基于流动控制的水下航行体流体动力特性分析

利用CFX对水下航行体流体动力特性进行了数值模拟研究.求解了混合介质的剪切压力输运湍流模型控制方程、雷诺-平均奈维尔-斯托克斯方程以及各相间的质量输运方程,采用三维数值模拟方法对比分析了不同流动控制方案的水下航行体空泡形态特征、表面压力分布和阻力系数变化特性,讨论了不同参数对减阻效果的影响.结果表明,对于有横流作用的水下垂直发射航行体,多相流动控制不仅可以降低通气空泡的不对称性和航行体阻力,同时可以均匀迎流面和背流面压力,从而实现航行体多相流空泡形态及表面压力特性等的控制.此外,通气口的位置对减阻效果具有显著影响.      

开孔变刚度层合板压缩屈曲性能研究

针对开孔变刚度层合板,建立3种尺寸的层合板有限元模型,采用了线性屈曲、引入残余热应力的线性屈曲和引入初始缺陷的非线性屈曲的3种分析方法,研究了开孔层合板在压缩条件下的屈曲行为,并通过自动铺丝制造层合板进行试验对比,对3种方法的合理性进行了分析。结果表明,引入残余热应力的线性屈曲分析方法与试验结果最吻合,两者仅相差0.63%。基于该方法,讨论开孔层合板残余热应力分布特点和应力水平,得出了开孔层合板的应力分布云图和应力分布规律,计算出残余热应力对开孔复合材料层合的屈曲影响。结果表明,残余热应力对传统直线开孔层合板的屈曲载荷影响很小,仅提高了3.57%,但大大提高了变刚度开孔层合板的屈曲载荷,最多可达23.40%。说明纤维曲线铺放可以改变内部残余热应力的分布,提高整个开孔层合板承载压缩载荷的能力。     

扩展型面排孔气膜冷却的实验研究

本文设计了三种型面的气膜孔扩展结构,研究了气膜冷却效率、壁面换热系数及流量系数随吹风比的变化规律。研究结果表明,与典型的圆柱形气膜孔相比,有后向扩展型面的气膜孔具有相对较高的冷却效率和换热系数,流量系数略有降低。扩展型面的流向扩展角α对冷却效率和换热系数的影响大于侧向扩展角 的影响。侧向扩展角 只在特定吹风比下才对提高气膜的侧向覆盖率、进而提高气膜冷却效率起作用,它使得位于二次流出流下游的低压区域范围增大,流量系数减小。     

A Parallel Adaptive 3D MHD Scheme for Modeling Coronal and Solar Wind Plasma Flows

A parallel adaptive mesh refinement (AMR) scheme is described for solving the governing equations of ideal magnetohydrodynamics (MHD) in three space dimensions. This solution algorithm makes use of modern finite-volume numerical methodology to provide a combination of high solution accuracy and computational robustness. Efficient and scalable implementations of the method have been developed for massively parallel computer architectures and high performance achieved. Numerical results are discussed for a simplified model of the initiation and evolution of coronal mass ejections (CMEs) in the inner heliosphere. The results demonstrate the potential of this numerical tool for enhancing our understanding of coronal and solar wind plasma processes. This revised version was published online in June 2006 with corrections to the Cover Date.     

Experimental investigation and correlation development of jet impingement heat transfer with two rows of aligned jet holes on an internal surface of a wing leading edge

Extensive experimental studies on the heat transfer characteristics of two rows of aligned jet holes impinging on a concave surface in a wing leading edge were conducted, where50000 Rej 90000, 1.74 H/d 27.5, 66° a 90°, and 13.2 r/d 42.03. The finding was that the heat transfer performance at the jet-impingement stagnation point with two rows of aligned jet holes was the same as that with a single row of jet holes or the middle row of three-row configurations when the circumferential angle of the two jet holes was larger than 30°. The attenuation coefficient distribution of the jet impingement heat transfer in the chordwise direction was so complicated that two zones were divided for a better analysis. It indicated that: the attenuation coefficient curve in the jet impingement zone exhibited an approximate upside-down bell shape with double peaks and a single valley; the attenuation coefficient curve in the non-jet impingement zone was like a half-bell shape, which was similar to that with three rows of aligned jet holes; the factors,including Rej, H/d and r/d, affected the attenuation coefficient value at the valley significantly.When r/d was increased from 30.75 to 42.03, the attenuation rates of attenuation coefficient increased only by 1.8%. Consequently, experimental data-based correlation equations of the Nusselt number for the heat transfer at the jet-impingement stagnation point and the distributionof the attenuation coefficient in the chordwise direction were acquired, which play an important role in designing the wing leading edge anti-icing system with two rows of aligned jet holes.     

