We present two self-consistent procedures that couple the hydrodynamics with calculations of the line-force in the frame of radiation wind theory. These procedures give us the line-force parameters, the velocity field, and the mass-loss rate. The first one is based on the so-called m-CAK theory. A full set of line-force parameters for $T_\text{eff}\ge 32,000$ K and surface gravities higher than 3.4 dex for two different metallicities are presented, along with their corresponding wind parameters. We find that the dependence of line-force parameters on effective temperature is enhanced by the dependence on $\log g$. For the case of homogeneous winds (without clumping) comparison of self-consistent mass-loss rates shows a good agreement with empirical values. We also consider self-consistent wind solutions that are used as input in FASTWIND to calculate synthetic spectra. By comparison with the observed spectra for three stars with clumped winds, we found that varying the clumping factor the synthetic spectra rapidly converge into the neighbourhood region of the solution. Therefore, this self-consistent m-CAK procedure significantly reduces the number of free parameters needed to obtain a synthetic spectrum.
The second procedure (called Lambert-procedure) provides a self-consistent solution beyond m-CAK theory, and line-acceleration is calculated by the full NLTE radiative transfer code CMFGEN. Both the mass-loss rate and the clumping factor are set as free parameters, hence their values are obtained by spectral fitting after the respective self-consistent hydrodynamics is calculated. Since performing the Lambert-procedure requires significant computational power, the analysis is made only for the star z-Puppis.
The promising results gives a positive balance about the future applications for the self-consistent solutions presented on this thesis.
Models for Weak Wind and Momentum Problems in the Winds of Hot Stars
我们提出了热星风超音速部分的速度结构模型，以估计密度和速度聚集的影响。使用XSTAR（Kallman，2018）计算Sobolev近似下谱线（力倍增器FM）中的辐射压力（Castor等人，1975 CAK; Stevens和Kallman，1990）。FM计算为两个参数的函数：Xi和t。线力包含在动量方程和质量守恒中。这些被集成在超音速部分的风的一个样本的OB-和WR-明星。用速度定律进行拟合，得到质量损失率和流出速度作为输出。亚音速部分的边界条件和速度定律用β定律公式（β = 0.6，Vin = 10 km/s）近似。据发现，WR-星，由于其大的吸收，已经在r/Rstar = 1.01辐射光谱缺乏软X射线低于230埃（氦II电离）。这一关键事实将力乘数提高了10倍，使其能够在CAK框架中加速风。因此，动量问题是一个不透明度问题（Gayley et al.，1995）。OB-stars的结果指向中等密度的聚集（Fvol=0.13）。此外，主序星OB需要速度聚集（Fvel=0.1，Sundqvist et al 2014）。这可以解释弱风的问题。
Radiation-driven winds of hot luminous stars. XVIII. The reliability of stellar and wind parameter determinations from spectral analysis of selected central stars of planetary nebulae and the possibility of single-star SN Ia progenitors
The relative impact of photoionizing radiation and stellar winds on different environments
来自大质量恒星的光致电离辐射和恒星风将能量和动量储存在星际介质中。它们可能会分散局部的ISM，改变其湍流的多相结构，甚至调节恒星的形成。电离辐射在大质量恒星的能量输出中占主导地位，但风的相对影响可能会随着恒星质量和周围ISM的性质而变化。模拟了12、23和60 M $_{\odot}$星在冷中性（CNM，$n_{0}$ = 100 cm $^{-3}$）、暖中性（WNM，$n_{0}$ = 1，10 cm $^{-3}$）或暖电离（WIM，$n_{0}$ = 0.1 cm $^{-3}$）介质中的星风和电离辐射的相互作用。FLASH仿真采用了新的基于树的辐射传输算法TreeRay。在现场近似和温度依赖的复合系数，它是耦合到一个化学网络与辐射加热和冷却。在均匀的CNM中，总动量注入范围从1.6 $\times$ 10 $^{4}$到4 $\times$ 10 $^{5}$ M $_{\odot}$ km s $^{-1}$，并且总是由电离H $_{\text{II}}$区域的膨胀所主导。在WIM中，恒星风占主导地位（2 $\times$ 10 $^{2}$到5 $\times$ 10 $^{3}$ M $_{\odot}$ km s $^{-1}$），而来自辐射的输入很小（$\sim$ 10 $^{2}$ M $_{\odot}$ km s $^{-1}$）。WNM（$n_{0}$ …
Metastable Helium Absorptions with 3D Hydrodynamics and Self-Consistent Photochemistry II: WASP-107b, Stellar Wind, Radiation Pressure, and Shear Instability
Radiation-ionization hydrodynamic simulations of AGN line-driven winds lead to transient shielding and BAL/UFO signatures
School of Physics and Astronomy, University of Southampton（南安普顿大学物理与天文学院）；Eureka Scientific Inc.（尤里卡科学公司）；Univ. Grenoble Alpes, CNRS, IPAG（格勒诺布尔阿尔卑斯大学，法国国家科学研究中心，天体物理学与行星学研究所）；Space Telescope Science Institute（太空望远镜科学研究所）；Department of Physics, Astrophysics, University of Oxford（牛津大学物理与天体物理系）；School of Mathematics and Physics, Queen’s University Belfast（贝尔法斯特女王大学数学与物理学院）
Solar Magnetic Configuration Control over Radiation Belt Electrons
Northumbria University（诺森比亚大学）；University College London, Mullard Space Science Laboratory（伦敦大学学院穆拉德空间科学实验室）；Donostia International Physics Center (DIPC)（圣塞巴斯蒂安国际物理中心）；Johns Hopkins University, Applied Physics Laboratory（约翰斯·霍普金斯大学应用物理实验室）
