标题： 脉冲星风星云与其前身恒星的周围介质相遇 显示英文标题

标题： Pulsar wind nebulae meeting the circumstellar medium of their progenitors

摘要： 高质量恒星相当一部分在星系的星际介质中航行。 一旦它们演化并以核心坍缩超新星的方式死亡，通常会留下一个磁化且旋转的中子星（脉冲星）。 脉冲星的即时周围是脉冲星风，它形成一个星云，其形态由超新星抛射物塑造，并在超新星之前被引导到前身恒星的周围介质中。 因此，不规则的脉冲星风星云表现出各种各样的无线电外观，这些外观被其相互作用的超新星冲击波所屏蔽或包含不对称的上下发射。 在这里，我们展示了一系列2.5维非相对论磁流体动力学模拟，探讨由红超巨星和沃尔夫-拉叶大质量超新星前身恒星产生的脉冲星风星云（PWNe）的演化，这些恒星以马赫数M eq. 到1和M eq. 到2的速度进入银河平面的温暖相。 在这种简化的研究方法中，前身恒星的运动方向、局部环境介质磁场、前身恒星和脉冲星的旋转轴都对齐，这将我们的研究限制在高赤道能量通量的特殊脉冲星风星云上。 我们发现，当脉冲星风星云的终止激波充分嵌入其死亡恒星周围并与其超新星抛射物相互作用时，其回响是不对称的，并且根据其前身恒星过去的周围介质演化而有很大差异，这反映在它们的投影无线电同步辐射发射中。 这种机制在涉及缓慢移动或非常大质量恒星的遗迹中尤为显著。 我们发现，在脉冲星风星云中不对称的回响强烈影响了等离子核心坍缩超新星遗迹中的物质混合。 显示英文摘要

摘要： A significative fraction of high mass stars sail away through the interstellar medium of the galaxies. Once they evolved and died via a core collapse supernova, a magnetized, rotating neutron star (a pulsar) is usually their leftover. The immediate surroundings of the pulsar is the pulsar wind, which forms a nebula whose morphology is shaped by the supernova ejecta, channeled into the circumstellar medium of the progenitor star in the pre supernova time. Consequently, irregular pulsar wind nebulae display a large variety of radio appearances, screened by their interacting supernova blast wave or harboring asymmetric up down emission. Here, we present a series of 2.5 dimensional non relativistic magnetohydrodynamical simulations exploring the evolution of the pulsar wind nebulae (PWNe) generated by a red supergiant and a Wolf Rayet massive supernova progenitors, moving with Mach number M eq. to 1 and M eq. to 2 into the warm phase of the galactic plane. In such a simplified approach, the progenitors direction of motion, the local ambient medium magnetic field, the progenitor and pulsar axis of rotation, are all aligned, which restrict our study to peculiar pulsar wind nebula of high equatorial energy flux. We found that the reverberation of the termination shock of the pulsar wind nebulae, when sufficiently embedded into its dead stellar surroundings and interacting with the supernova ejecta, is asymmetric and differs greatly as a function of the past circumstellar evolution of its progenitor, which reflects into their projected radio synchrotron emission. This mechanism is particularly at work in the context of remnants involving slowly moving or very massive stars. We find that the mixing of material in plerionic core collapse supernova remnants is strongly affected by the asymmetric reverberation in their pulsar wind nebulae.