We fit the observed high ionisation X-ray absorption lines in the neutron star binary GX13+1 with a full simulation of a thermal-radiative wind. This uses a radiation hydrodynamic code coupled to Monte Carlo radiation transfer to compute the observed line profiles from Hydrogen and Helium-like iron and Nickel, including all strong K{\alpha} and K{\beta} transitions. The wind is very strong as this object has a very large disc and is very luminous. The absorption lines from Fe K{\alpha} are strongly saturated as the ion columns are large, so the line equivalent widths (EWs) depend sensitively on the velocity structure. We additionally simulate the lines including isotropic turbulence at the level of the azimuthal and radial velocities. We fit these models to the Fe xxv and xxvi absorption lines seen in the highest resolution Chandra third order HETGS data. These data already rule out the addition of turbulence at the level of the radial velocity of ~500 km/s. The velocity structure predicted by the thermal-radiative wind alone is a fairly good match to the observed profile, with an upper limit to additional turbulence at the level of the azimuthal velocity of ~100 km/s. This gives stringent constraints on any remaining contribution from magnetic acceleration.

中文翻译：

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中子星低质量X射线双星GX 13 + 1中的热辐射风

我们用热辐射风的完整模拟拟合了中子星双星 GX13+1 中观察到的高电离 X 射线吸收线。这使用与蒙特卡罗辐射传递耦合的辐射流体动力学代码来计算观察到的氢和类氦铁和镍的线轮廓，包括所有强 K{\alpha} 和 K{\beta} 跃迁。风非常大，因为这个物体有一个非常大的圆盘并且非常发光。由于离子柱很大，来自 Fe K{\alpha} 的吸收线强烈饱和，因此线等效宽度 (EW) 敏感地取决于速度结构。我们还在方位角和径向速度的水平上模拟了包括各向同性湍流的线。我们将这些模型拟合到最高分辨率 Chandra 三阶 HETGS 数据中看到的 Fe xxv 和 xxvi 吸收线。这些数据已经排除了在约 500 公里/秒的径向速度水平上增加的湍流。仅由热辐射风预测的速度结构与观察到的剖面相当吻合，在大约 100 公里/秒的方位速度水平上附加湍流的上限。这对磁加速度的任何剩余贡献给出了严格的限制。在大约 100 km/s 的方位角速度水平上附加湍流的上限。这对磁加速度的任何剩余贡献给出了严格的限制。在大约 100 km/s 的方位角速度水平上附加湍流的上限。这对磁加速度的任何剩余贡献给出了严格的限制。