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Dynamical friction on satellite galaxies

机译：卫星星系上的动摩擦

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摘要

For a rigid model satellite, Chandrasekhar's dynamical friction formula describes the orbital evolution quite accurately, when the Coulomb logarithm is chosen appropriately. However, it is not known if the orbital evolution of a real satellite with the internal degree of freedom can be described by the dynamical friction formula. We performed an N-body simulation of the orbital evolution of a self-consistent satellite galaxy within a self-consistent parent galaxy. We found that the orbital decay of the simulated satellite is significantly faster than an estimate from the dynamical friction formula. The main cause of this discrepancy is that the stars stripped out of the satellite are still close to the satellite, and increase the drag force on the satellite through two mechanisms. One is a direct drag force from particles in the trailing tidal arm, a non-axisymmetric force that slows the satellite down. The other is an indirect effect that is caused by the particles remaining close to the satellite after escaping. The force from them enhances the wake caused in the parent galaxy by dynamical friction, and this larger wake in turn slows the satellite down more than expected from the contribution of its bound mass. We found that these two have comparable effects, and that the combined effect can be as large as 20% of the total drag force on the satellite.
机译：对于刚性模型卫星，当适当选择库仑对数时，钱德拉塞卡（Chandrasekhar）的动摩擦公式可以非常准确地描述轨道演化。但是，尚不清楚是否可以通过动摩擦公式描述具有内部自由度的真实卫星的轨道演化。我们对自洽父系星系中自洽卫星星系的轨道演化进行了N体模拟。我们发现，模拟卫星的轨道衰减明显快于动摩擦公式的估计。造成这种差异的主要原因是，从卫星中剥离出来的恒星仍然靠近卫星，并通过两种机制增加了对卫星的阻力。一种是来自潮汐后臂中粒子的直接阻力，这是一种非轴对称的力，它使卫星减速。另一个是间接效应，是由逃逸后仍保留在卫星附近的粒子引起的。它们的作用力增强了由动力摩擦在母星系中引起的尾迹，而这种较大的尾迹又使卫星的减速比其结合质量的贡献所预期的要慢得多。我们发现这两者具有可比的效果，并且组合效果可能高达卫星上总阻力的20％。

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