本文研究了有效温度1.5e4K <= Teff <= 3e 4K，辐射光度1.2e6L_odot <= L <= 1.9e6L_odot，质量35.7M_odot <= M <= 49.1M_odot的LBV--星激发的非线性径向振荡。根据星族I星（X=0.7，Z=0.02）的演化序列，以70 ~ 90 Modot的初始质量为初始条件，进行了流体动力学计算。所有的流体动力学模型都表现出对径向振荡的不稳定性，其振幅增长时间与恒星的动力学时间尺度相当。径向振荡以非线性行波的形式存在，从致密核的边界传播到流体动力学模型的上边界。外层的速度振幅是几百公里/秒，而辐射光振幅不超过0.2马格。恒星振荡不是由卡帕机制驱动的，是由于气体的不稳定性与绝热指数接近临界值Gamma_1 = 4/3，由于在总压的辐射的贡献大。流体动力学模型的光变周期范围（6天<= P <= 31天）与在LBV--星中观测到的微变周期一致。
英文摘要：
In this study we consider the nonlinear radial oscillations exciting in LBV--stars with effective temperatures 1.5e4 K <= Teff <= 3e4 K, bolometric luminosities 1.2e6 L_odot <= L <= 1.9e6 L_odot and masses 35.7 M_odot <= M <= 49.1 M_odot. Hydrodynamic computations were carried out with initial conditions obtained from evolutionary sequences of population I stars (X=0.7, Z=0.02) with initial masses from 70M_odot to 90 M_odot. All hydrodynamical models show instability against radial oscillations with amplitude growth time comparable with dynamical time scale of the star. Radial oscillations exist in the form of nonlinear running waves propagating from the boundary of the compact core to the upper boundary of the hydrodynamical model. The velocity amplitude of outer layers is of several hundreds of km/s while the bolometric light amplitude does not exceed 0.2 mag. Stellar oscillations are not driven by the kappa-mechanism and are due to the instability of the gas with adiabatic exponent close to the critical value Gamma_1 = 4/3 due to the large contribution of radiation in the total pressure. The range of the light variation periods (6 day <= P <= 31 day) of hydrodynamical models agrees with periods of microvariability observed in LBV--stars.
最壮观的变星是亮蓝变星（LBV），它可以显示三种类型的变化。对LBV进化阶段的了解很少，并且不知道可变性的驱动机制。最常见的变异类型，S Dor不稳定性，发生在数十年的时间尺度上。在S Dor爆发期间，恒星的视星等增加，而热星等保持近似不变。在这项工作中，我们调查脉动作为一个可能的触发S多尔型爆发。我们使用非线性流体动力学代码，包括随时间变化的对流处理的包络模型计算脉动。我们初始化的脉动流体动力学模型的基础上线性非绝热计算。计算了从20到85 M $_{\odot}$的完整网格模型的脉动特性，在本文中，我们专注于少数几个模型，显示长周期脉动或爆发的行为，光球径向速度达到70-80公里/秒。目前，我们的模型无法跟踪质量损失，因此一旦爆发事件开始，我们的模拟就终止了。我们的研究结果表明，脉动本身不能驱动足够的表面膨胀，以喷射外层。然而，这里讨论的爆发和长周期脉动会产生有效温度和光度的巨大变化，预计会产生辐射驱动的质量损失率的巨大变化。
Evolution of wide O star binaries through their LBV stage. Population synthesis with mass-ejection-driven orbital evolution
Tsung-Dao Lee Institute, Shanghai Jiao-Tong University（上海交大李政道研究所）；London Institute for Stellar Astrophysics（伦敦恒星天体物理学研究所）；University of Oxford, St Edmund Hall（牛津大学圣埃德蒙学堂）；Argelander-Institut für Astronomie, Universität Bonn（波恩大学阿格勒兰德尔天文学研究所）；Purple Mountain Observatory, Chinese Academy of Sciences（中国科学院紫金山天文台）；School of Astronomy and Space Science, Nanjing University（南京大学天文与空间科学学院）；Key Laboratory of Modern Astronomy and Astrophysics, Nanjing University, Ministry of Education（南京大学现代天文与天体物理教育部重点实验室）；School of Physics and Astronomy, Monash University（蒙纳士大学物理与天文学院）；Dublin Institute for Advanced Studies, Astronomy & Astrophysics Section, DIAS Dunsink Observatory（都柏林高等研究院天文与天体物理部都柏林星象观测站）；Max-Planck-Institut für Astrophysik（马克斯·普朗克天体物理学研究所）
The IACOB project: IV. New predictions for high-degree non-radial mode instability domains in massive stars and connection with macroturbulent broadening
Probing the wind and evolutionary state of the quiescent luminous blue variable Var$\,$2 in the Galaxy M33: constraints from self-consistent non-LTE modeling
Linear and nonlinear properties of the Goldreich-Schubert-Fricke instability in stellar interiors with arbitrary local radial and latitudinal differential rotation
Nonlinear Outcome of Coagulation Instability in Protoplanetary Disks I: First Numerical Study of Accelerated Dust Growth and Dust Concentration at Outer Radii
