Algol, Beta Lyrae, and W Serpentis: Some new results for three well studied eclipsing binaries

The properties of the eclipsing binaries Algol, Beta Lyrae, and W Serpentis are discussed and new results are presented. The physical properties of the components of Algol are now well determined. High resolution spectroscopy of the H-alpha feature by Richards et al. and by Gillet et al. and spectroscopy of the ultraviolet resonance lines with the International Ultraviolet Explorer satellite reveal hot gas around the BBV primary. Gas flows also have been detected apparently originating from the low mass, cooler secondary component and flowing toward the hotter star through the Lagrangian L1 point. Analysis of 6 years of multi-bandpass photoelectric photometry of Beta Lyrae indicates that systematic changes in light curves occur with a characteristic period of -275 ± 25 days. These changes may arise from pulsations of the B8II star or from changes in the geometry of the disk component. Hitherto unpublished u, v, b, y, and H-alpha index light curves of W Ser are presented and discussed. W Ser is a very complex binary system that undergoes complicated, large changes in its light curves. The physical properties of W Ser are only poorly known, but it probably contains one component at its Roche surface, rapidly transfering matter to a component which is embedded in a thick, opaque disk. In several respects, W Ser resembles an upscale version of a cataclysmic variable binary system.     

Algol,Beta Lyrae,and W Serpentis: Some new results for three well studied eclipsing binaries

The properties of the eclipsing binaries Algol, Beta Lyrae, and W Serpentis are discussed and new results are presented. The physical properties of the components of Algol are now well determined. High resolution spectroscopy of the H-alpha feature by Richards et al. and by Gillet et al. and spectroscopy of the ultraviolet resonance lines with the International Ultraviolet Explorer satellite reveal hot gas around the BBV primary. Gas flows also have been detected apparently originating from the low mass, cooler secondary component and flowing toward the hotter star through the Lagrangian L1 point. Analysis of 6 years of multi-bandpass photoelectric photometry of Beta Lyrae indicates that systematic changes in light curves occur with a characteristic period of -275 ± 25 days. These changes may arise from pulsations of the B8II star or from changes in the geometry of the disk component. Hitherto unpublished u, v, b, y, and H-alpha index light curves of W Ser are presented and discussed. W Ser is a very complex binary system that undergoes complicated, large changes in its light curves. The physical properties of W Ser are only poorly known, but it probably contains one component at its Roche surface, rapidly transfering matter to a component which is embedded in a thick, opaque disk. In several respects, W Ser resembles an upscale version of a cataclysmic variable binary system.     

A gentle process for the formation of Algols

This work is concerned with binary systems that we call ‘moderately close’. These are systems in which the primary (by which we mean the initially more massive star) fills its Roche lobe when it is on the giant branch with a deep convective envelope but before helium ignition (late case B). We find that if the mass ratio q(= M ₁/M ₂) < q _crit = 0.7 when the primary fills its Roche lobe positive feedback will lead to a rapid hydrodynamic phase of mass transfer which will probably lead to common envelope evolution and thence to either coalescence or possibly to a close binary in a planetary nebula. Although most Algols have probably filled their Roche lobes before evolving off the main-sequence we find that some could not have and are therefore ‘moderately close’. Since rapid overflow is unlikely to lead to an Algol-like system there must be some way of avoiding it. The most likely possibility is that the primary can lose sufficient mass to reduce q below q _crit before overflow begins. Ordinary mass loss rates are insufficient but evidence that enhanced mass loss does take place is provided by RS CVn systems that have inverted mass ratios but have not yet begun mass transfer. We postulate that the cause of enhanced mass loss lies in the heating of the corona by by magnetic fields maintained by an α — ω dynamo which is enhanced by tidal effects associated with corotation. In order to model the the effects of enhanced mass loss we ignore the details and adopt an empirical approach calibrating a simple formula with the RS CVn system Z Her. Using further empirical relations (deduced from detailed stellar models) that describe the evolution of red giants we have investigated the effect on a large number of systems of various initial mass ratios and periods. These are notable in that some systems can now enter a much gentler Algol-like overflow phase and others are prevented from transferring mass altogether. We have also investigated the effects of enhanced angular momentum loss induced by corotation of the wind in the strong magnetic fields and consider this in relation to observed period changes. We find that a typical ‘moderately close’ Algol-like system evolves through an RS CVn like system and then possibly a symbiotic state before becoming an Algol and then goes on through a red giant-white dwarf state which may become symbiotic before ending up as a double white dwarf system in either a close or wide orbit depending on how much mass is lost before the secondary fills its Roche lobe.     

