the entire star surface, hydrogen atmosphere models lead to uncomfortably large distances of the CCO, above 7-8 kpc. On the other hand, the carbon atmosphere model formally excludes distances above 5-6 kpc and is compatible with the source located in the Scutum-Crux (3 kpc) or Norma-Cygnus (4.5 kpc) Galactic spiral arm. We provide and discuss the corresponding confidence contours in the NS mass-radius plane. The measured effective temperature indicates that the NS is exceptionally hot for the estimated age of 30 kyr. We discuss possible cooling scenarios to explain this property, as well as possible additional constraints on the star mass and radius from cooling theory.