Learning Physics from the Stars: Its All in the Coefficients
Steven D. Kawaler
备注：
This will appear as a chapter in "Asteroseismology", Canary Islands Winter School of Astrophysics, Volume XXII, edited by Pere L. Pallé, published by Cambridge University Press
In this chapter, I present an overview and discussion of the basic equations of stellar structure, and show where the physics of stellar interiors appears within the coefficients of these famous equations. I discuss the basic input physics and weaknesses that we need to fix. Asteroseismology shows significant promise in helping us reduce those uncertainties and, in the process, improve our understanding of a variety of nasty physics problems. This chapter summarizes a series of lectures that were a part of the 22nd Canary Islands Winter School of Astrophysics, presented in November 2010.
Modeling Multi-Wavelength Stellar Astrometry. II. Determining Absolute Inclinations, Gravity Darkening Coefficients, and Spot Parameters of Single Stars with SIM Lite
Spherically-symmetric model stellar atmospheres and limb darkening I: limb-darkening laws, gravity-darkening coefficients and angular diameter corrections for red giant stars
模型恒星大气是理解恒星干涉测量、微透镜、食双星和行星凌日观测的基本工具。然而，计算还包括假设，例如模型的几何形状。我们使用的强度分布计算的平面平行和球对称模型的大气，以确定拟合系数在BVRIHK，CoRot和开普勒波段的临边昏暗使用几种不同的拟合法律，重力暗化和干涉角直径校正。比较每种几何结构的预测变量，我们发现球对称模型几何结构导致对表面重力log g < 3的不同预测。特别是，最常用的临边暗化法律产生的球对称模型大气，这表明需要更复杂的法律的强度分布拟合差。球对称模型的角直径校正范围为0.67至1，而平面平行模型的范围为0.95至1。
Influence of Collisions with Hydrogen on Titanium Abundance Determinations in Cool Stars
我们进行了非局域热力学平衡（非LTE）计算Ti I-II与更新的模型原子，其中包括非弹性碰撞与氢原子的量子力学速率系数。本文首次计算了钛原子和钛离子与氢原子的非弹性碰撞中束缚-束缚跃迁的速率系数以及Ti I + H Ti II + H-和Ti II + H Ti III + H-的电荷交换过程的速率系数。<-><->这些数据对非LTE丰度测定的影响已经在太阳和四颗贫金属恒星上进行了测试。对于Ti I和Ti II，应用导出的速率系数导致与速率系数的近似公式相比，偏离LTE和钛丰度增加。在贫金属恒星，我们未能实现一致的非LTE丰度线的两个电离阶段。文献中已知的Ti I和Ti II线在贫金属恒星中的非LTE丰度的差异不能通过改进经典模型大气中非LTE计算中与氢原子碰撞的非弹性过程的速率来解决。
Moment-based formulas for the transport coefficients
School of Science, Harbin Institute of Technology（哈尔滨理工大学理学院）；Shenzhen Key Laboratory of Numerical Prediction for Space Storm, Harbin Institute of Technology, Shenzhen（深圳大学空间风暴数值预测重点实验室）
