来自动力摩擦尾流的潮汐力：翘曲、不平衡和运动失准
Tidal forces from the wake of dynamical friction: warps, lopsidedness and kinematic misalignment
摘要：
当一个星系在暗物质粒子背景中运动时，会产生一个高密度的暗物质粒子或尾流。尾流对星系的反作用是一个力场，可以分解为一个有效的减速（称为动力学摩擦）和一个潮汐场。在本文中，我们确定的潮汐力，从而产生的星系，以及由此产生的观测，这是扭曲，lopsidedness和/或运动光度位置角失调。我们估计的潮汐效应的大小需要复制孤立星系IC 2487上观察到的翘曲和不平衡。在暗物质分布特性的实际范围内，可以再现IC 2487所观察到的扭曲和不平衡的运动学特性（暗物质粒子的背景介质具有$\lesssim 80\,{\rm km\,s^{-1}}$的速度色散和$10^4-10^5~{\rm M_\odot\,kpc^{-3}}$的密度，更可能在下端）。我们的结论是，提出的机制可以产生翘曲，偏心和失调观察孤立星系或星系松散的群体。该方法也可用于约束暗物质的空间和速度分布特性。
英文摘要：
A galaxy moving through a background of dark matter particles, induces an overdensity of these particles or a wake behind it. The back reaction of this wake on the galaxy is a force field that can be decomposed into an effective deceleration (called dynamical friction) and a tidal field. In this paper we determine the tidal forces, thus generated on the galaxy, and the resulting observables, which are shown to be warps, lopsidedness and/or kinematic-photometric position angle misalignments. We estimate the magnitude of the tidal-like effects needed to reproduce the observed warp and lopsidedness on the isolated galaxy IC 2487. Within a realistic range of dark matter distribution properties the observed warped and lopsided kinematical properties of IC 2487 is possible to reproduce (the background medium of dark matter particles has a velocity dispersion of $\lesssim 80\,{\rm km\,s^{-1}}$ and the density $10^4-10^5~{\rm M_\odot\,kpc^{-3}}$, more likely at the lower end). We conclude that the proposed mechanism can generate warps, lopsidedness and misalignments observed in isolated galaxies or galaxies in loose groups. The method can be used also to constrain dark matter spatial and velocity distribution properties.
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