转动潮汐变形双星理论模型研究

转动和潮汐效应是影响双星系统结构和演化不可忽略的重要物理因素. 根据大质量双星系统V478 Cyg的观测结果, 检验了提出的转动潮汐变形的理论模型. 将转动潮汐变形的模型与传统的双星演化模型对比发现: 转动和潮汐效应使恒星外层(低于平均密度区)发生的形变远大于内层; 恒星两极点重力加速度变大, 赤道面上重力加速度变小; 转动潮汐变形模型具有较大的半径、赤道速度和中心集中度, 较低的氢核能产生率, 恒星向低温和低光度端演化. 此外, 大质量双星系统V478 Cyg由潮汐形变造成的拱线运动速率大于转动形变造成的拱线运动速率, 广义相对论效应造成的拱线运动最小. 由于主星具有较高的中心集中度, 次星潮汐、转动形变造成的拱线运动速率均大于主星相应的拱线运动速率.     

转动双星模型及演化

提出了转动双星的结构和演化模型,给出了主星的重力势,并模拟其加速度在等势面上的分布.结果表明在忽略自引力势高阶项的情况下,极地处重力加速度最大,赤道上长轴顶点处重力加速度最小.自转、公转和伴星潮汐作用力的联合效应降低了子星的有效温度,延长了子星在氢主序上的演化时间.     

三轴椭球体模型下转动双星系统的演化

采用三轴椭球体模型和非均匀的星风物质损失的理论计算,数值模拟并分析了转动双星系统的演化.结果表明子星间物质交换和氢开始燃烧提前,主序带变宽,演化更大幅度地向蓝方向运动并形成较大回绕,演化轨迹向低光度偏转,子星半径在慢速物质交换过程中出现周期性的膨胀和收缩,角动量损失率变小.     

辐射压对非同步转动双星系统洛希势函数的影响

辐射压是影响大质量恒星结构和演化不可忽视的重要物理因素. 根据辐射压对非同步转动的洛希势函数的影响, 数值计算了洛希瓣的大小和3个拉格朗日点的位置和相应的势函数, 并与同步转动的洛希模型计算的结果做了对比. 结果发现: 辐射压可以整体地减小大质量恒星表面的重力加速度, 而转动离心力能最大减少赤道附近的重力加速度. 辐射压和非同步转动均可以明显地改变洛希瓣的大小和3个拉格朗日点的位置和势函数, 影响双星系统物质交换的时间. 因此, 研究辐射压, 非同步转动等物理因素对大质量双星系统洛希势函数的影响, 对密近双星的演化具有重要意义. 关键词： 恒星结构与演化 转动 辐射压     

双星运行轨道的研究

文章首先把双星运动看做二体问题,研究以一个星体为参照系,另一个星体的轨迹为圆锥曲线,以系统的质心为参照系,每一个星体的轨迹也是圆锥曲线,然后提出了行星与恒星之间也是双星现象,地球与月球之间也是双星现象,解释了困扰物理学与天文学多年的行星运行轨道的共面性、公转的同向性难题,指出了研究行星运行轨道时惯性质量应当用折合质量计算。     

He和D_2分子相互作用转动激发研究

用T .T(K .T .TangandJ .Peter.Toennies)势模型和公认精密度较高的密耦 (Close Coupling)近似方法计算了E =0 .1eV和E =0 .2eV时 ,0 0— 0 0弹性碰撞及 0 0— 0 2、0 0— 0 4、0 0— 0 6非弹性碰撞 ,得出D2 分子转动激发分波截面 ,并得到了原子与分子碰撞弹性分波截面和非弹性激发截面随量子数增加的变化规律。     

He和D2分子相互作用转动激发研究

用T.T(K.T.TangandJ.Peter.Toennies)势模型和公认精密度较高的密耦(Close-Coupling)近似方法计算了E=0.1eV和E=0.2eV时,00-00弹性碰撞及00-02、00-04、00-06非弹性碰撞,得出D2分子转动激发分波截面,并得到了原子与分子碰撞弹性分波截面和非弹性激发截面随量子数增加的变化规律.     

