A change in the quiescent X-ray spectrum of the neutron star low-mass X-ray binary MXB 1659-29

TL;DR

This study tracks the long-term X-ray spectral evolution of the neutron star binary MXB 1659-29, revealing unexpected changes in quiescent emission that challenge simple cooling models and suggest complex disk or absorption effects.

Contribution

It presents the first long-term, multi-epoch X-ray spectral analysis of MXB 1659-29, highlighting unexpected spectral changes years into quiescence.

Findings

A significant drop in count rate and spectral change after 11 years in quiescence.

Possible explanations include increased absorption or a sudden drop in neutron star temperature.

The results suggest complex accretion disk or absorption dynamics during quiescence.

Abstract

The quasi-persistent neutron star low-mass X-ray binary MXB 1659-29 went into quiescence in 2001, and we have followed its quiescent X-ray evolution since. Observations over the first 4 years showed a rapid drop in flux and temperature of the neutron star atmosphere, interpreted as cooling of the neutron star crust which had been heated during the 2.5 year outburst. However, observations taken approximately 1400 and 2400 days into quiescence were consistent with each other, suggesting the crust had reached thermal equilibrium with the core. Here we present a new Chandra observation of MXB 1659-29 taken 11 years into quiescence and 4 years since the last Chandra observation. This new observation shows an unexpected factor of ~3 drop in count rate and change in spectral shape since the last observation, which cannot be explained simply by continued cooling. Two possible scenarios are that either the neutron star temperature has remained unchanged and there has been an increase in the column density, or, alternatively the neutron star temperature has dropped precipitously and the spectrum is now dominated by a power-law component. The first scenario may be possible given that MXB 1659-29 is a near edge-on system, and an increase in column density could be due to build-up of material in, and a thickening of, a truncated accretion disk during quiescence. But, a large change in disk height may not be plausible if standard accretion disk theory holds during quiescence. Alternatively, the disk may be precessing, leading to a higher column density during this latest observation.