Determining rotation rates from light curves: RW Mon and RW Tau

We present light curve solutions for the non-synchronously rotating Algols RW Mon and RW Tau, and we illustrate how rotation rates are determined from light curves. We find RW Mon's primary component to spin at about 5 times the synchronous rate, which confirms the indication of fast rotation from reported emission line activity. RW Tau turns out to be only a mildly rapidly rotating Algol system, and our light curve solutions do not yield any firm value for the rotation rate of the primary component. It is suggested that continued efforts should be made to do good quality line broadening studies in order to find rotation rates for systems with only modest degrees of rapid rotation, and in order to further test photometric rotation rates against those of line broadening studies.     

New ways to rotation rates

Progress in determining rotation rates of Algol primary stars from light curves is assessed. Included are elementary ideas on why the new method works, how to carry out solutions, and how and when to apply the constraint on rotational lobe filling. Some comments are made on desirable improvements for measuring rotation from line broadening. A few remarks are made about the problem of identifying likely fast rotating Algols.     

New ways to rotation rates

Progress in determining rotation rates of Algol primary stars from light curves is assessed. Included are elementary ideas on why the new method works, how to carry out solutions, and how and when to apply the constraint on rotational lobe filling. Some comments are made on desirable improvements for measuring rotation from line broadening. A few remarks are made about the problem of identifying likely fast rotating Algols.     

The relation of Algols and W Serpentis stars

Evidence on the issues of whether the W Serpentis stars are a coherent class, and how they may interface with the Algol systems, is reviewed, with emphasis on the idea that they are semi-detached systems in the latter part of the rapid phase of mass transfer, with optically and geometrically thick disks of transferred gas around the (now) more massive star. We are interested in what will be seen when the gas clears away, and mainly examine the idea that it will be an Algol-type system. More particularly, consideration is given to centrifugally limited accretion as a mechanism to build up a substantial disk, and the presumed evolutionary sequence is from a W Ser to a rapidly rotating Algol to a normal Algol system. Systems such as V367 Cyg and RW Tau fit into this scheme only with difficulty. Because it is extremely difficult to measure the rotation of some W Ser (mass) primaries, it is natural to look at the rotation statistics of Algols to test this idea. The badly behaved light curves and spectroscopy of some Algols (eg. U Cep, RZ Sct) may be attributable to the double contact condition, and the ramifications of this possibility are discussed. If so, the rotation statistics of Algols should show two spikes, corresponding to the two special conditions into which a system should be driven by tidal braking and centrifugally limited spinup. Present rotation statistics do show these spikes. Algols should flip between these states fairly quickly, depending on the mass transfer rate. Thus, to the extent that the meager statistics can be accepted as meaningful, the new (fourth) morphological type of close binary (double contact) has attained demonstrable reality. The rotation statistics are presented in terms of a particular rotation parameter, R, which is zero for synchronism and unity for the centrifugal limit. Future work should develop rotation statistics to see if the rotational lobe-filling (R = 1) spike persists. It should also look into whether W Ser primaries are on the hydrogen burning main sequence, or in general what they are. We also need more light curves of W Ser type systems, high resolution line profiles for the (mass) primaries (with particular attention to the W Ser-Algol transition cases), and spectroscopy of low inclination W Serpentis systems, such as KX And.     

