Cooling of neutron stars and X-ray observations

Cooling of neutron stars is calculated using an exact stellar evolution code. The full general relativistic version of the stellar structure equations are solved, with the best physical input currently available. For neutron stars with a stiff equation of state, we find that the deviation from the isothermality in the interior is significant and that it takes at least a few thousand years to reach the isothermal state. By comparing the most recent theoretical and observational results, we conclude that for Cas A, SN1006, and probably Tycho, standard cooling is inconsistent with the results from the Einstein Observatory, if neutron stars are assumed to be present in these objects. On the other hand, the detection points for RCW103 and the Crab are consistent with these theoretical results.On leave from Department of Physics, Ibaraki University, Japan     

σ-stability analysis of hydromagnetic instabilities in stars with toroidal magnetic fields

-stability analysis is used to investigate the adiabatic stability of a star containing an axisymmetric toroidal magnetic field. Necessary and sufficient conditions for -stability are derived. Special attention is devoted to the typical hydromagnetic instabilities that can be introduced by a weak toroidal magnetic field in a star that is stably stratified in the absence of any magnetic field. An expression for the maximum growth rate of instability is derived and the basic properties of the displacement fields associated with the instabilities are indicated.     

旋转整流罩积冰过程中水膜流动和脱离的数值研究

为了更准确地模拟旋转整流罩积冰过程,在现有三维积冰与冰层表面薄水膜流动耦合模型基础上,基于功平衡分析的方法引入了旋转部件表面水膜脱离模型,并发展了相应的计算方法,给出了水膜脱离的判定依据:当气流曳力做的功和由于离心力使水膜增加的潜能之和大于黏附功时整流罩表面的水膜会发生脱离。对旋转整流罩积冰进行数值模拟,计算结果与实验结果吻合得较好,验证了该模型的合理性和计算方法的可行性。之后分析了转速和来流速度对整流罩表面水膜脱离和积冰的影响,结果表明:转速和来流速度越大,水膜发生脱离的比例越大。在研究范围内,转速为3000r/min和6000r/min时,因水膜脱离导致积冰总量分别减少13.4%和15.8%;来流速度为40、50m/s和60m/s时,因水膜脱离导致积冰总量分别减少为12.2%、13.4%、14.2%。      

迎风面三维积冰过程中水膜流动的计算方法

对影响迎风面三维积冰过程的冰层表面水膜流动进行分析,建立描述其流动的数学模型,引入在流动前锋下游预设薄水膜的方法处理其在表面干区的流动推进过程,提出超过临界厚度的水膜被吹除的方法处理角状冰下游局部水膜被吹离表面的现象.通过对翼型-平板结构中翼型上的冰形对比和水膜流动规律分析,验证了该水膜流动数学模型的合理性和计算方法的可行性.研究表明:与Messinger模型相比,积冰模型中引入水膜流动后,可以较好地模拟三维明冰积冰,同时明冰极限的模拟结果也更接近试验值;冰层表面的水膜厚度约为10-5m,流动速度约为10-2m/s.      

Streamwise-body-force-model for rapid simulation combining internal and external flow fields

A streamwise-body-force-model (SBFM) is developed and applied in the overall flow simulation for the distributed propulsion system, combining internal and external flow fields. In view of axial stage effects, fan or compressor effects could be simplified as body forces along the streamline. These body forces which are functions of local parameters could be added as source terms in Navier-Stokes equations to replace solid boundary conditions of blades and hubs. The val-idation of SBFM with uniform inlet and distortion inlet of compressors shows that pressure perfor-mance characteristics agree well with experimental data. A three-dimensional simulation of the integration configuration, via a blended wing body aircraft with a distributed propulsion system using the SBFM, has been completed. Lift coefficient and drag coefficient agree well with wind tun-nel test results. Results show that to reach the goal of rapid integrated simulation combining inter-nal and external flow fields, the computational fluid dynamics method based on SBFM is reasonable.     

Effects of DC and AC electric and magnetic fields on people andanimals

The calculation of field intensity is briefly reviewed. The effects of DC fields and fields from 60-Hz and three-phase power lines are discussed. Measurement of the field under a 12-kV distribution line is described. The insignificant nature of most exposure is emphasized     

喷嘴间距对贫油熄火特性和流场结构的影响

为深入认识喷嘴间距对燃气轮机燃烧室贫油熄火和气动性能的影响,基于典型的双旋流扩散燃烧喷嘴设计了喷嘴位置连续变化可调的双头部模型燃烧室。实验测量了不同初始当量比条件下喷嘴间的最大传焰距离,分析了火焰传播的动态过程;此外还研究了喷嘴间距对贫油熄火当量比、反应流场和方均根速度场的影响。实验结果表明:当量比每增加0.1,无量纲最大联焰间距增大0.2左右,并且喷嘴间的联焰过程大致可分为四个阶段;单喷嘴的贫油熄火当量比大于任意喷嘴间距下双喷嘴的贫油熄火当量比;随着喷嘴间距的减小,贫油熄火当量比先减小后增大;另外,喷嘴间距减小导致射流合并,气流径向速度抵消变小,中心射流速度峰值增大以及回流区尺寸缩小;随着喷嘴彼此靠近,喷嘴间的方均根速度变大,分布区域变广。      

