论文标题
3xmm J185246.6+003317作为磁场低的磁场的证据
Evidence for 3XMM J185246.6+003317 as a massive magnetar with a low magnetic field
论文作者
论文摘要
3xmm J185246.6+003317是一个瞬态磁铁，位于超新星残留物Kes \，79的附近。到目前为止，观察结果仅设定了其表面磁场并旋转的上限，并且对其质量和半径没有估计。使用射线追踪建模和贝叶斯推断，分析了大约三周的几个光曲线，我们发现它可能是迄今为止最庞大的中子恒星之一。此外，我们的分析表明具有亚临界场强度和碳大气组成的多极磁场结构。由于可用光曲线的时间分辨率限制，我们估计表面磁场和质量为$ \ log_ {10}（b/{\ rm g}）= 11.89^{+0.19} _ { - 0.93} $ { - 0.93} $ and $ m = 2.09^{+0.16^{+0.16^{+0.16}} $1σ$置信水平，而半径估计为$ r = 12.02^{+1.44} _ { - 1.42} $ km，$2σ$置信度。通过模拟，即具有已知模型参数的数据注射及其随后的恢复。最合适的型号具有三个小热点，其中两个在南半球。但是，这些只是基于具有各向异性发射的简单射线追踪模型的首先估计和结论。我们还估计建模对参数不确定性的影响以及将重点放在更精确的分析中的相关现象。我们将上述最佳拟合结果解释为由于超新星层/星际培养基的积聚到3xmm J185246.6+003317上，导致埋葬并随后磁场的再出现，并且由于氢/想要型想要形式而形成了碳气氛。最后，我们简要讨论了我们发现对超密集物质约束的一些后果。
3XMM J185246.6+003317 is a transient magnetar located in the vicinity of the supernova remnant Kes\,79. So far, observations have only set upper limits to its surface magnetic field and spindown, and there is no estimate for its mass and radius. Using ray-tracing modelling and Bayesian inference for the analysis of several light curves spanning a period of around three weeks, we have found that it may be one of the most massive neutron stars to date. In addition, our analysis suggests a multipolar magnetic field structure with a subcritical field strength and a carbon atmosphere composition. Due to the time-resolution limitation of the available light curves, we estimate the surface magnetic field and the mass to be $\log_{10} (B/{\rm G}) = 11.89^{+0.19}_{-0.93}$ and $M=2.09^{+0.16}_{-0.09}$~$M_{\odot}$ at $1σ$ confidence level, while the radius is estimated to be $R=12.02^{+1.44}_{-1.42}$ km at $2σ$ confidence level. They were verified by simulations, i.e., data injections with known model parameters, and their subsequent recovery. The best-fitting model has three small hot spots, two of them in the southern hemisphere. These are, however, just first estimates and conclusions, based on a simple ray-tracing model with anisotropic emission; we also estimate the impact of modelling on the parameter uncertainties and the relevant phenomena on which to focus in more precise analyses. We interpret the above best-fitting results as due to accretion of supernova layers/interstellar medium onto 3XMM J185246.6+003317 leading to burying and a subsequent re-emergence of the magnetic field, and a carbon atmosphere being formed possibly due to hydrogen/helium diffusive nuclear burning. Finally, we briefly discuss some consequences of our findings for superdense matter constraints.