The relation of Algols and W Serpentis stars

Evidence on the issues of whether the W Serpentis stars are a coherent class, and how they may interface with the Algol systems, is reviewed, with emphasis on the idea that they are semi-detached systems in the latter part of the rapid phase of mass transfer, with optically and geometrically thick disks of transferred gas around the (now) more massive star. We are interested in what will be seen when the gas clears away, and mainly examine the idea that it will be an Algol-type system. More particularly, consideration is given to centrifugally limited accretion as a mechanism to build up a substantial disk, and the presumed evolutionary sequence is from a W Ser to a rapidly rotating Algol to a normal Algol system. Systems such as V367 Cyg and RW Tau fit into this scheme only with difficulty. Because it is extremely difficult to measure the rotation of some W Ser (mass) primaries, it is natural to look at the rotation statistics of Algols to test this idea. The badly behaved light curves and spectroscopy of some Algols (eg. U Cep, RZ Sct) may be attributable to the double contact condition, and the ramifications of this possibility are discussed. If so, the rotation statistics of Algols should show two spikes, corresponding to the two special conditions into which a system should be driven by tidal braking and centrifugally limited spinup. Present rotation statistics do show these spikes. Algols should flip between these states fairly quickly, depending on the mass transfer rate. Thus, to the extent that the meager statistics can be accepted as meaningful, the new (fourth) morphological type of close binary (double contact) has attained demonstrable reality. The rotation statistics are presented in terms of a particular rotation parameter, R, which is zero for synchronism and unity for the centrifugal limit. Future work should develop rotation statistics to see if the rotational lobe-filling (R = 1) spike persists. It should also look into whether W Ser primaries are on the hydrogen burning main sequence, or in general what they are. We also need more light curves of W Ser type systems, high resolution line profiles for the (mass) primaries (with particular attention to the W Ser-Algol transition cases), and spectroscopy of low inclination W Serpentis systems, such as KX And.     

倾转旋翼机转动机构运动学仿真分析

转动机构在倾转旋翼机过渡飞行阶段起着重要作用。为了研究倾转旋翼机转动机构在发动机短舱与旋翼向前倾转90°过程中的运动特征,寻找较为适用的转动模式,以倾转旋翼机转动机构为研究对象,简化机构模型,采用MATLAB软件计算两种转动方案机构的运动学特征,采用LMS软件仿真两种方案机构的转动过程。通过对比分析两种方案的运动学特征图,发现MATLAB和LMS软件得出的两种方案的角速度、速度、角加速度和加速度曲线是一致的,两种方案各有其优势。     

有无叶顶冷却涡轮叶栅气热性能的旋转效应研究

为揭示叶片或机匣旋转条件和叶顶冷却对涡轮动叶气热性能的影响机理,选用LISA 1.5级涡轮动叶片,构建叶顶冷却孔,开展了不同冷气流量下的数值模拟研究。计算结果表明:不同旋转条件下,当冷气与主流的流量比为0.3%时,叶栅能量损失最低,当流量比为1.0%时,间隙泄漏流量最低、叶顶传热性能最好。叶片旋转、机匣旋转和平移运动都能降低泄漏损失和泄漏流量,叶片旋转时,叶栅出口下游上半叶高截面的能量损失最大降低约26.10%。旋转效应对泄漏损失的影响不随流量比变化而改变,但对叶栅总损失和叶顶传热品质的影响随流量比增加会不同。当流量比小于0.3%时,叶片旋转情况下叶栅总损失低于静止工况但高于机匣运动工况,且叶顶传热品质最优;当流量比大于0.7%时,叶片旋转使叶栅总损失最高,机匣运动使叶顶传热品质最优。     

旋转对冲击射流流动及换热影响的数值研究

为了探究旋转对动叶前缘冲击射流流动及换热的影响机制,采用数值模拟的方法对比分析了静止条件和三种不同旋转转速下的流场结构与换热情况。结果表明:冲击靶面的平均努塞尔数随转速的增大而减小,最高转速下,靶面平均努塞尔数下降约16%。另一方面,压力面和吸力面侧对旋转的敏感性不同。高转速下,换热的削弱主要集中在吸力面和压力面无量纲弧长s/d小于2的区域,压力面s/d大于2区域的换热略有增强;旋转对流场结构产生了明显的影响,旋转改变了射流孔的流量分配,在科氏力的作用下,射流向压力面偏转,这种特征随转速的增大而更加显著。另外,旋转通道内的离心力改变了局部横向流强度。      

跨声速压气机转子叶尖泄漏涡非定常特性数值研究

为了研究跨声速单转子压气机系统叶尖泄漏涡的非定常特性,选取Rotor 67孤立转子为研究对象,针对不同背压工况与不同转速工况进行了非定常数值模拟。结果表明:在每一转速状态都存在一非定常边界,其将特性线分为定常部分和非定常部分。当转子运行在特性线非定常部分时,随着背压提高,叶尖泄漏涡脉动频率逐渐减小。这是由于背压提高使叶尖前缘负荷变小,叶尖泄漏涡的驱动力也变小。叶尖泄漏涡的频率特征与转子转速息息相关。高转速状态时叶尖泄漏涡主要表现出低频特征,低转速状态时叶尖泄漏涡主要表现出高频特征。这是由于转速不同,叶尖激波的脱体程度不同,激波对于叶尖泄漏涡的激励位置也不同。由非定常叶尖泄漏涡引起的压力波的周向传播速度在各转速下表现出较强的规律性。随着流量系数的减小,压力波波速呈线性减小趋势,且各转速下减小的速率大致相同。且在波速-流量系数曲线中,各转速的非定常状态起始点基本位于同一条直线。      

