3D hydrodynamics simulations of core convection in supermassive main-sequence stars
3D hydrodynamics simulations of core convection in supermassive main-sequence stars
复制标题
超大质量主序星核心对流的 3D 流体动力学模拟
DOI：
10.1093/mnras/stad846
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发表时间：
2023
影响因子：
4.8
通讯作者：
Herwig, Falk
中科院分区：
文献类型：
--
作者：
Blouin, Simon;Mao, Huaqing;Woods, Tyrone E.;Denissenkov, Pavel;Woodward, Paul R.;Herwig, Falk
超大质量恒星是第三星族恒星，质量超过500万，可能是第一个超大质量黑洞的祖先。它们的内部处于辐射压主导状态方程的状态。在本工作中，我们使用显式气体动力学程序codeppmstar来模拟大质量主序星星星的氢燃烧核心。这是超大质量恒星核心对流的第一个三维流体动力学模拟。我们进行了一系列的10个模拟在不同的加热速率和笛卡尔网格分辨率为7683，11523，和17283。我们研究对流的不同性质，包括它的大尺度形态，它的速度谱，和它的混合特性。我们的结论是，辐射压力占主导地位的性质的内部不显着影响对流的行为相比，在一个大规模的主序星星的气体压力占主导地位的核心对流的情况下。我们的模拟也提供了支持使用混合长度理论的超大质量恒星的一维模型。
Supermassive stars are Population III stars with masses exceedingthat could be the progenitors of the first supermassive black holes. Their interiors are in a regime where radiation pressure dominates the equation of state. In this work, we use the explicit gas dynamics codeppmstarto simulate the hydrogen-burning core of asupermassive main-sequence star. These are the first three-dimensional hydrodynamics simulations of core convection in supermassive stars. We perform a series of 10 simulations at different heating rates and on Cartesian grids with resolutions of 7683, 11523, and 17283. We examine different properties of the convective flow, including its large-scale morphology, its velocity spectrum, and its mixing properties. We conclude that the radiation pressure-dominated nature of the interior does not noticeably affect the behaviour of convection compared to the case of core convection in a massive main-sequence star where gas pressure dominates. Our simulations also offer support for the use of mixing-length theory in one-dimensional models of supermassive stars.