论文标题
太阳能邻居XLVII：将M DWARF模型与哈勃空间望远镜动力学和光谱法进行比较
The Solar Neighborhood XLVII: Comparing M Dwarf Models with Hubble Space Telescope Dynamical Masses and Spectroscopy
论文作者
论文摘要
我们在五个紧密分离的二进制系统中使用十个M矮人的HST/STIS光谱来测试M矮结构和进化的模型。从先前的工作中知道，全明星的个体动力质量范围为0.083至0.405 mo。我们首先通过拟合BT-SETTL大气模型来得出温度，半径，光度，表面重力和金属性。我们验证我们的方法论与类似光谱类型的恒星长基线光学干涉法的经验结果一致。然后，我们测试进化模型是否可以预测这些数量，因为恒星的已知动力学质量以及每个二元系统内的同时性和相等金属性的条件。我们将此测试应用于五个不同的进化模型集：达特茅斯模型，台面/雾模型，Baraffe等人的模型。 2015年，PARSEC模型和YAPSI模型。我们发现进化模型预测和观察结果之间的边际一致，很少有模型以自洽的方式尊重同时性的条件。我们讨论了每个模型家族的利弊，并比较其预测能力。
We use HST/STIS optical spectroscopy of ten M dwarfs in five closely separated binary systems to test models of M dwarf structure and evolution. Individual dynamical masses ranging from 0.083 to 0.405 Mo for all stars are known from previous work. We first derive temperature, radius, luminosity, surface gravity, and metallicity by fitting the BT-Settl atmospheric models. We verify that our methodology agrees with empirical results from long baseline optical interferometry for stars of similar spectral types. We then test whether or not evolutionary models can predict those quantities given the stars' known dynamical masses and the conditions of coevality and equal metallicity within each binary system. We apply this test to five different evolutionary model sets: the Dartmouth models, the MESA/MIST models, the models of Baraffe et al. 2015, the PARSEC models, and the YaPSI models. We find marginal agreement between evolutionary model predictions and observations, with few cases where the models respect the condition of coevality in a self-consistent manner. We discuss the pros and cons of each family of models and compare their predictive power.
