{ "id": "2408.12940", "version": "v1", "published": "2024-08-23T09:44:46.000Z", "updated": "2024-08-23T09:44:46.000Z", "title": "An Analytic Model of Gravitational Collapse Induced by Radiative Cooling: Instability Scale, Infall Velocity, and Accretion Rate", "authors": [ "James Gurian", "Boyuan Liu", "Donghui Jeong", "Takashi Hosokawa", "Shingo Hirano", "Naoki Yoshida" ], "comment": "11+3 pages, 14+3 figures", "categories": [ "astro-ph.GA" ], "abstract": "We present an analytic description of the spherically symmetric gravitational collapse of radiatively cooling gas clouds. The approach is based on developing the \"one-zone\" density-temperature relationship of the gas into a full dynamical model. We convert this density-temperature relationship into a barotropic equation of state, which we use to calculate the density and velocity profiles of the gas. From these quantities we calculate the time-dependent mass accretion rate onto the center of the cloud. The approach clarifies the mechanism by which radiative cooling induces gravitational instability. In particular, we distinguish the rapid, quasi-equilibrium contraction of a cooling gas core to high central densities from the legitimate instability this contraction establishes in the envelope. We develop a refined criterion for the mass scale of this instability, based only on the chemical-thermal evolution in the core. We explicate our model in the context of a primordial mini-halo cooled by molecular hydrogen, and then provide two further examples, a delayed collapse with hydrogen deuteride cooling and the collapse of an atomic cooling halo. In all three cases, our results agree well with full hydrodynamical treatments.", "revisions": [ { "version": "v1", "updated": "2024-08-23T09:44:46.000Z" } ], "analyses": { "keywords": [ "gravitational collapse", "instability scale", "analytic model", "infall velocity", "radiative cooling" ], "note": { "typesetting": "TeX", "pages": 3, "language": "en", "license": "arXiv", "status": "editable" } } }