Constraints on neutron star mass and radius in GS 1826-24 from sub-Eddington X-ray bursts

TL;DR

This study uses models of X-ray burst lightcurves and spectral evolution to constrain the neutron star's mass and radius in GS 1826-24, providing limits that suggest a smaller radius than previous estimates.

Contribution

It introduces a method to determine neutron star mass and radius constraints from burst spectral data without relying on distance measurements.

Findings

Upper limit on neutron star radius: 9.0-13.2 km

Upper limit on neutron star mass: 1.2-1.7 solar masses

Distance to GS 1826-24 constrained to less than 4.0-5.5 kpc

Abstract

We investigate the constraints on neutron star mass and radius in GS 1826-24 from models of lightcurves and spectral evolution of type I X-ray bursts. This source shows remarkable agreement with theoretical calculations of burst energies, recurrence times, and lightcurves. We first exploit this agreement to set the overall luminosity scale of the observed bursts. When combined with a measured blackbody normalization, this leads to a distance and anisotropy independent measurement of the ratio between the redshift 1+z and color correction factor f_c. We find 1+z=1.19-1.28 for f_c=1.4-1.5. We then compare the evolution of the blackbody normalization with flux in the cooling tail of bursts with predictions from spectral models of Suleimanov et al. (2011b). The observations are well described by the models at luminosities greater than about one third of the peak luminosity, with deviations emerging at luminosities below that. We show that this comparison leads to distance independent upper limits on R_\infty and neutron star mass of R_\infty\lesssim 9.0-13.2 km and M<1.2-1.7 M_\odot, respectively, for solar abundance of hydrogen at the photosphere and a range of metallicity and surface gravity. The radius limits are low in comparison to previous measurements. This may be indicative of a subsolar hydrogen fraction in the GS 1826-24 photosphere, or of larger color corrections than that predicted by spetral models. Our analysis also gives an upper limit on the distance to GS 1826-24 of d<4.0-5.5 kpc \xi_b^{-1/2}, where \xi_b is the degree of anisotropy of the burst emission.