First millimetric detections of AE Aquarii

We report the first millimetric detections of the magnetic cataclysmic variable AE Aquarii, accompanied by contemporaneous microwave observations. These data show that the time-averaged spectrum is well fit by a power-law which extends to mm wavelengths. We suggest that the spectrum is consistent with that expected from a superposition of flare-like events.     

Variability of soft X-ray emission of EX Hydrae observed with Einstein Observatory

The cataclysmic variable EX Hydrae has been observed in X-rays with Einstein Observatory. A 67 min periodic X-ray modulation has been found in the energy range. 1 – 2 keV, whereas the source is approximately constant above 2 keV. The modulation is approx. in phase with the stable 47 min modulation in the optical brightness. The X-ray spectrum changes slightly with the 67 min phase but is consistent with a two component model with constant temperature only changing in relative intensity. Quasi-simultaneous optical observations were also obtained and used to extend the time base of the optical modulation. The result is indicative of a decrease in the 67 min period on a time scale of 3 10⁶ yr. The implications for the hypothesis of a non-uniform rotating white dwarf as the origin of the 67 min optical and X-ray modulation are discussed.     

The evolution of moderately close and moderately wide binaries

We discuss evolutionary processes in binaries where the primary becomes a red giant with a deep convective envelope before it fills its Roche lobe. Such binaries (late Case B or late Case C, if they evolve conservatively) ought to suffer drastic mass transfer, on a hydrodynamic timescale. In some circumstances this may lead to a common envelope, spiral-in, and finally either a very short-period binary or coalescence. But there appear to be other circumstances in which the outcome is an ordinary Algol, or a wide binary with a white dwarf companion as in Barium stars and some symbiotics. We try to demonstrate that stellar-wind mass loss, enhanced one or two orders of magnitude by tidal interaction with a companion, can vitally affect the approach to RLOF, and indeed may prevent RLOF in binaries with periods over 1000 d. Such mass loss is probably accompanied by angular momentum loss, by magnetic braking combined with tidal friction. The result is that it will not be easy to predict definitively the outcome of evolution in a given zero-age binary.     

The evolution of moderately close and moderately wide binaries

We discuss evolutionary processes in binaries where the primary becomes a red giant with a deep convective envelope before it fills its Roche lobe. Such binaries (late Case B or late Case C, if they evolve conservatively) ought to suffer drastic mass transfer, on a hydrodynamic timescale. In some circumstances this may lead to a common envelope, spiral-in, and finally either a very short-period binary or coalescence. But there appear to be other circumstances in which the outcome is an ordinary Algol, or a wide binary with a white dwarf companion as in Barium stars and some symbiotics. We try to demonstrate that stellar-wind mass loss, enhanced one or two orders of magnitude by tidal interaction with a companion, can vitally affect the approach to RLOF, and indeed may prevent RLOF in binaries with periods over 1000 d. Such mass loss is probably accompanied by angular momentum loss, by magnetic braking combined with tidal friction. The result is that it will not be easy to predict definitively the outcome of evolution in a given zero-age binary.     

A gentle process for the formation of Algols

This work is concerned with binary systems that we call moderately close. These are systems in which the primary (by which we mean the initially more massive star) fills its Roche lobe when it is on the giant branch with a deep convective envelope but before helium ignition (late case B). We find that if the mass ratio q(= M ₁/M ₂) < q _crit = 0.7 when the primary fills its Roche lobe positive feedback will lead to a rapid hydrodynamic phase of mass transfer which will probably lead to common envelope evolution and thence to either coalescence or possibly to a close binary in a planetary nebula. Although most Algols have probably filled their Roche lobes before evolving off the main-sequence we find that some could not have and are therefore moderately close. Since rapid overflow is unlikely to lead to an Algol-like system there must be some way of avoiding it. The most likely possibility is that the primary can lose sufficient mass to reduce q below q _crit before overflow begins. Ordinary mass loss rates are insufficient but evidence that enhanced mass loss does take place is provided by RS CVn systems that have inverted mass ratios but have not yet begun mass transfer. We postulate that the cause of enhanced mass loss lies in the heating of the corona by by magnetic fields maintained by an — dynamo which is enhanced by tidal effects associated with corotation. In order to model the the effects of enhanced mass loss we ignore the details and adopt an empirical approach calibrating a simple formula with the RS CVn system Z Her. Using further empirical relations (deduced from detailed stellar models) that describe the evolution of red giants we have investigated the effect on a large number of systems of various initial mass ratios and periods. These are notable in that some systems can now enter a much gentler Algol-like overflow phase and others are prevented from transferring mass altogether. We have also investigated the effects of enhanced angular momentum loss induced by corotation of the wind in the strong magnetic fields and consider this in relation to observed period changes. We find that a typical moderately close Algol-like system evolves through an RS CVn like system and then possibly a symbiotic state before becoming an Algol and then goes on through a red giant-white dwarf state which may become symbiotic before ending up as a double white dwarf system in either a close or wide orbit depending on how much mass is lost before the secondary fills its Roche lobe.     

