Thin shell morphology in the circumstellar medium of massive binaries
Thin shell morphology in the circumstellar medium of massive binaries
复制标题
大质量双星星周介质中的薄壳形态
DOI：
10.1051/0004-6361/201015517
复制
发表时间：
2010
影响因子：
6.5
通讯作者：
Z. Meliani
中科院分区：
文献类型：
--
作者：
A. J. Marle;R. Keppens;Z. Meliani
上下文在大质量双星中，两颗恒星的强大恒星风碰撞，导致形成只能在3D中建模的激波主导环境。目标。本文研究了两个长周期双星系统中双星星风之间的碰撞前沿壳层的形态，一个是富氢沃尔夫-拉叶星星（WNL）和O-星星，另一个是亮蓝变星（LBV）和O-星星。我们遵循的发展和演变的不稳定性，由于风的相互作用和轨道运动，形成在这个壳，如果它是足够的压缩。方法.我们使用MPI-AMRVAC的流体动力学方程，结合光学薄辐射冷却，在一个自适应网格三维网格的时间积分。使用参数的通用的二进制系统，我们模拟的风的两颗恒星之间的相互作用。结果WNL + O星星双星是绝热风碰撞的典型例子。生成的壳厚而光滑，没有不稳定性。另一方面，O型星星风与LBV风碰撞产生的壳层，以及双星的轨道运动，容易受到薄壳层不稳定性的影响，从而形成高度结构化的形态。我们确定为线性和非线性薄壳不稳定性的不稳定性，有明显的差异之间的领先和落后的部分碰撞前。我们还发现，包含一个星星与（相对）慢风的双星，壳的全球形状是由慢风速和轨道运动的二进制，比冲压压力之间的平衡风。结论.需要对大质量双星风之间的相互作用进行额外的参数研究，以确定碰撞前沿多重不稳定性的作用和动力学重要性，如图所示，LBV + O星星系统。
Context. In massive binaries, the powerful stellar winds of the two stars collide, leading to the formation of shock-dominated environments that can be modeled only in 3D. Aims. We investigate the morphology of the collision-front shell between the stellar winds of binary components in two long-period binary systems, one consisting of a hydrogen-rich Wolf-Rayet star (WNL) and an O-star and the other of a luminous blue variable (LBV) and an O-star. We follow the development and evolution of instabilities due to both the wind interaction and the orbital motion, that form in this shell if it is sufficiently compressed. Methods. We use MPI-AMRVAC to time-integrate the equations of hydrodynamics, combined with optically thin radiative cooling, on an adaptive mesh 3D grid. Using parameters for generic binary systems, we simulate the interaction between the winds of the two stars. Results. The WNL + O star binary represent a typical example of an adiabatic wind collision. The resulting shell is thick and smooth, showing no instabilities. On the other hand, the shell created by the collision of the O star wind with the LBV wind, as well as the orbital motion of the binary components, is susceptible to thin shell instabilities, which create a highly structured morphology. We identify the instabilities as both linear and non-linear thin-shell instabilities, there being distinct differences between the leading and the trailing parts of the collision front. We also find that for binaries containing a star with a (relatively) slow wind, the global shape of the shell is determined more by the slow wind velocity and the orbital motion of the binary, than the ram pressure balance between the two winds. Conclusions. Additional parametric studies of the interaction between the massive binary winds are needed to identify the role and dynamical importance of multiple instabilities at the collision front, as shown here for an LBV + O star system.