旋转方截面U型通道分离流二阶相关分量测量

为了深入了解旋转涡轮叶片内冷通道中的紊流特性，并为CFD研究提供实验数据，用激光多普勒测速仪（LDA）测量了旋转U型通道中分离流的雷诺应力分量。通道的转轴与弯道的曲率轴平行，测量是在与转轴垂直的对称平面中进行的，流动状态为Re=100,000,Ro=0,0.2和－0．2。直接测量的分量为ux^2^-,Ux^2^-和uxux^-，结果表明旋转对紊流分布的形式有很强的影响。在测量的三种旋转状态中Ro=0.2的正转和Ro=0.2的负转分别具有最低和最高的紊流强度。根据测量到的信息估算了雷诺应力uiuj^-的产生率，结果显示负转的产生率比正转时高。     

涡轮泵转子的临界转速研究(Ⅳ)分布质量轴的传递矩阵法

根据旋转的 Timoskenko梁的运动微分方程式 ,导出分布质量轴段的 4× 4阶精确传递矩阵 ,计入轴分布质量的平动惯量、转动惯量、陀螺力矩和剪切变形的影响 ,并计算了三个转子的临界转速。算例的计算结果表明 ,轴模型是否按分布质量考虑、是否计入平动惯量、转动惯量、陀螺力矩和剪切变形 ,对临界转速有明显的差别 ;同时在等截面轴不分段情况下 ,传递矩阵的计算结果和精确解一致性很好 ,表明计算实际转轴临界转速时 ,只需按截面不同划分轴段 ,即所取的轴分段数量少 ,就可以达到很高的计算精度     

转静系盘腔转盘风阻温升实验

采用红外测温技术对转静系盘腔转盘风阻温升特性进行了实验研究,利用高速旋转实验台测量了不同流动参数以及转静间隙比下转盘各半径处的壁面温升,并研究了径向出流处增加封严环对于转盘温升量的影响.同时通过CFD数值模拟得到转静系盘腔内流动特点.结果表明:由于风阻引起转盘温升量实际上就是转盘的绝热壁温与环境温度之差,并能通过红外热像仪准确测量.针对无封严开式转静系,转盘温升量主要受到旋转影响,仅在小转静间隙比时,通流的变化才会影响风阻温升.总体上,转静间隙比的改变对转盘温升影响不大.与封严转静系对比可知,在湍流参数较小的情况,封严环的引入会使转盘温度有所升高.      

强制对流对 Al-4.5wt%Cu 合金枝晶生长的影响

研究了ACRT（坩埚加速旋转技术）对Al-4.5wt%Cu合金在静态温度梯度GL为120℃/cm时枝晶生长的影响。实验发现,在给定抽拉速度下,枝晶一次间距λ1随着坩埚旋转强度的增大而减小;而在给定的坩埚旋转参数下,λ1随着抽拉速度的增大而降低。经过线性回归,发现λ1∝V-b,此处V为生长速度;b的取值范围为0.31～0.38,并随着坩埚旋转强度的增大而减小。此外,坩埚加速旋转产生的强制对流限制了枝晶高次分枝的生长,促使一次枝晶生长过程中的分叉。通过对强制对流的具体分析,解释了ACRT对枝晶生长影响的机理。     

基于形态分量分析与阶次跟踪的齿轮箱复合故障诊断方法

针对变转速下齿轮箱复合故障的故障特征提取,提出了基于形态分量分析与阶次跟踪的齿轮箱复合故障诊断方法.该方法根据齿轮箱复合故障振动信号中齿轮和滚动轴承故障成分的形态差异性,先用形态分量分析将其分解为包含齿轮局部故障信息的谐振分量、包含滚动轴承局部故障信息的冲击分量和随机噪声分量,再根据实测转速信号分别对谐振分量和冲击分量进行包络阶次分析,根据各包络阶次谱诊断齿轮箱复合故障.算法仿真和应用实例表明:该方法能有效分离变转速下齿轮和滚动轴承的故障特征,且其故障特征提取效果要优于传统的包络阶次谱方法.      