The evolution of massive stars

The evolution of stars with masses between 15 M ₀ and 100M ₀ is considered. Stars in this mass range lose a considerable fraction of their matter during their evolution.The treatment of convection, semi-convection and the influence of mass loss by stellar winds at different evolutionary phases are analysed as well as the adopted opacities.Evolutionary sequences computed by various groups are examined and compared with observations, and the advanced evolution of a 15M ₀ and a 25M ₀ star from zero-age main sequence (ZAMS) through iron collapse is discussed.The effect of centrifugal forces on stellar wind mass loss and the influence of rotation on evolutionary models is examined. As a consequence of the outflow of matter deeper layers show up and when the mass loss rates are large enough layers with changed composition, due to interior nuclear reactions, appear on the surface.The evolution of massive close binaries as well during the phase of mass loss by stellar wind as during the mass exchange and mass loss phase due to Roche lobe overflow is treated in detail, and the value of the parameters governing mass and angular momentum losses are discussed.The problem of the Wolf-Rayet stars, their origin and the possibilities of their production either as single stars or as massive binaries is examined.Finally, the origin of X-ray binaries is discussed and the scenario for the formation of these objects (starting from massive ZAMS close binaries, through Wolf-Rayet binaries leading to OB-stars with a compact companion after a supernova explosion) is reviewed and completed, including stellar wind mass loss.     

The polars

The class of cataclysmic variables called Polars, or AM Her systems, is comprehensively reviewed. Each part of these systems, from the two underlying stars, to the accretion region and the stream, is considered in turn. New developments in our understanding of the accretion region are outlined in some detail.     

基于地月L1点的载人登月飞行方案分析

为解决传统载人登月方案中重型运载火箭难以研制、交会对接窗口选择困难等问题,提出了符合我国现有技术条件的基于地月L1点的载人登月方案设想。基于对圆形限制性三体模型和地月三,点特性的分析,将载人登月任务划分为不同的飞行阶段,研究了载人登月任务的规模、系统组成以及各舱段的质量分配等。通过与基于环月轨道方案各参数的分析和对比,提出通过付出较小代价将基于环月轨道的载人登月方案转化为基于地月,L1点的载人登月方案的方法。结果分析表明,经方案转化,不但能充分发挥地月L1点的优势,而且在一定条件下可以使节省燃料成为可能。     

复合材料变截面压杆变形性能研究

为了对复合材料变截面压杆的变形性能进行理论预测,本文以航天器空间桁架结构中的复合材料变截面压杆作为研究对象,首先,基于经典层合板理论,将复合材料变截面杆的壁板等效为主方向与杆轴线方向一致的正交异性板,此时复合材料变截面杆可近似为正交异性杆;其次,基于弹性变形理论和小变形假设,推导了反映杆轴向变形能力的等效轴压刚度理论公式;最后,利用有限元对等效轴压刚度理论的准确性进行了验证。结果表明,不同中间半径和变截面段长度条件下,理论值和有限元值之间的偏差基本保持在3%以内;不同铺层角条件下,理论值和有限元值之间的偏差基本保持在2%以内。因此,本文的理论能够较准确地预测复合材料变截面压杆的变形。     

用于结构优化的一种新的两点近似函数

提出一种基于两点信息的近似函数,它在当前设计点能够保证原函数的函数值、一阶导数值和近似二阶导数值;在另一设计点保证原函数的一阶导数值。用该近似函数形成结构优化原问题的序列近似问题,再用约束变尺度法解近似问题。通过典型算例的计算,结果表明本方法具有较好的收敛性和较高的计算效率,适用于结构优化问题的求解     

涡轮叶片内部冷却通道传热和压力 分布特性的实验

针对带45°肋片圆形弯头U型通道进行了传热和压力分布特性的实验研究.实验中进口雷诺数变化范围在30000~55000之间.研究表明,肋片引起的横向二次流在弯头前区域是强化传热的主要因素.不同雷诺数下传热分布和压力分布的趋势完全一致,但弯头区后半段上传热分布有所差异.通道中的最大压降出现在弯头区,进口雷诺数越大,弯头损失系数和总损失系数都有所减小.流体在圆形弯头中,加速效果没有矩形弯头强烈,弯头区和弯头后的传热较矩形弯头都有较大幅度地减小.      

