Asymmetric supernova remnants generated by Galactic, massive runaway stars
Asymmetric supernova remnants generated by Galactic, massive runaway stars
复制标题
DOI：
10.1093/mnras/stv898
复制
发表时间：
2015-07
影响因子：
4.8
通讯作者：
D. Meyer;N. Langer;J. Mackey;P. Velázquez;A. Gusdorf
中科院分区：
文献类型：
--
作者：
D. Meyer;N. Langer;J. Mackey;P. Velázquez;A. Gusdorf
在一颗失控的大质量恒星死亡后，它的超新星激波与它死去的祖先产生的弓形激波相互作用，在膨胀到本地星际介质（ISM）之前可能会失去能量、动量和它的球形对称性。我们研究这些祖星的初始质量和空间速度是否与不对称超新星残余物有关。我们运行的流体动力学模型的超新星爆炸在移动的星系核坍缩祖的预成形介质。我们发现累积超过1.5 m⊙的弓形激波会产生不对称残余物。在超新星形成160 - 750年之后，冲击波首先与这些弓形激波发生碰撞，碰撞持续到830 - 4900年。激波位于距离爆炸中心1.35 - 5%的地方，它自由地扩展到ISM，而在相反的方向上，它被引导到未受干扰的风物质区域。这适用于最初以20km - 1速度运动的20M⊙祖星和我们最初以40M⊙祖星。这些残留物混合了ISM气体、恒星风和超新星喷出物，这在爆炸中心的上游尤为重要。它们的光曲线主要由光学薄冷却的发射和受冲击的ISM气体的x射线发射决定。我们发现这些残余物很可能在[OIII] - 5007光谱线发射或x射线的软能带中被观测到。最后，我们在观测到的银河系超新星遗迹（如3C391和天鹅座环）的背景下讨论了我们的结果。
After the death of a runaway massive star, its supernova shock wave interacts with the bow shocks produced by its defunct progenitor, and may lose energy, momentum, and its spherical symmetry before expanding into the local interstellar medium (ISM). We investigate whether the initial mass and space velocity of these progenitors can be associated with asymmetric supernova remnants. We run hydrodynamical models of supernovae exploding in the pre-shaped medium of moving Galactic core-collapse progenitors. We find that bow shocks that accumulate more than about1.5M⊙ generate asymmetric remnants. The shock wave first collides with these bow shocks 160 − 750yr after the supernova, and the collision lasts until 830 − 4900yr. The shock wave is then located 1.35 − 5pc from the center of the explosion, and it expands freely into the ISM, whereas in the opposite direction it is channelled into the region of undisturbed wind material. This applies to an initially 20M⊙ progenitor moving with velocity 20kms −1 and to our initially 40M⊙ progenitor. These remnants generate mixing of ISM gas, stellar wind and supernova ejecta that is particularly important upstream from the center of the explosion. Their lightcurves are dominated by emission from optically-thin cooling and by X-ray emission of the shocked ISM gas. We find th at these remnants are likely to be observed in the [OIII] �5007 spectral line emission or in the soft energy-band of X-rays. Finally, we discuss our results in the context of observed Galactic supernova remnants such as 3C391 and the Cygnus Loop.