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首页> 外文期刊>The Astrophysical journal >MONITORING CHANDRA OBSERVATIONS OF THE QUASI-PERSISTENT NEUTRON STAR X-RAY TRANSIENT MXB 1659-29 IN QUIESCENCE: THE COOLING CURVE OF THE HEATED NEUTRON STAR CRUST
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MONITORING CHANDRA OBSERVATIONS OF THE QUASI-PERSISTENT NEUTRON STAR X-RAY TRANSIENT MXB 1659-29 IN QUIESCENCE: THE COOLING CURVE OF THE HEATED NEUTRON STAR CRUST

机译：静止的准持久中子星X射线瞬态MXB 1659-29的监测钱德拉观测：加热的中子星壳的冷却曲线

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摘要

We 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.
机译：我们已经用Chandra观察了准持久的中子星X射线瞬变并以静态方式使双星MXB 1659-29黯然失色。我们观察的目的是监视源于2001年9月结束的最后一次长时间（〜2.5年）爆发后的静态行为。源的X射线光谱与来自中子星表面的热辐射一致。我们发现，在我们的第一个和最后一个钱德拉观测之间，辐射源的辐射热通量在1.5年的时间跨度内下降了7-9倍。有效温度也降低了1.6-1.7倍。辐射热通量和有效温度的减少可以用指数衰减函数来描述，电子折叠时间分别为〜0.7和〜3年。我们的结果与以下假设相符：我们观察到冷却的中子星外壳在长时间的积聚过程中被相当大地加热，但仍然与中子星芯没有达到热平衡。由于中子星核的热态，我们只能确定任何光度贡献的上限。中子星地壳的快速冷却意味着它具有很大的热导率。我们的结果还表明，中子星核中存在增强的冷却过程。

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