Rudy Wijnands et al 2004 ApJ 606 L61 doi:10.1086/421081
Rudy Wijnands1,2, Jeroen Homan3, Jon M. Miller4,5 and Walter H. G. Lewin3
Show affiliationsWe have observed the quasi-persistent neutron star X-ray transient and eclipsing binary MXB 1659-29 in quiescence on three occasions with Chandra. The purpose of our observations was to monitor the quiescent behavior of the source after its last prolonged (~2.5 yr) outburst that ended in 2001 September. The X-ray spectra of the source are consistent with thermal radiation from the neutron star surface. We found that the bolometric flux of the source decreased by a factor of 7-9 over the timespan of 1.5 yr between our first and last Chandra observations. The effective temperature also decreased, by a factor of 1.6-1.7. The decrease in time of the bolometric flux and effective temperature can be described using exponential decay functions, with e-folding times of ~0.7 and ~3 yr, respectively. Our results are consistent with the hypothesis that we observed a cooling neutron star crust that was heated considerably during the prolonged accretion event and that is still out of thermal equilibrium with the neutron star core. We could only determine upper limits for any luminosity contribution because of the thermal state of the neutron star core. The rapid cooling of the neutron star crust implies that it has a large thermal conductivity. Our results also suggest that enhanced cooling processes are present in the neutron star core.
accretion, accretion disks; stars: individual (MXB 1659−29); stars: neutron; X-rays: stars
Issue 1 (2004 May 1)
Received 2003 October 21, accepted for publication 2004 March 18
Published 2004 April 7
Rudy Wijnands et al 2004 ApJ 606 L61
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