受限空间内三级旋流流场和燃烧性能研究

为研究受限空间内三级旋流器流场特征和对应的燃烧性能,对不同方案三级旋流器开展了试验和仿真研究,分析了2种典型流场（贴壁流场和锥形流场）特性及其对火焰形态、燃烧室性能指标的影响。结果表明,通过控制三级孔特征可实现三级旋流器下游贴壁流场和锥形流场之间的转变。三级孔为30°时,旋流器的高湍动能有利于强化燃油雾化,同时形成贴壁的大尺寸回流区有利于燃油在主燃区的空间扩散和均匀分布,能够改善燃烧室点熄火性能,但会导致主燃区火焰筒壁温较高。     

旋转状态下方形通道内部流场特性热线实验

为了解决旋转条件下热线技术应用问题并且在此基础上精确测量旋转方形通道内部流场特性,搭建了用于旋转通道流场测试实验平台,采用了两种连线方式对热线进行了标定实验,获得了热线测量旋转通道内部平均速度的相对误差为±6%,对雷诺数和旋转数范围分别是5000~10000和0~0.222的旋转通道流场进行了测量,结果表明:旋转导致速度型整体向后缘面（Y/D=-0.5）偏转,X/D和旋转数越大,速度型偏转越明显;旋转数为0.222时,后缘面附近边界层速度型出现了一个拐点,可能与由哥氏力不稳定性引起的二次流有关.      

弹性空腔流致噪声/结构振动特性试验

高速空腔中经常存在高强度且多频率分量的流致噪声,空腔噪声与结构振动之间耦合效应严重,甚至可能发生结构共振。为此,在0.6m×0.6m高速风洞中,通过调整空腔底板厚度,改变其结构固有频率,模拟空腔流致噪声/振动相互作用。利用脉动压力和振动加速度测试技术,获取亚跨声速条件下,弹性空腔流致噪声特性及其结构振动响应特性。马赫数变化范围为0.6~1.2。结果表明,当振动强度较弱时,结构振动对空腔噪声影响较小,而空腔噪声对结构振动影响较大,在噪声载荷主频位置,振动谱出现峰值并且噪声/振动相关性达到最强;此外,空腔结构振动还与其固有频率特性密切相关,振动主要以低阶模态为主。     

复杂几何形状喷管内外三维流场的数值模拟

研究了球面收敛矩形扩张的二元喷管（ＳＣＦＮ）流场的数值模拟,为了有效地捕获激波与滑流面及较好地模拟分离,采用了Ｒｏｅ格式、ＭＵＳＣＬ方法及Ｖｅｎｄａｔａｋｒｉｓｈｎａｎ限制器、Ｓｐａｌａｒｔ－Ａｌｌｍａｒａｓ方程紊流模型。研究中给出了两个喷管模型四个流动状态的数值模拟结果。结果表明,除了有严重分离的流动情况以外,该算法能得到相当满意的计算结果。     

外涵偏轴分开排气喷管的流场和声场数值计算

以某型涡扇发动机为原型,建立了1/10缩比的分开排气式涡扇发动机排气喷管物理模型,采用大涡模拟(LES)计算了不同外涵偏轴距离的排气喷管非稳态流场,利用FW-H(Ffows Williams-Hawkings)声学模型和傅里叶变换得到了排气喷流噪声声压级空间分布特征.计算结果表明:外涵偏轴式分开排气喷管有抑制排气喷流噪声的作用.喷流噪声整体抑制效果与偏轴距离有关,在偏轴距离为0.15D时,排气喷管下方的噪声降低达到最大,且排气噪声峰值由原型的146.7dB降低到139.5dB,降低了7.2dB.研究的排气结构和数值计算方法可作为分开排气式涡扇发动机降噪设计的参考.      

