Star formation and clumps in cosmological galaxy simulations with radiation pressure feedback
Star formation and clumps in cosmological galaxy simulations with radiation pressure feedback
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具有辐射压力反馈的宇宙星系模拟中的恒星形成和团块
DOI：
10.1093/mnras/stu1534
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发表时间：
2014
影响因子：
4.8
通讯作者：
J. Primack
中科院分区：
文献类型：
--
作者：
Christopher E. Moody;Yicheng Guo;Nir Mandelker;D. Ceverino;M. Mozena;D. Koo;A. Dekel;J. Primack
星系的宇宙学模拟通常在早期产生了太多的恒星。我们在八对高分辨率宇宙学星系形成模拟中研究了辐射压（RP）的整体和形态影响。我们发现额外的反馈将全球恒星的形成抑制了 2 倍。尽管如此，相对于丰度匹配方法对质量大于 5 10 11 M h 1 的光环所提供的预测，模拟仍然过度产生了 2 倍的恒星（Behroozi、Wechsler & Conroy 2013）。我们还研究了辐射压力对我们的模拟的形态影响。在 RP 模拟中，低质量团块的平均数量急剧下降。只有具有恒星质量 Mclump=Mdisk 6 5% 的团块才会受到 RP 包含的影响，并且高于此范围的 RP 和无 RP 团块数量具有可比性。对于小于盘质量 5% 的团块质量，包含 RP 会使团块对比度降低几倍。对于更大的团块，RP 和无 RP 模拟之间的差异会缩小。然而我们注意到，分析的模拟中盘状恒星质量低于约 2 10 10 M h 1 。通过创建模拟哈勃太空望远镜观测结果，我们
Cosmological simulations of galaxies have typically produced too many stars at early times. We study the global and morphological eects of radiation pressure (RP) in eight pairs of high-resolution cosmological galaxy formation simulations. We nd that the additional feedback suppresses star formation globally by a factor of 2. Despite this reduction, the simulations still overproduce stars by a factor of 2 with respect to the predictions provided by abundance matching methods for halos more massive than 5 10 11 M h 1 (Behroozi, Wechsler & Conroy 2013). We also study the morphological impact of radiation pressure on our simulations. In simulations with RP the average number of low mass clumps falls dramatically. Only clumps with stellar masses Mclump=Mdisk 6 5% are impacted by the inclusion of RP, and RP and no-RP clump counts above this range are comparable. The inclusion of RP depresses the contrast ratios of clumps by factors of a few for clump masses less than 5% of the disk masses. For more massive clumps, the dierences between and RP and no-RP simulations diminish. We note however, that the simulations analysed have disk stellar masses below about 2 10 10 M h 1 . By creating mock Hubble Space Telescope observations we