旋转致密双星后牛顿轨道的引力波研究

本文利用辛算法和功率谱研究旋转致密双星保守的后牛顿哈密顿系统的引力辐射, 讨论了系统的动力学参量、旋转-轨道耦合、旋转-旋转耦合效 应及轨道类型对后牛顿近似引力波形的影响. 数值结果表明有序轨道的引力波随时间呈周期性地变化, 而混沌轨道引力波的变化具有混沌性, 并且轨道的混沌特性可提高引力波的辐射能量, 尤其指出的是旋转参量大小对引力波形的变化发挥至关重要的作用.     

临界转动恒星Achernar的斜压结构与引力昏暗的精细研究

转动和潮汐效应是影响恒星结构和演化的非常重要的物理因素. 根据对Achernar的观测数据, 用扰动理论推导了临界转动恒星Achernar分别作为单星和双星的斜压结构的特征, 给出Achernar等压面上的密度等物理量的分布. 利用考虑转动和潮汐及形变效应的单、双星模型研究了Achernar的引力昏暗现象. 结果表明正剪切增强离心力、减小赤道的重力加速度和温度, 反剪切结果则与之相反. 反剪切和刚性转动情况并不符合对Achernar的引力昏暗观测结果. 发现转动双星模型比单星模型虽更符合Achernar赤道和极半径之比的观测值, 但理论计算的角速度比观测值小. 对比理论计算和观测结果发现, 当Achernar的自转角速度为4.65× 10^-5 s^-1, 正剪切率Ω/Ω_s为0.7851时, Achernar的极点温度为16041 K, 赤道温度为12073 K. 所有理论计算与观测值的相对误差不超过7%.     

On the non-synchronous rotation of binary systems

During the evolution of the binary system,many physical processes occur,which can influence the orbital angular velocity and the spin angular velocities of the two components,and influence the non-synchronous or synchronous rotation of the system.These processes include the transfer of masses and angular momentums between the component stars,the loss of mass and angular momentum via stellar winds,and the deformation of the structure of component stars.A study of these processes indicates that they are closely related to the combined effects of tide and rotation.This means,to study the synchronous or non-synchronous rotation of binary systems,one has to consider the contributions of different physical processes simultaneously,instead of the tidal effect alone.A way to know whether the rotation of a binary system is synchronous or non-synchronous is to calculate the orbital angular velocity and the spin angular velocities of the component stars.If all of these angular velocities are equal,the rotation of the system is synchronous.If not,the rotation of the system is non-synchronous.For this aim,a series of equations are developed to calculate the orbital and spin angular velocities.The evolutionary calculation of a binary system with masses of 10M⊙+6M⊙shows that the transfer of masses and angular momentums between the two components,and the deformation of the components structure in the semidetached or in the contact phase can change the rotation of the system from synchronous into non-synchronous rotation.     

Birthrates and delay times of Type Ia supernovae

Type Ia supernovae (SNe Ia) play an important role in diverse areas of astrophysics, from the chemical evolution of galaxies to observational cosmology. However, the nature of the progenitors of SNe Ia is still unclear. In this paper, according to a detailed binary population synthesis study, we obtained SN Ia birthrates and delay times from different progenitor models, and compared them with observations. We find that the Galactic SN Ia birthrate from the double-degenerate (DD) model is close to those infe...     

