恒星基本参数的概率推断：对闪烁星的应用
Probabilistic inference of basic stellar parameters: application to flickering stars
摘要：
可观测的恒星参数之间的关系通常被假定为确定性的。也就是说，给定自变量“$x$”的无限精确测量值和某种模型，因变量“$y$”的值可以被精确地知道。在实践中，这种假设很少是有效的，内在的随机性意味着具有完全相同的“$x$”的两颗星，将具有略微不同的“$y$”。恒星的短时间尺度亮度波动（闪烁）与表面重力和恒星密度之间的关系是两个这样的随机关系，到目前为止，一直被视为确定性的。我们重新校准这些关系的概率框架中，使用层次贝叶斯建模（HBM）约束内在的分散的关系。我们发现的证据，额外的分散的关系，不能单独占观测的不确定性。表面重力和恒星密度的分散并不依赖于闪烁，这表明使用闪烁作为$\log g$和$ρ_\star$的替代物对矮星和巨星同样有效，尽管事实上矮星的观测不确定性往往更大。
英文摘要：
The relations between observable stellar parameters are usually assumed to be deterministic. That is, given an infinitely precise measurement of independent variable, `$x$', and some model, the value of dependent variable, `$y$' can be known exactly. In practise this assumption is rarely valid and intrinsic stochasticity means that two stars with exactly the same `$x$', will have slightly different `$y$'s. The relation between short-timescale brightness fluctuations (flicker) of stars and both surface gravity and stellar density are two such stochastic relations that have, until now, been treated as deterministic ones. We recalibrate these relations in a probabilistic framework, using Hierarchical Bayesian Modelling (HBM) to constrain the intrinsic scatter in the relations. We find evidence for additional scatter in the relationships, that cannot be accounted for by the observational uncertainties alone. The scatter in surface gravity and stellar density does not depend on flicker, suggesting that using flicker as a proxy for $\log g$ and $ρ_\star$ is equally valid for dwarf and giant stars, despite the fact that the observational uncertainties tend to be larger for dwarfs.
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