论文标题
带有磁制动的台面模型
MESA models with magnetic braking
论文作者
论文摘要
在台面中实现了两种磁制动模型，以用于薄雾恒星模型网格。通过与磁性恒星风相互作用（即磁性制动），观察到恒星小于1.3 $ m _ {\ odot} $随着时间的流逝而旋转。这是陀螺仪的基础，也是下质恒星进化的基础。磁制动背后的详细物理以及一维恒星演化模型也不确定。因此，我们校准了模型并与开放群集的数据进行比较。此处测试的每个制动模型都能重现数据，尽管具有一些重要的区别。 Matt等人。 （2015年）处方与在开放簇中观察到的缓慢旋转的恒星相匹配，但往往高估了迅速旋转的恒星的存在。 Garraffo等。 （2018）处方通常会产生太多的角动量损失，无法准确匹配下质量恒星的慢速序列，但是再现了在开放式簇中观察到的缓慢且快速旋转的恒星的双峰性质。我们发现其他证据表明，在这些制动模型中可能缺少某种水平的质量依赖性，以使在超过1 Gyr的群集中观察到的旋转周期匹配。
Two magnetic braking models are implemented in MESA for use in the MIST stellar model grids. Stars less than about 1.3 $M_{\odot}$ are observed to spin down over time through interaction with their magnetized stellar winds (i.e., magnetic braking). This is the basis for gyrochronology, and fundamental to the evolution of lower mass stars. The detailed physics behind magnetic braking are uncertain, as are 1D stellar evolution models. Thus, we calibrate our models and compare to data from open clusters. Each braking model tested here is capable of reproducing the data, albeit with some important distinctions. The Matt et al. (2015) prescription matches the slowly rotating stars observed in open clusters, but tends to overestimate the presence of rapidly rotating stars. The Garraffo et al. (2018) prescription often produces too much angular momentum loss to accurately match the observed slow sequence for lower mass stars, but reproduces the bimodal nature of slow and rapidly rotating stars observed in open clusters fairly well. We find additional evidence that some level of mass dependency may be missing in these braking models to match the rotation periods observed in clusters older than 1 Gyr better.
