A Chandra observation of the long-duration X-ray transient KS 1731–260 in quiescence: too cold a neutron star?

After more than a decade of actively accreting at about a tenth of the Eddington critical mass accretion rate, the neutron-star X-ray transient KS 1731–260 returned to quiescence in early 2001. We present a Chandra/ACIS-S observation taken several months after this transition. We detected the source at an unabsorbed flux of ∼ 2 × 10 erg cm s (0.5–10 keV). For a distance of 7 kpc, this results in a 0.5–10 keV luminosity of ∼ 1 × 10 erg s and a bolometric luminosity approximately twice that. This quiescent luminosity is very similar to that of the other quiescent neutron star systems. However, if this luminosity is due to the cooling of the neutron star, this low luminosity may indicate that the source spends at least several hundreds of years in quiescence in between outbursts for the neutron star to cool. If true, then it might be the first such X-ray transient to be identified and a class of hundreds of similar systems may be present in the Galaxy. Alternatively, enhanced neutrino cooling could occur in the core of the neutron star which would cool the star more rapidly. However, in that case the neutron star in KS 1731–260 would be more massive than those in the prototypical neutron star transients (e.g., Aql X-1 or 4U 1608–52). Subject headings: accretion, accretion disks — stars: individual (KS 1731–260)— X-rays: stars Center for Space Research, Massachusetts Institute of Technology, 77 Massachusetts Avenue, Cambridge, MA 02139-4307, USA; [email protected] NASA/Goddard Space Flight Center, Code 662, Greenbelt, MD 20771 Astronomical Institute “Anton Pannekoek”, University of Amsterdam, Kruislaan 403, NL-1098 SJ Amsterdam, The Netherlands