Geometrical statistics of the vorticity vector and the strain rate tensor in rotating turbulence

We report results on the geometrical statistics of the vorticity vector obtained from experiments in electromagnetically forced rotating turbulence. A range of rotation rates Ω is considered, from non-rotating to rapidly rotating turbulence with a maximum background rotation rate of Ω = 5 rad/s (with Rossby number much smaller than unity). Typically, the Taylor-scale Reynolds number in our experiments is around Re_λ ≈ 100. The measurement volume is located in the centre of the fluid container above the bottom boundary layer, where the turbulent flow can be considered locally statistically isotropic and horizontally homogeneous for the non-rotating case, see L.J.A. van Bokhoven, H.J.H. Clercx, G.J.F. van Heijst, and R.R. Trieling, Experiments on rapidly rotating turbulent flows, Phys. Fluids 21 (2009) 096601. Based on the full set of velocity derivatives, measured in a Lagrangian way by three-dimensional (3D) particle tracking velocimetry, we have been able to quantify statistically the effect of system rotation on several flow properties. For the range of rotation rates considered, the experimental results show how the turbulence evolves from almost isotropic 3D turbulence (Ω ? 0.2 rad/s) to quasi-two-dimensional turbulence (Ω ≈ 5.0 rad/s), and how this is reflected by several statistical quantities. In particular, we have studied the orientation of the vorticity vector with respect to the three eigenvectors of the local strain rate tensor and with respect to the vortex stretching vector. Additionally, we have quantified the role of system rotation on the self-amplification terms of the enstrophy and strain rate equations and the direct contribution of the background rotation on these evolution equations. The main effect of background rotation is the strong reduction of extreme events and related (strong) reduction of the skewness of PDFs of several quantities, for example, the intermediate eigenvalue of the strain rate tensor and the enstrophy self-amplification term.     

Turbulent structures in cylindrical density currents in a rotating frame of reference

Gravity currents are flows generated by the action of gravity on fluids with different densities. In some geophysical applications, modeling such flows makes it necessary to account for rotating effects, modifying the dynamics of the flow. While previous works on rotating stratified flows focused on currents of large Coriolis number, the present work focuses on flows with small Coriolis numbers (i.e. moderate-to-large Rossby numbers). In this work, cylindrical rotating gravity currents are investigated by means of highly resolved simulations. A brief analysis of the mean flow evolution to the final state is presented to provide a complete picture of the flow dynamics. The numerical results, showing the well-known oscillatory behavior of the flow (inertial waves) and a final state lens shape (geostrophic adjustment), are in good agreement with experimental observations and theoretical models. The turbulent structures in the flow are visualized and described using, among others, a stereoscopic visualization and videos as supplementary material. In particular, the structure of the lobes and clefts at the front of the current is presented in association to local turbulent structures. In rotating gravity currents, the vortices observed at the lobes front are not of hairpin type but are rather of Kelvin-Helmholtz type.     

二维简谐势阱中旋转理想玻色气体热力学性质的修正

利用截断求和方法修正了二维简谐势阱中旋转理想玻色气体的热力学性质.对玻色-爱因斯坦凝聚(BEC)临界温度的修正表明:旋转框架下的BEC临界温度随旋转频率增大而快速趋近于零,到达势阱特征频率时,基态将会发生从BEC态到强关联非凝聚态的转变;由合成磁场引起的旋转对BEC临界温度的影响则要弱得多.对旋转导致的抗磁性的修正表明:磁化强度随旋转频率和合成磁场的增大而增强.利用截断求和方法计算的结果与考虑有限尺度效应的修正结果获得了很好的一致.     

含时旋转磁场中的两耦合粒子的纠缠演化(英文)

我们研究了含时旋转磁场中海森堡XXX模型下的双量子比特的动力学演化情况.基于此非自治系统的代数结构,我们用代数动力学方法求得了系统的精确解析解.在此基础上,进一步研究了在不同初态下系统的纠缠测度随时间的演化,发现纠缠测度由系统的初态的系数和耦合强度决定.     

基于旋转照明光的数字全息相干噪声抑制

提出一种数字全息相干噪声抑制方法。首先在照明光方位角给定的前提下,通过在极向平面内连续旋转照明光,实现在多角度照明条件下记录离轴数字全息图。然后对所获得的全息图分别重构,同时利用倾斜相差补偿算法和数字图像自相关配准方法分别补偿再现像的相位倾斜及横向偏移。最后将重构像进行非相干叠加,从而有效抑制再现像的相干噪声。实验结果及相关统计评价数据皆验证了该方法的有效性。