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首页> 外文期刊>Astronomy and astrophysics >Consistent accretion-induced heating of the neutron-star crust in MXB 1659?29 during two different outbursts ?
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Consistent accretion-induced heating of the neutron-star crust in MXB 1659?29 during two different outbursts ?

机译：在两次不同的爆发过程中，MXB 1659？29中的中子星地壳不断吸积诱发的加热？

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Monitoring the cooling of neutron-star crusts heated during accretion outbursts allows us to infer the physics of the dense matter present in the crust. We examine the crust cooling evolution of the low-mass X-ray binary MXB 1659?29 up to ～505 days after the end of its 2015 outburst (hereafter outburst II) and compare it with what we observed after its previous 1999 outburst (hereafter outburst I) using data obtained from the Swift , XMM-Newton , and Chandra observatories. The observed effective surface temperature of the neutron star in MXB 1659???29 dropped from ～92 eV to ～56 eV from ～12 days to ～505 days after the end of outburst II. The most recently performed observation after outburst II suggests that the crust is close to returning to thermal equilibrium with the core. We model the crust heating and cooling for both its outbursts collectively to understand the effect of parameters that may change for every outburst (e.g. the average accretion rate, the length of outburst, the envelope composition of the neutron star at the end of the outburst) and those which can be assumed to be the same during these two outbursts (e.g. the neutron star mass, its radius). Our modelling indicates that all parameters were consistent between the two outbursts with no need for any significant changes. In particular, the strength and the depth of the shallow heating mechanism at work (in the crust) were inferred to be consistent during both outbursts, contrary to what has been found when modelling the cooling curves after multiple outburst of another source, MAXI J0556?332. This difference in source behaviour is not understood. We discuss our results in the context of our current understanding of cooling of accretion-heated neutron-star crusts, and in particular with respect to the unexplained shallow heating mechanism.
机译：监测在增生爆发过程中加热的中子星地壳的冷却，使我们能够推断出地壳中存在的致密物质的物理性质。我们研究了低质量X射线二进制MXB 1659？29在其2015年爆发（此后为爆发II）结束后直至505天之前的地壳冷却演化，并将其与我们在1999年先前爆发后（此后）观察到的情况进行了比较。 I）使用从Swift，XMM-Newton和Chandra天文台获得的数据爆发。爆发II结束后，从MXB 1659〜29观测到的中子星的有效表面温度从〜92 eV〜〜56 eV从〜12天降至〜505天。爆发II之后最近进行的观测表明，地壳接近与岩心恢复热平衡。我们共同模拟两个爆发的地壳加热和冷却，以了解每个爆发可能改变的参数的效果（例如，平均吸积率，爆发长度，爆发末尾中子星的包壳成分）以及在这两次爆发中可以被假定为相同的那些（例如中子星质量，其半径）。我们的模型表明，两次爆发之间的所有参数都是一致的，无需进行任何重大更改。特别是，在两次爆发期间，工作中（在地壳中）浅层加热机制的强度和深度被推定为一致的，这与在另一个源MAXI J0556多次爆发后对冷却曲线进行建模时发现的结果相反。 332。源行为的这种差异尚不明确。我们在目前对吸积加热的中子星结壳的冷却，特别是对无法解释的浅层加热机理的理解的背景下讨论我们的结果。

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