不锈钢管板小群孔加工技术

分析了不锈钢管板加工的难点,介绍了机床和钻头的选择及优化切削参数,获得较好的技术经济效果.     

Large-scale Coronal Heating, Clustering of Coronal Bright Points, and Concentration of Magnetic Flux

By combining quiet-region Fe XII coronal images from SOHO/EIT with magnetograms from NSO/Kitt Peak and from SOHO/MDI, we show that the population of network coronal bright points and the magnetic flux content of the network are both markedly greater under the bright half of the large-scale quiet corona than under the dim half. These results (1) support the view that the heating of the entire corona in quiet regions and coronal holes is driven by fine-scale magnetic activity (microflares, explosive events, spicules) seated low in the magnetic network, and (2) suggest that this large-scale modulation of the magnetic flux and coronal heating is a signature of giant convection cells. This revised version was published online in June 2006 with corrections to the Cover Date.     

跨声速风洞斜孔壁非线性流动试验

为分析跨声速风洞斜孔壁近壁区域的流动特性，评估气流偏角-压力系数的非线性关联，在0.6 m跨超声速风洞中开展了基于七孔探针的流动特性测量试验。通过气流偏角和压力系数分布分析了斜孔壁流动的差阻特性，以及马赫数、模型升力对斜孔壁流动的影响，最后基于试验结果发展了计算斜孔壁特性参数的微分法，并与经验方法结果进行对比。结果表明，斜孔壁流动呈现出明显的差阻性和非线性，在负压差范围内，近壁流动仍以出流为主；高亚声速时，空风洞模型区孔壁流动特性趋于实壁；安装模型后，随着升力的增大，升力面对应的孔壁区域流动向入流发展，孔壁流动特性趋于开口边界。     

The Evolving Sigmoid: Evidence for Magnetic Flux Ropes in the Corona Before, During, and After CMES

It is generally accepted that the energy that drives coronal mass ejections (CMEs) is magnetic in origin. Sheared and twisted coronal fields can store free magnetic energy which ultimately is released in the CME. We explore the possibility of the specific magnetic configuration of a magnetic flux rope of field lines that twist about an axial field line. The flux rope model predicts coronal observables, including heating along forward or inverse S-shaped, or sigmoid, topological surfaces. Therefore, studying the observed evolution of such sigmoids prior to, during, and after the CME gives us crucial insight into the physics of coronal storage and release of magnetic energy. In particular, we consider (1) soft-X-ray sigmoids, both transient and persistent; (2) The formation of a current sheet and cusp-shaped post-flare loops below the CME; (3) Reappearance of sigmoids after CMEs; (4) Partially erupting filaments; (5) Magnetic cloud observations of filament material.     

Indicators of black-hole mass and Eddington accretion ratio from QSO X-ray and UV spectra

The evolution of luminous QSOs is linked to the evolution of massive galaxies. We know this because the relic black-holes found locally have masses dependent on the properties of the host galaxy’s bulge. An important way to explore this evolution would be to measure dependences of black-hole masses and Eddington accretion ratios over a range of redshifts, i.e., with cosmological age. For low redshift QSOs (and their lower luminosity Seyfert galaxy counterparts) it has been possible to infer black-hole masses from the luminosities and velocity dispersions of their host-galaxy bulges. These masses agree with those virial black-hole masses calculated from the Doppler widths of the broad Hβ emission lines. The latter method can then be extended to more distant and luminous QSOs, up to redshifts of 0.6 with ground-based optical observations. We discuss ways to extend these explorations to higher redshifts – up to 3 using the widths of QSOs’ broad UV emission lines, and in principle, and to redshifts near 4 from ground-based infrared observations of rest-frame Hβ at 2.5 μm. We discuss the possibility of investigating the accretion history of the higher redshift QSOs using measures of Eddington accretion ratio – the soft X-ray spectral index and the eigenvectors of Principal Components Analyses of QSOs’ UV emission-line spectra.