面对恒星物理学中的不确定性II。探索主序星恒星演化轨迹的差异
Confronting uncertainties in stellar physics II. exploring differences in main-sequence stellar evolution tracks
摘要：
我们评估恒星演化计算的系统不确定性低到中等质量，主序星。我们比较公布的恒星轨道从几个不同的演化代码与我们自己的轨道计算使用恒星代码星和MESA。特别是，我们专注于轨道1和3太阳质量在太阳金属丰度。我们发现，在现有的1太阳质量轨道（计算前，最近的太阳组成修订的Asplund等人）的传播。可以被使用STARS代码计算的0.97-1.01太阳质量之间的轨迹覆盖。我们评估了这种不确定性的起源的一些可能的原因，包括如何选择的输入物理和用于执行太阳能校准的太阳能约束影响的轨道。我们发现，对于一个1太阳质量的轨道，在初始氢丰度和初始金属丰度约10%的不确定性产生约2%的质量误差。对于3个太阳质量轨道，不同恒星代码的轨道之间几乎没有差异。主要的区别在于主序列的范围，我们认为这是由于对流超冲在核中的实施的不同选择的结果。初始丰度的不确定性导致质量测定的1-2%误差。这些不确定性仅涵盖总误差预算的一部分，其还应包括输入物理中的不确定性（例如，反应速率、不透明度、对流模型）和任何缺失的物理特性（例如，辐射悬浮、旋转、磁场）。恒星表面性质如光度和有效温度的不确定性将进一步降低任何潜在质量测定的准确性。
英文摘要：
We assess the systematic uncertainties in stellar evolutionary calculations for low- to intermediate-mass, main-sequence stars. We compare published stellar tracks from several different evolution codes with our own tracks computed using the stellar codes STARS and MESA. In particular, we focus on tracks of 1 and 3 solar masses at solar metallicity. We find that the spread in the available 1 solar mass tracks (computed before the recent solar composition revision by Asplund et al.) can be covered by tracks between 0.97-1.01 solar masses computed with the STARS code. We assess some possible causes of the origin of this uncertainty, including how the choice of input physics and the solar constraints used to perform the solar calibration affect the tracks. We find that for a 1 solar mass track, uncertainties of around 10% in the initial hydrogen abundance and initial metallicity produce around a 2% error in mass. For the 3 solar mass tracks, there is very little difference between the tracks from the various different stellar codes. The main difference comes in the extent of the main sequence, which we believe results from the different choices of the implementation of convective overshooting in the core. Uncertainties in the initial abundances lead to a 1-2% error in the mass determination. These uncertainties cover only part of the total error budget, which should also include uncertainties in the input physics (e.g., reaction rates, opacities, convective models) and any missing physics (e.g., radiative levitation, rotation, magnetic fields). Uncertainties in stellar surface properties such as luminosity and effective temperature will further reduce the accuracy of any potential mass determinations.
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