浅凹槽底壁横向燃料喷射对流动和燃烧特性的影响

模拟了高度30km,飞行马赫数6的超声速燃烧室流场和燃烧特性.通过对固定长度、不同深度的一组浅凹槽底壁燃料横向喷射的燃烧室的冷态与燃烧工况进行数值计算,并将其和传统壁面横向喷射方式进行比较,发现引入浅凹槽底壁喷射结构能有效减弱流场的激波系强度,明显降低燃烧流场的总压损失;凹槽前壁面和喷流柱之间形成稳定的亚声速回流区,能够稳定火焰,这在较大深度凹槽会更明显.引入浅凹槽一定程度降低了横向射流穿透深度,这也导致燃烧效率相比传统壁面横向喷射结构有一定下降.     

Integration and calibration of a multi slit spectropolarimeter

Multi-slit spectropolarimeter is a next-generation spectropolarimeter to obtain vector magnetic field information at high spatial, spectral, and temporal resolution for studying the magnetic structures on the Sun. Once developed, it can be used as ground based instrument at solar observatories, also as a space payload for various solar missions. A high spectral resolution is invariably an important parameter for accurate vector magnetic field measurements and faster cadence is required for the study of dynamical evolution of structures (e.g., solar flares, sunspots etc.) on the Sun and hence better understanding on the physics behind their evolution.     

双管爆轰单引射增推机理的数值研究

基于二维Euler方程,结合高精度Roe/HLL(Harten-Lax-Van Leer)混合格式与自适应网格加密技术,对引射模态下的双管爆轰非定常单次引射复杂流场进行了数值模拟.结果分别描述了方管爆轰波喷出及引射管内二次爆轰波的传播过程.双爆轰波喷出爆轰管后,以欠膨胀射流形式向外传播,同时,它们相互作用延长了引射管尾...     

环形脉冲爆震发动机引射性能

采用解析方法得出爆震波在爆震管内的参数分布,应用数值方法对爆震波衰退为激波后的传播、排除过程进行了多循环模拟.通过对环形爆震管非稳态引射过程的分析,得出非稳态引射过程可以分成四个阶段,环形爆震管比传统的圆形爆震管的引射作用更强.不同结构参数的引射喷管对环形爆震管的引射增推性能不同,经过分析,得到了较佳的引射喷管的入口尺...     

The Role of Magnetic Reconnection in CME Acceleration

Observations carried out from the coronagraphs on board space missions (LASCO/SOHO, Solar Maximum and Skylab) and ground-based facilities (HAO/Mauna Loa Observatory) show that coronal mass ejections (CMEs) can be classified into two classes based on their kinematics evolution. These two classes of CMEs are so-called fast and slow CMEs. The fast CME starts with a high initial speed that remains more or less constant; it is also called the constant-speed CME. On the other hand, the slow CME starts with a low initial speed, but shows a gradual acceleration; it is also called the accelerated and slow CME. Low and Zhang [Astrophys. J. 564, L53–L56, 2002] suggested that these two classes of CMEs could be a result of a difference in the initial topology of the magnetic fields associated with the underlying quiescent prominences. A normal prominence magnetic field topology will lead to a fast CME, while an inverse quiescent prominence results in a slow CME, because of the nature of the magnetic reconnection processes. In a recent study given by Wu et al. [Solar Phys. 225, 157–175, 2004], it was shown that an inverse quiescent prominence magnetic topology also could produce a fast CME. In this study, we perform a numerical MHD simulation for CMEs occurring in both normal and inverse quiescent prominence magnetic topology. This study demonstrates three major physical processes responsible for destabilization of these two types of prominence magnetic field topologies that can launch CMEs. These three initiation processes are identical to those used by Wu et al. [Solar Phys. 225, 157–175, 2004]. The simulations show that both fast and slow CMEs can be initiated from these two different types of magnetic topologies. However, the normal quiescent prominence magnetic topology does show the possibility for launching a reconnection island (or secondary O-line) that might be thought of as a “CME’’.     

β Cep stars from a spectroscopic point of view

In this review we present the current status of line-profile-variation studies of β Cep stars. Such studies have been performed for 26 bright members of this class of pulsating stars in the past 25 years. We describe all these currently available data and summarize the interpretations based on them in terms of the excited pulsation modes. We emphasize that line-profile variations offer a much more detailed picture of the pulsational behaviour of pulsating stars compared to ground-based photometric data. The latter, however, remain necessary to unravel the often complex frequency pattern and to achieve unambiguous mode identification for multiperiodic β Cep stars and also to derive the pulsational properties of the faint members of the class. We highlight the statistical properties of the sample of 26 stars for which accurate spectroscopic studies are available and point out some future prospects. This revised version was published online in June 2006 with corrections to the Cover Date.     

材料特性对热障涂层合理压入深度的影响

基于有限元计算方法和量纲分析原理提出了热障涂层合理压入深度的确定方法,并研究了涂层及基体材料特性对合理压入深度的影响.首先,根据量纲分析原理提出了合理压入深度的无量纲表达式;其次基于锥形压头识别理想弹塑性材料的材料特性的方法,提出合理压入深度的确定方法;最后研究了各无量纲因素对合理压入深度的影响.研究发现基体的弹性模量对合理压入深度的影响最大,粘结层材料特性的影响较大,热氧化生成层的材料特性及基体的屈服极限对合理压入深度的影响不大.     

高速弹射试验机操稳性能的计算与试飞

本文介绍了为研究高速弹射试验机的操稳性能和在弹射力扰动下飞机的动态响应,把弹射力以瞬态脉冲载荷的形式作用于飞机时所建立的数学模型和采用的计算方法.把计算结果与试飞结果和原型机试飞结果作了比较,计算结果与试飞结果的一致性是令人满意的。这为高速弹射试验机的安全飞行和指导飞行员实施弹射试验提供了可靠的依据。     

Numerical investigation on flow and heat transfer characteristics of supercritical RP-3 in inclined pipe

Numerical simulations of flow and heat transfer to supercritical RP-3 through the inclined tubes have been performed using LS k–e model embedded in Fluent. The physical properties of RP-3 were obtained using the generalized corresponding state laws based on the fourcomponent surrogate model. Mass flow rate is 0.3 g/s, system pressure is 3 MPa, inlet temperature is 373 K. Inclination of the inclined pipe varied from -90° to 90°, with heat flux varied from 300 k W/m~2 to 400 kW/m~2. Comparison between the calculated result and the experimental data indicates the range of error reasonable. The results of ±45° show that temperature inhomogeneity in inclined pipe produce the secondary flow in its cross section due to the buoyancy force. Depending on the strength of the temperature inhomogeneity, there will be two different forms of secondary flow and both contribute to the convective heat transfer in the pipe. The secondary flow intensity decreases when the inhomogeneity alleviates and thermal acceleration will play a leading role. It will have a greater impact on the turbulent flow to affect the convective heat transfer in the pipe. When changing the inclination, it affects the magnitude of the buoyant component in flow direction. The angle increases, the buoyancy component decreases. And the peak temperature of wall dominated by the secondary flow will move forward and increase in height.