Reconstructed 3-d magnetic field structure and hard X-ray two ribbons for 2000 Bastille-day event

The Bastille-day event in 2000 produced energetic 3B/X5.6 flare with a halo CME, which had great geo-effects consequently. This event has been studied extensively and it is considered that it follows the two-ribbon flare model. The flare/CME event was triggered by an erupting filament and TRACE observations showed formation of giant arcade structures during the flare process. Hard X-ray (HXR) two ribbons revealed for the first time in this flare event (Masuda et al., 2001). The reconstruction of 3-D coronal magnetic fields revealed a magnetic flux rope structure, for the first time, from extrapolation of observed photospheric vector magnetogram data and the flux rope structure was co-spatial with portion of the filament and a UV bright lane (Yan et al., 2001a, 2001b). Here we review some recent work related to the flux rope structure and the HXR two ribbons by comparing their locations and the flux temporal profiles during the flare process so as to understand the energy release and particle accelerations. It is proposed that the rope instability may have triggered the flare event, and reconnection may occur during this process. The drifting pulsation structure in the decimetric frequency range is considered to manifest the rope ejection, or the initial phase of the coronal mass ejection. The HXR two ribbons were distributed along the flux rope and the rope foot points coincide with HXR sources. The energy dissipation from IPS observations occurred within about 100 R _⋅ is consistent with the estimate for the flux rope system. This revised version was published online in August 2006 with corrections to the Cover Date.     

锯齿尾缘叶片气动特性和绕流流场的数值研究

以基于NACA 0018翼型的锯齿尾缘仿生叶片为研究对象,采用大涡模拟的方法研究锯齿相对齿宽与相对齿高对锯齿尾缘叶片的气动特性和非定常绕流流场的影响规律和机制.研究表明,尾缘锯齿参数对叶片气动性能的影响是复杂的非线性过程,在一定来流攻角范围内能提高升阻比,但失速提前.如在9.4°~14.8°来流攻角范围内,不同相对齿宽系列叶片的升阻比高于原始叶片,升阻比与锯齿相对齿宽之间没有线性关系.研究还表明,锯齿尾缘能延迟边界层分离,加速尾迹的流动掺混和能量扩散,改变非定常涡结构和涡脱落频率.相对齿高的变化对非定常流动特性的影响更为显著.尾缘锯齿诱导的二次湍流射流和吸力面侧反向涡对改变了原始叶片的绕翼环量,进而影响锯齿尾缘叶片的气动特性和绕流流场特性.      

尖拱弹身横向喷流数值模拟

本文通过数值求解层流Navier—Stakes方程来模拟超声速流场中横向超声速喷流的干扰流场，采用分块对接网格和“O”型网格技术，精确模拟喷口截面形状并生成高质量的贴体计算网格，对尖拱弹身的横向超声速喷流的干扰流场进行了数值模拟，研究了喷口附近的流场结构、涡系结构、波系结构及流动分离等流场特性，得到喷流流场的干扰效应，计算结果与实验值吻合较好。     

多重网格技术在复杂粘性流场计算中的应用及研究

流体力学控制方程的数值求解过程中,当网格加密、粘性效应强或来流马赫数低的时候,流场收敛非常缓慢。本文在多块网格、LUSGS隐式格式基础上采用多重网格技术,计算了NLR7301case#1两段翼型的低速绕流及DLRF4跨声速流场,在复杂二维、三维粘性流场求解中获得了满意的加速收敛效果。文中还比较了V循环、W循环的加速效率,为多重网格的工程应用奠下基础。     

The effects of magnetic fields on period changes,mass transfer and evolution of algol binaries

Variations in the magnetic pressure and flux blocking by starspots during the magnetic cycle of the cool semidetached component of an Algol binary may cause cyclic changes in the quadrupole moment and moment of inertia of the star which can cause alternate period changes. Since several different processes and timescales are involved, the orbital period changes may not correlate strongly with the indicators of magnetic activity. The structural changes in the semidetached component can also modulate the mass transfer rate. Sub-Keplerian velocities, supersonic turbulence, and high temperature regions in circumstellar material around the accreting star may all be a consequence of magnetic fields embedded in the flow. Models for the evolution of Algols which include the effects of angular momentum loss (AML) through a magnetized wind may have underestimated the AML rate by basing it on results from main sequence stars. Evolved stars appear to have higher AML rates, and there may be additional AML in a wind from the accretion disk.     

The effects of magnetic fields on period changes, mass transfer and evolution of algol binaries

Variations in the magnetic pressure and flux blocking by starspots during the magnetic cycle of the cool semidetached component of an Algol binary may cause cyclic changes in the quadrupole moment and moment of inertia of the star which can cause alternate period changes. Since several different processes and timescales are involved, the orbital period changes may not correlate strongly with the indicators of magnetic activity. The structural changes in the semidetached component can also modulate the mass transfer rate. Sub-Keplerian velocities, supersonic turbulence, and high temperature regions in circumstellar material around the accreting star may all be a consequence of magnetic fields embedded in the flow. Models for the evolution of Algols which include the effects of angular momentum loss (AML) through a magnetized wind may have underestimated the AML rate by basing it on results from main sequence stars. Evolved stars appear to have higher AML rates, and there may be additional AML in a wind from the accretion disk.