A signification fraction of Galactic massive stars (> 8Mo) are ejected from their parent cluster and supersonically sail away through the interstellar medium (ISM). The winds of these fast-moving stars blow asymmetric bubbles thus creating a circumstellar environment in which stars eventually die with a supernova explosion. The morphology of the resulting remnant is largely governed by the circumstellar medium of the defunct progenitor star. In this paper, we present 2D magneto-hydrodynamical simulations investigating the effect of the ISM magnetic field on the shape of the supernova remnants of a 35Mo star evolving through a Wolf-Rayet phase and running with velocity 20 and 40 km/s, respectively. A 7 microG ambient magnetic field is sufficient to modify the properties of the expanding supernova shock front and in particular to prevent the formation of filamentary structures. Prior to the supernova explosion, the compressed magnetic field in the circumstellar medium stabilises the wind/ISM contact discontinuity in the tail of the wind bubble. A consequence is a reduced mixing efficiency of ejecta and wind materials in the inner region of the remnant, where the supernova shock wave propagates. Radiative transfer calculations for synchrotron emission reveal that the non-thermal radio emission has characteristic features reflecting the asymmetry of exiled core-collapse supernova remnants from Wolf-Rayet progenitors. Our models are qualitatively consistent with the radio appearance of several remnants of high-mass progenitors, namely the bilateral G296.5+10.0 and the shell-type remnants CTB109 and Kes 17, respectively.
沃尔夫-拉叶星（WR）是大质量（$\geq$ 10 M $_{\odot}$）演化的恒星，在其核心经历高级核燃烧，迅速接近超新星生命的终点。它们强大的风使星际介质富含重元素，为未来的恒星提供原材料。我们简要总结了WR星的高能过程，主要集中在它们的X射线发射。我们提出了新的结果，从钱德拉观测的食WR+O二进制CQ Cep覆盖一个完整的轨道，严格测试X射线发射模型。
Modelling the thermal X-ray emission around the Galactic centre from colliding Wolf-Rayet winds
我们计算的热X射线发射的流体动力学模拟的30个沃尔夫-拉叶（WR）星轨道内的Sgr A $^*$秒差距，解释钱德拉X射线观测的目的是在这个地区。该模型很好地再现了观测的光谱形状，表明冲击WR风是这种热辐射的主要来源。模型X射线通量与Sgr A $^*$流出的强度相关，该流出将Sgr A $^*$附近的热气清除。适度的外流最符合目前的观测结果，尽管这个超大质量黑洞（SMBH）的外流在$\sim$ 100年前就结束了。
The Wolf-Rayet + Black Hole Binary NGC 300 X-1: What is the Mass of the Black Hole?
利用钱德拉X射线天文台和哈勃空间望远镜宇宙起源光谱仪对Wolf-Rayet +黑洞双星系统NGC 300 X-1进行了新的X射线和紫外观测。当与档案X射线观测相结合时，我们的X射线和紫外线观测对整个双星轨道进行采样，为系统几何形状和黑洞吸积盘与施主星风之间的相互作用提供线索。我们测量的双星轨道周期为32.7921 $\pm$ 0.0003小时，与以前的研究一致，并使用X射线数据进行相位分辨光谱。X射线光变曲线揭示了一个深食，与$i=60-75^{\circ}$的倾角一致，以及与吸积流撞击盘边缘一致的食前过剩。我们进一步测量径向速度变化的几个突出的FUV谱线，最显着的He II $λ$ 1640和C IV $λ$ 1550。我们发现，He II发射线系统滞后于预期的沃尔夫-拉叶星轨道运动的相位差$Δϕ\sim0.3$，而C IV $λ$ 1550匹配的相位预期的径向速度曲线的沃尔夫-拉叶施主。我们假设C IV $λ$ 1550发射线遵循正弦径向速度曲线（半振幅= 250 km s $^{-1}$），并推断BH质量为17 $\pm$ 4 M $_{\odot}$。我们的观察结果是一致的风-洛希瓣溢出吸积盘的存在下，吸积流的形式从引力集中的风材料和影响的黑洞吸积盘的边缘。
