Ram pressure stripping of disc galaxies orbiting in clusters – I. Mass and radius of the remaining gas disc
Ram pressure stripping of disc galaxies orbiting in clusters – I. Mass and radius of the remaining gas disc
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DOI：
10.1111/j.1365-2966.2007.12241.x
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发表时间：
2007-07
影响因子：
4.8
通讯作者：
Elke Roediger;M. Brüggen
中科院分区：
文献类型：
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作者：
Elke Roediger;M. Brüggen
我们提出了第一个三维流体动力学模拟冲压压力剥离的盘星系在星系团轨道。沿着轨道，这个星系经历的冲压压力随时间而变化。本文重点研究了剩余气盘半径和质量的演化，并与古恩& Gott提出的经典解析估计进行了比较。我们发现，这个简单的估计工程以及在预测剩余的气体盘的半径的演变。只有当冲压压力的增加快于汽提时间尺度时，盘半径才保持大于预测值。然而，具有如此短的冲压压力峰值的轨道不太可能发生在紧凑的星团之外的其他地方。与半径演化不同的是，星系的质量损失历史并不能通过分析估计准确描述。一般来说，在模拟中，星系失去气体的速度比预测的要慢。
We present the first 3D hydrodynamical simulations of ram pressure stripping of a disc galaxy orbiting in a galaxy cluster. Along the orbit, the ram pressure that this galaxy experiences varies with time. In this paper, we focus on the evolution of the radius and mass of the remaining gas disc, and compare it with the classical analytical estimate proposed by Gunn & Gott. We find that this simple estimate works well in predicting the evolution of the radius of the remaining gas disc. Only if the ram pressure increases faster than the stripping time-scale, the disc radius remains larger than predicted. However, orbits with such short ram pressure peaks are unlikely to occur in other than compact clusters. Unlike the radius evolution, the mass-loss history for the galaxy is not accurately described by the analytical estimate. Generally, in the simulations the galaxy loses its gas more slowly than predicted.