吸积星系际流的外星系盘中密度分布的方位角依赖性
Azimuthal dependence of the density distribution in outer galactic discs accreting intergalactic flows
摘要：
目标。银河系气体盘密度的振幅和尺度高度与自重力轴对称盘中的预期不同。然而，这种不平衡可以用星系间吸积流来解释，它在圆盘上产生非轴对称的压力。这种机制也可能导致翘曲的形成。方法.我们解析地导出了圆盘密度与自重和外压之间的关系。结果与我们多年前提出的解释翘曲形成的吸积相同的场景解释了密度及其尺度高度的方位角依赖性，最小/最大值位于翘曲最大振幅的位置（φ =95度）。和275 °），正如其压力分布所预期的那样。
英文摘要：
AIMS. The amplitude and scaleheight of the Galactic gas disc density are not axisymmetric against expectations in a self-gravity axisymmetric disc. However, this lopsidedness can be explained in terms of intergalactic accretion flows, which produce non-axisymmetric pressure on the disc. This mechanism could be also responsible for the formation of a warp. METHODS. We analytically derive the relationship between the disc density and the self-gravity and external pressure. RESULTS. The same scenario of accretion as we proposed years ago to explain the formation of the warp explains the azimuthal dependence of the density and its scaleheight, with minimum/maximum in the positions of maximum amplitude of the warp (phi=95 deg. and 275 deg.), as expected from its pressure distribution.
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