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首页> 外文期刊>The Astrophysical journal >MAGNETOHYDRODYNAMICS OF CLOUD COLLISIONS IN A MULTIPHASE INTERSTELLAR MEDIUM
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MAGNETOHYDRODYNAMICS OF CLOUD COLLISIONS IN A MULTIPHASE INTERSTELLAR MEDIUM

机译：多相星际介质中云团碰撞的磁水动力学

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We extend previous studies of the physics of interstellar cloud collisions by beginning an investigation of the role of magnetic fields through two-dimensional magnetohydrodynamical (MHD) numerical simu- lations. In particular, we study head-on collisions between equal mass, mildly supersonic, diffuse clouds similar to those in our previous study. Here we include a moderate magnetic field, corresponding to βp_g/p_b = 4, and two limiting field geometries, with the field lines parallel (aligned)and perpendicular (transverse) to the colliding cloud motion. We explore both adiabatic and radiative cases, and we simulate collisions between clouds evolved through prior motion in the intercloud medium. In addition to the collision of evolved identical clouds (symmetric cases), wc also study colli- sions of clouds that are initially, identical but have different evolutionary ages (asymnictric cases). Depending on their geometry, magnetic fields can significantly alter the outcome of the collisions com- pared to the hydrodynamic (HD) case. (l) In the aligned case, adiabatic collisions, like their HD counter- parts, are very disruptive independently of the symmetry. However, when radiative processes arc taken into account, partial coalescence takes place even in the asymmetric case, unlike the HD calculations. (2) In the transverse case, the effects of the magnetic field are even more dramatic, with reniarkable diffr- ences between unevolved and evolved clouds, Collisions between (initially adjacent) unevolved clouds arc almost unaffected by magnetic fields. However, the interaction
机译：我们通过二维磁流体动力学（MHD）数值模拟开始对磁场作用的研究，从而扩展了星际云碰撞物理学的先前研究。特别是，我们研究了等质量，轻度超音速，弥漫性云之间的正面碰撞，类似于我们先前的研究。在这里，我们包括一个中等磁场（对应于βp_g/ p_b = 4）和两个极限场几何形状，其中场线与碰撞云的运动平行（对齐）和垂直（横向）。我们研究了绝热和辐射情况，并模拟了在云间介质中通过先验运动演化而来的云之间的碰撞。除了演化的相同云的碰撞（对称情况）之外，wc还研究了最初相同，但具有不同演化年龄的云的碰撞（非对称情况）。与流体动力学（HD）情况相比，磁场根据其几何形状可以显着改变碰撞的结果。 （l）在对齐的情况下，绝热碰撞像其HD零件一样，具有很强的破坏性，与对称性无关。但是，当考虑辐射过程时，与HD计算不同，即使在非对称情况下也会发生部分合并。 （2）在横向情况下，磁场的影响更为显着，在未发展和发展的云之间存在可分辨的差异，（最初相邻的）未发展的云之间的碰撞几乎不受磁场的影响。但是，互动

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