The galactic dust-up: modelling dust evolution in FIRE
The galactic dust-up: modelling dust evolution in FIRE
复制标题
银河尘暴：在 FIRE 中模拟尘埃演化
DOI：
10.1093/mnras/stac1542
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发表时间：
2022
影响因子：
4.8
通讯作者：
Faucher-Giguère, Claude-André
中科院分区：
文献类型：
--
作者：
Choban, Caleb R.;Kereš, Dušan;Hopkins, Philip F.;Sandstrom, Karin M.;Hayward, Christopher C.;Faucher-Giguère, Claude-André
最近已经取得了长足的进步，发展尘埃演化模型的星系形成模拟，但这些方法在他们的假设和复杂程度不同。在这里，我们介绍和比较两个独立的尘埃演化模型（标记为“元素”和“物种”），最近的方法的基础上，纳入thegizmocode，再加上火-2恒星反馈和星际介质物理。这两种模型都解释了湍流尘埃扩散、恒星产生的尘埃、通过气尘吸积产生的尘埃、时间分辨的超新星造成的尘埃破坏、热气中的热溅射和星暴。“元素”模型跟踪广义尘埃物种的演变，并利用一个简单的，“可调”的尘埃生长例程，而“物种”模型跟踪特定的尘埃物种与设置的化学成分的演变，并结合了物理动机，两个阶段的尘埃生长例程。我们测试和比较这些模型在一个理想化的银河系质量的星系，发现，虽然都产生合理的星系集成的尘埃金属（D/Z）的比率和预测气体尘埃吸积作为主要的尘埃生长机制，需要一个化学激发的模型来重现所观察到的比例关系之间的个别元素耗尽和D/Z与柱密度和局部气体密度。我们还发现，包括理论上的金属铁和含O的尘埃物种的情况下，需要特定的尘埃物种，以配合观察O和Fe的耗尽，和一个亚分辨率致密分子气体/CO计划的整合是必要的，以配合观察到的C耗尽，并确保碳质尘埃不会在密集的环境中过度生产。
Recent strides have been made developing dust evolution models for galaxy formation simulations but these approaches vary in their assumptions and degree of complexity. Here, we introduce and compare two separate dust evolution models (labelled ‘Elemental’ and ‘Species’), based on recent approaches, incorporated into thegizmocode and coupled withfire-2 stellar feedback and interstellar medium physics. Both models account for turbulent dust diffusion, stellar production of dust, dust growth via gas-dust accretion, and dust destruction from time-resolved supernovae, thermal sputtering in hot gas, and astration. The ‘Elemental’ model tracks the evolution of generalized dust species and utilizes a simple, ‘tunable’ dust growth routine, while the ‘Species’ model tracks the evolution of specific dust species with set chemical compositions and incorporates a physically motivated, two-phase dust growth routine. We test and compare these models in an idealized Milky Way-mass galaxy and find that while both produce reasonable galaxy-integrated dust-to-metals (D/Z) ratios and predict gas-dust accretion as the main dust growth mechanism, a chemically motivated model is needed to reproduce the observed scaling relation between individual element depletions and D/Z with column density and local gas density. We also find the inclusion of theoretical metallic iron and O-bearing dust species are needed in the case of specific dust species in order to match observations of O and Fe depletions, and the integration of a sub-resolution dense molecular gas/CO scheme is needed to both match observed C depletions and ensure carbonaceous dust is not overproduced in dense environments.