GAS LOSS BY RAM PRESSURE STRIPPING AND INTERNAL FEEDBACK FROM LOW-MASS MILKY WAY SATELLITES
GAS LOSS BY RAM PRESSURE STRIPPING AND INTERNAL FEEDBACK FROM LOW-MASS MILKY WAY SATELLITES
复制标题
冲压压力剥离造成的气体损失和来自低质量银河系卫星的内部反馈
DOI：
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发表时间：
2016
期刊：
影响因子：
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通讯作者：
A. Gatto
中科院分区：
文献类型：
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作者：
A. Emerick;M. M. Low;J. Grcevich;A. Gatto
银河系中矮卫星的演化受到冲压剥离（RPS）、潮汐剥离和大质量恒星内部反馈的共同影响。我们调查气体损失过程中最小的卫星MW使用三维，高分辨率，理想化的风洞模拟，占气体损失通过冲压压力剥离和驱逐超新星反馈。使用适合于像狮子座T矮星系的初始条件，我们调查是否环境气体剥离和内部反馈可以淬火这些低质量星系的预期时间尺度，短于2 Gyr。我们发现超新星反馈对这些低星星形成率星系的剥离率的贡献可以忽略不计。然而，我们也发现，RPS是低于预期的剥离方案，我们考虑的效率。我们的工作表明，尽管RPS最终可以完全剥离这些星系，但其他物理学可能会发挥作用，使我们计算的剥离时间与从低质量MW矮星系观测中推导出的快速淬火时间尺度相一致。我们讨论的角色，额外的物理可能在这种情况下，包括主机卫星潮汐相互作用，核心与尖状暗物质配置文件，再电离，卫星预处理。我们的结论是，这些物理一起适当的会计是必要的，以了解淬火的低质量MW卫星。
The evolution of dwarf satellites in the Milky Way (MW) is affected by a combination of ram pressure stripping (RPS), tidal stripping, and internal feedback from massive stars. We investigate gas loss processes in the smallest satellites of the MW using three-dimensional, high-resolution, idealized wind tunnel simulations, accounting for gas loss through both ram pressure stripping and expulsion by supernova feedback. Using initial conditions appropriate for a dwarf galaxy like Leo T, we investigate whether or not environmental gas stripping and internal feedback can quench these low-mass galaxies on the expected timescales, shorter than 2 Gyr. We find that supernova feedback contributes negligibly to the stripping rate for these low star formation rate galaxies. However, we also find that RPS is less efficient than expected in the stripping scenarios we consider. Our work suggests that although RPS can eventually completely strip these galaxies, other physics is likely at play to reconcile our computed stripping times with the rapid quenching timescales deduced from observations of low-mass MW dwarf galaxies. We discuss the roles additional physics may play in this scenario, including host-satellite tidal interactions, cored versus cuspy dark matter profiles, reionization, and satellite preprocessing. We conclude that a proper accounting of these physics together is necessary to understand the quenching of low-mass MW satellites.