旋转通道一维非定常计算模型

采用特征线法,对航空发动机二次空气系统的旋转通道结构一维非定常流动及换热的计算模型进行了研究,通过将广义的定截面、有摩擦、考虑对外热交换的旋转通道可压缩非定常流动偏微分方程组转换为常微分方程组,考虑旋转离心力,并采用Colebrook White方程定义其阻力特性,进而获得旋转通道内部沿流动方向压力、质量流量、温度等系统参数的特征线数值解,采用商业软件Fluent对其进行验证.结果表明:特征线法利用压力波传播方式对旋转通道进行求解,能够直观地描述旋转通道一维非定常流动及换热特性,计算误差不超过5%,可以作为二次空气系统旋转通道一维非定常计算研究的有效手段.      

1.5级涡轮实验台前腔燃气入侵实验

在1.5级涡轮实验台上,针对不同转速和不同封严质量流量,分别采用稳态压力测量、瞬态压力测量和二氧化碳体积分数法对燃气入侵现象进行了实验研究,以确定不同工况下主流的动静叶相互作用对燃气入侵的影响以及入侵到盘腔的燃气在腔内与冷气的掺混过程.结果表明:静叶后的时均压力在周向有明显的周期分布,部分区域封严环外的压力高于腔内压力,且随着封严质量流量增加,这一区域逐渐缩小;动叶扫掠带来同频率的压力波动,对于燃气入侵的发生有着重要的影响;通过二氧化碳体积分数实验获得了最小封严质量流量,并得到在封严质量流量不足情况下燃气沿着静盘侧入侵盘腔的结果.      

基于权函数法的应力强度因子计算和断裂评估

仅利用一个参考载荷,建立一种近似公式来计算共线裂纹和中心裂纹的张开位移。通过该方法确定的裂纹面张开位移及其偏导与精确解之间吻合良好。该方法将中心裂纹的权函数计算模型简化为形状因子和裂纹面张开位移偏导之间的积分。基于权函数法,研究了带中心裂纹的旋转叶片的应力强度因子与裂纹长度、位置、转速及转动加速度之间的关系。结果发现:应力强度因子随着裂纹长度的增加和裂纹与旋转轴间距的减小而增大;转动加速度对应力强度因子的影响较小;转速的增大会使应力强度因子增大。在断裂力学理论的基础上,建立了断裂控制准则,计算表明叶片的临界转速随着裂纹长度的增加而降低。     

The Rotation of the Fe XIV Solar Corona During the Recent Solar Activity Minimum

We analyze data observed by the LASCO C1 coronagraph on board the SOHO spacecraft during the solar minimum activity from April 1996 to March 1997. Using the phase dispersion technique, we investigate the periodicity and recurrence of Fe XIV emission structures with heliospheric latitude and distance above the Sun's surface with high spatial resolution. We find no significant deviation from a rigidly rotating Fe XIV corona with latitude or with distance from the Sun even on these small scales. In agreement with earlier work, the coronal rotation period at solar minimum is about 27.5 ± 1 days. This revised version was published online in June 2006 with corrections to the Cover Date.     

变刚性支承转子的动力特性讨论

一、一种理想的转子稳态幅频线 一个转子如采用不同刚性的支承,则转子支承系统的幅频特性（r～ω）线不同。图1中虚线示出同一转子采用低刚性引和较高刚性K₂′支承时的幅频特性线1和2。有人想利用改变支承的方法来减小通过临界转速时的振动。方法是对图1（a）情况在转子角速度ω≤ω_Ⅰ时使支承刚性为k₂′,ω≥ω_Ⅰ时变支承刚性为K₁′;对图1（b）的情况则在ω≤ω_Ⅰ和ω_Ⅱ≤ω≤ω+Ⅲ支承刚性.