工程数值优化方法研究进展

回顾与分析了工程数值优化方法研究的发展历程 ,着重介绍与讨论了优化问题的几种数学列式、近似问题的保真度与近似函数 ,以及复杂优化问题的求解策略等。指出优化问题的对偶列式变式 DFOP-V2与高精度多点近似函数和二级近似概念结合而产生的数值优化解法 ,具有通用性 ,高的计算效率 ,并易于与市场现有分析软件结合使用等显著优点     

Radar Signature of a Helicopter Illuminated by a Long LFM Signal

Helicopters exhibit a very particular Doppler radar signature caused by the movement of rotor blades. This signature can easily be derived using a short-time approximation: the blades are assumed to be static during each pulse. In wideband linear frequency modulated (LFM) radars, however, this assumption cannot be made. The work presented here describes the echo of rotary blades illuminated by LFM radars without the short-time assumption and provides useful information for detection and recognition purposes.     

一种新型涡轮叶栅非轴对称端壁造型的数值研究

为探讨非轴对称端壁造型降低涡轮叶栅二次流损失的有效性,构建基于高压涡轮直列叶栅的非轴对称端壁气动优化设计方法,并用NUMECA／FineTurbo模块对优化后的结果和原涡轮叶栅分别进行流场计算。结果表明：非轴对称端壁造型使叶栅通道的总压损失系数面降低了2．84％;改变了通道内的叶片载荷分布,形成了叶型的载荷后置;改善了流场内的流动结构,使气流的流动变得更加通畅;延迟了通道涡的过早形成,减小了通道涡的强度和尺度。因此,非轴对称端壁造型可以有效地降低涡轮叶栅通道内的二次流损失。     

大子午扩张变几何涡轮可调叶片端区设计优化

提出采用高负荷设计以减少叶片数的方法,增大圆盘直径而减小泄漏面积;结合叶片进行后加载改型措施以减小由于高负荷设计所增加的二次流损失.对定几何涡轮、仅有驱动轴的变几何涡轮与带圆盘型冠的变几何涡轮的流场进行三维数值模拟计算,分析了3种涡轮性能的优劣.结果表明:大间隙尺度下了间隙泄漏涡强度较大,并与通道涡相互融合,从而增大了泄漏损失区域,增加了泄漏损失;而在涡轮叶片由于高负荷设计会增加了主流区的二次流损失.该方法可以有效地减小周向泄漏面积,极大地抑制由大间隙尺度所导致的间隙泄漏涡与通道涡的相互融合,减小泄漏损失.而通过后加载改型的措施,抑制了主流区的通道涡的发展趋势,减小了二次流损失.这两种措施结合后的变几何涡轮具有较高的全工况性能.      

前体激波系重构技术及其在高超声速进气道上的应用

提出了一种激波系整体重构的激波控制技术,并对其流动机理和控制规律进行了仿真分析,继而探索了其在定几何可调进气道上的应用.研究结果表明:该激波控制方法可对前体第1级激波进行有效推动,并可减弱第2级激波强度甚至使其完全蜕化,故实现了对前体激波系的重新构造.随着二次流注入缝的角度增大,将前体激波推动至贴口状态所需消耗的二次流流量逐步减少.并且,最多消耗占主流2.04%的二次流,便可使该进气道在马赫数为5.0~6.0范围内保持贴口状态.与已有各级激波独立控制的可调进气道相比,该进气道在调节状态下的总压恢复较高、消耗的二次流较少,具有明显的优势.      

500 – 3200 Å observations of the interacting binary stars V356 Sgr and β Lyr

In this paper we present new results from the Voyager ultraviolet spectrometers and the IUE spacecraft on V356 Sgr and β Lyr. The V356 Sgr observations cover, in detail, two eclipses and include one IUE high dispersion SWP image. During both eclipses the total strength of the UV emission lines were found to be invariant. Also, an uneclipsed UV continuum was detected at wavelengths shorter than 1600 Å. The IUE high dispersion SWP spectrum revealed that the emission lines are extremely broad, almost symmetrical lines with weak, slightly blue shifted absorption components. No evidence of carbon is seen in the emission or absorption spectrum of V356 Sgr in eclipse. A model for the origin of the circumstellar matter in this binary system is presented. The Voyager ultraviolet observations of β Lyr show a strong far-UV continuum that is detectable down to 912 Å The far-UV continuum flux level was variable on time scales shorter than the orbital period and displayed no obvious orbital modulation or eclipses. The spectral shape of the far-UV continuum closely resembles that of a UX UMa type cataclysmic variable. On 16 August 1985 an rapid brightening of the far-UV continuum was observed which was also reminiscent of cataclysmic variables. Analysis of the β Lyr data suggest that the central object must be small, with a radius on the order of 1 R_⊙ or less.