Unravelling the interplay between SIDM and baryons in MW haloes: defining where baryons dictate heat transfer
Unravelling the interplay between SIDM and baryons in MW haloes: defining where baryons dictate heat transfer
复制标题
揭示 SIDM 和 MW 晕中重子之间的相互作用：定义重子决定传热的位置
DOI：
10.1093/mnras/stac3634
复制
发表时间：
2022
影响因子：
4.8
通讯作者：
O’Neil, Stephanie
中科院分区：
文献类型：
--
作者：
Rose, Jonah C.;Torrey, Paul;Vogelsberger, Mark;O’Neil, Stephanie
我们提出了一组新的类银河系 (MW) 宇宙学放大模拟，其中首次包括弹性速度相关自相互作用暗物质 (SIDM) 和 IllustrisTNG 物理。通过这些模拟，我们研究了 SIDM 和重子之间的相互作用及其对星系演化过程的影响。我们还引入了一套新颖的修改后的纯暗物质模拟，可以合理地复制完全实现的流体动力学对 DM 晕的影响，同时简化分析并降低计算成本。我们发现重子对晕中心区域热结构的改变程度比类MW星系的SIDM散射更大。此外，我们发现类MW晕的新热结构导致SIDM产生尖峰中心密度而不是核心，因为SIDM散射通过将热量从星系中心转移而消除了热支撑。我们发现，这种由重子收缩引起的效应开始影响恒星质量为108M⊙的星系，并且强度增加到MW质量规模。
We present a new set of cosmological zoom-in simulations of a Milky Way (MW)-like galaxy that for the first time include elastic velocity-dependent self-interacting dark matter (SIDM) and IllustrisTNG physics. With these simulations, we investigate the interaction between SIDM and baryons and its effects on the galaxy evolution process. We also introduce a novel set of modified dark matter-only simulations that can reasonably replicate the effects of fully realized hydrodynamics on the DM halo while simplifying the analysis and lowering the computational cost. We find that baryons change the thermal structure of the central region of the halo to a greater extent than the SIDM scatterings for MW-like galaxies. Additionally, we find that the new thermal structure of the MW-like halo causes SIDM to create cuspier central densities rather than cores because the SIDM scatterings remove the thermal support by transferring heat away from the centre of the galaxy. We find that this effect, caused by baryon contraction, begins to affect galaxies with a stellar mass of 108M⊙and increases in strength to the MW-mass scale.