New evolutionary models for pre-main sequence and main sequence low-mass stars down to the hydrogen-burning limit
New evolutionary models for pre-main sequence and main sequence low-mass stars down to the hydrogen-burning limit
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DOI：
10.1051/0004-6361/201425481
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发表时间：
2015-05-01
影响因子：
6.5
通讯作者：
Chabrier, Gilles
中科院分区：
文献类型：
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作者：
Baraffe, Isabelle;Homeier, Derek;Chabrier, Gilles
我们提出了低质量恒星低至氢燃烧极限的新模型，该模型始终耦合大气层和内部结构，从而取代了广泛使用的 BCAH98 模型。新模型包括更新的分子线表和太阳丰度，以及在 2D/3D 辐射流体动力学模拟上校准的大气对流参数。将这些模型与不同年龄的各种颜色幅度图中的观察结果进行比较，表明比前几代模型有显着改进。新模型可以解决以前模型中存在的缺陷，例如与 M 矮星观测结果相比，预测的光学颜色太蓝。与任何现有模型相比，他们还可以在具有单一等时线的颜色幅度图中重现年轻四重系统 LkCa 3 的四个组成部分。在本文中，我们还强调了比较模型和观测结果时保持一致性的必要性，以及使用基于相同大气结构的进化模型和颜色的必要性。
We present new models for low-mass stars down to the hydrogen-burning limit that consistently couple atmosphere and interior structures, thereby superseding the widely used BCAH98 models. The new models include updated molecular linelists and solar abundances, as well as atmospheric convection parameters calibrated on 2D/3D radiative hydrodynamics simulations. Comparison of these models with observations in various colour-magnitude diagrams for various ages shows significant improvement over previous generations of models. The new models can solve flaws that are present in the previous ones, such as the prediction of optical colours that are too blue compared to M dwarf observations. They can also reproduce the four components of the young quadruple system LkCa 3 in a colour-magnitude diagram with one single isochrone, in contrast to any presently existing model. In this paper we also highlight the need for consistency when comparing models and observations, with the necessity of using evolutionary models and colours based on the same atmospheric structures.