SNAPSHOT：大质量恒星内部和表面性质之间的联系
SNAPSHOT: Connections between Internal and Surface Properties of Massive Stars
摘要：
我们介绍了SNAPSHOT，一种系统地计算恒星结构模型在流体静力学和热平衡的基础上的3个结构属性-核心质量$M_{\rm core}$，信封质量$M_{\rm env}$和核心组成的技术。这种方法使我们能够将恒星内部的这些性质与光度和有效温度$T_{\rm eff}$以比恒星演化模型更系统的方式联系起来。对于MS模型，我们推导出$M_{\rm core}$，$M_{\rm total}$和中心H丰度之间的解析关系，可用于快速恒星演化算法。核心氦燃烧模型的$M_{\rm core}/M_{\rm total}$从0.2到0.8有对流包层，低$T_{\rm eff}$，将出现红超巨星。对于给定的$M_{\rm core}$，它们在$M_{\rm env}$（$\sim 2 - 20\,\mathrm{M}_{\odot}$）的宽范围内表现出光度（0.02 dex）和$T_{\rm eff}$（$\sim 400\,\mathrm{K}$）的小变化。这意味着不可能仅从光度和$T_{\rm eff}$推导出红超巨星的质量。本文导出了红超巨星在核He燃烧时$M_{\rm core}$与总光度之间的关系式：$\log M_{\rm core} \simeq 0.44 \log L/L_{\odot} - 1.38$。在$M_{\rm core}$ / $M_{\rm total} \approx 0.2$中，我们的模型表现出双稳定性，并从RSG跳到BSG结构。我们的模型与$M_{\rm core}/M_{\rm total} > 0.8$，这对应于剥离的恒星产生的质量损失或二元相互作用，表明$T_{\rm eff}$有很强的依赖于$M_{\rm env}$，$M_{\rm core}$和核心组成。我们发现在一个双星系统中，HD 45166的质量小于它的动力学质量。当一个大的观测样本的剥离恒星变得可用，我们的结果可以用来限制他们的质量和物理的二元相互作用。
英文摘要：
We introduce SNAPSHOT, a technique to systematically compute stellar structure models in hydrostatic and thermal equilibrium based on 3 structural properties - core mass $M_{\rm core}$, envelope mass $M_{\rm env}$ and core composition. This approach allows us to connect these properties of stellar interiors to the luminosity and effective temperature $T_{\rm eff}$ in a more systematic way than with stellar evolution models. For MS models, we derive an analytical relationship between $M_{\rm core}$, $M_{\rm total}$ and central H abundance that can be used in rapid stellar evolution algorithms. Core-He burning models with $M_{\rm core}/M_{\rm total}$ from 0.2 to 0.8 have convective envelopes, low $T_{\rm eff}$ and will appear as red supergiants. For a given $M_{\rm core}$, they exhibit a small variation in luminosity (0.02 dex) and $T_{\rm eff}$ ($\sim 400\,\mathrm{K}$) over a wide range of $M_{\rm env}$ ($\sim 2 - 20\,\mathrm{M}_{\odot}$). This means that it is not possible to derive red supergiant masses from luminosities and $T_{\rm eff}$ alone. We derive the following relationship between $M_{\rm core}$ and the total luminosity of a red supergiant during core He burning: $\log M_{\rm core} \simeq 0.44 \log L/L_{\odot} - 1.38$. At $M_{\rm core}$/$M_{\rm total} \approx 0.2$, our models exhibit a bi-stability and jump from a RSG to a BSG structure. Our models with $M_{\rm core}/M_{\rm total} > 0.8$, which correspond to stripped stars produced by mass loss or binary interaction, show that $T_{\rm eff}$ has a strong dependence on $M_{\rm env}$, $M_{\rm core}$ and the core composition. We find the mass of one of these stripped stars in a binary system, HD 45166, to be less than its dynamical mass. When a large observational sample of stripped stars becomes available, our results can be used to constrain their masses and the physics of binary interaction.
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