先进旋涡燃烧室多场协同分析

为了对先进旋涡燃烧室(AVC)的流动和传热性能进行综合评价,对不同来流速度、来流温度、壁面温度下AVC燃烧性能进行了数值模拟,对速度场、温度场、压力场进行了多场协同分析。结果表明:随着燃烧室来流速度的增大,速度与速度梯度的协同角α、速度与温度梯度的协同角β,速度与压力梯度的协同角θ均减小,温度梯度与速度梯度的协同角γ及压力梯度与速度梯度的协同角φ增大。随着来流温度的提高,α,θ增大,β,γ,φ减小。随着壁面温度的提高,α,θ减小,β,γ,φ增大。对于AVC湍流流场的传热强化问题,增大来流速度和来流温度,降低壁面温度会强化流动换热;增大来流速度和壁面温度,降低来流温度可以减少传热功耗;增大来流速度和壁面温度,降低来流温度能够提高强化传热的综合性能。     

驻涡燃烧室驻涡区涡系特点数值模拟

为深入了解驻涡燃烧室凹腔内流场的涡系分布特性,采用FLUENT对不同驻涡区前进口堵塞比和不同燃烧室入口速度的驻涡区流场进行计算,分析典型截面压力场和流线图,研究驻涡区涡系特点.结果表明:不同纵截面旋涡特点不同,主流被联焰板堵塞的凹腔纵截面只有主涡,为稳定点火和火焰稳定提供条件;不同横截面的旋涡差别较大,离驻涡区前壁越远的截面涡心距越大,贴近前壁和后壁的截面均无旋涡;燃烧室入口速度对轴向中间截面的旋涡结构无影响,而前进口堵塞比对旋涡结构影响较大.     

钝体改进结构对先进旋涡燃烧室燃烧流动特性影响

为探究先进旋涡燃烧室凹腔稳焰机制,提出了一种后钝体结构改进方案,并对改进后的燃烧室燃烧特性进行了预混和非预混燃烧数值模拟.结果表明:预混燃烧条件下,当量比为0.6和1.0时,钝体改进结构可有效增强凹腔内旋涡流动强度,增加凹腔内温度,同时使温度分布更加均匀.另外,凹腔内温度随预混进气速度增加而增加,且当速度增大到一定值时,温度变化不明显;非预混燃烧条件下,钝体改进结构可改善凹腔内旋涡流动及温度分布,在贫油燃烧状态时,凹腔内仍可维持较高的温度;钝体改进使燃烧室质量更小,具有一定的工程参考意义.     

紧凑喷射下钝体回流区内当量比影响因素数值研究

针对先进加力燃烧室火焰稳定器采用的紧凑喷射模式,以包含一个钝体稳定器的矩形模型件为研究对象,数值研究了加力条件下来流温度和速度以及喷口直径、喷射距离、钝体宽度对钝体稳定器后回流区局部当量比的影响。结果表明:提高来流温度、速度,扩大喷口直径,增加喷射距离或槽宽,都会增大钝体回流区内的当量比。最后,利用获得的数据建立了简单拟合函数,以预估紧凑喷射模式下回流区内的局部当量比。     

驻涡燃烧室最佳中心驻体宽度选择的数值研究

为确定驻涡燃烧室中心驻体最佳宽度,在四种来流条件下,对当量宽度为0.3～0.8范围,间隔为0.05当量宽度的中心驻体驻涡燃烧室三维黏性流场进行了冷态数值模拟.计算结果表明,当量宽度在0.65～0.70的中心驻体有利于在驻涡腔内形成低速且稳定的流动.驻体宽度增加会导致驻涡腔外侧主流气流速度提高,引起摩擦损失的加大,燃烧室出口截面处的总压损失增加.      

超燃冲压发动机燃烧室出口温度场分布CARS测量

针对超燃冲压发动机研究中对燃烧室出口温度场的测量需求以及暂冲式超燃冲压发动机燃烧台架试验中的应用难点,开发了适用于瞬态燃烧场温度测量的单脉冲相干反斯托克斯拉曼反射（CARS）系统及CARS光谱计算和温度反演软件CARSCF。采用USED相位匹配方式来降低湍流影响,结合多尺度小波分析方法来实现CARS光谱降噪处理,提高信噪比。在暂冲式脉冲燃烧风洞上开展了来流马赫数2.6条件下超燃冲压发动机燃烧室出口温度测量试验,获取了超声速来流（冷态）建立、H₂点火加热空气、建立超声速燃烧流场直至试验结束过程中的燃烧室出口温度,以及煤油/空气燃烧时燃烧室出口温度场分布。结果显示,超声速冷流时温度处于低温（约205K）状态,随着H₂点火加热来流空气,来流温度上升至853K;随着煤油/Air点火,温度急剧上升,稳定燃烧状态下燃烧流场温度为1970K±144K。燃烧室出口截面温度场分布测量结果显示,高温区位于燃烧室出口截面上侧区域,而燃烧室出口截面上中间区域的温度低于上下两侧。燃烧室出口温度分布CARS测量结果与火焰自发光成像结果一致,表明单脉冲CARS技术用于瞬态燃烧流场温度测量的可行性。     

基于支板凹腔结构的超燃燃烧室数值研究

为探究基于支板凹腔结构的超燃燃烧室性能,在超声速来流条件下,采用带中心支板且凹腔长高比为7.5的三维超燃燃烧室模型,针对支板阻塞比、扩张段扩张角、不同燃料喷射方式以及不同燃料当量比对燃烧室相关性能的影响进行了数值研究。研究发现:支板阻塞比会对隔离段内的激波分布以及支板后缘速度分布产生明显影响,而扩张段扩张角会影响超声气流在燃烧室出口的膨胀状态;采用壁面以及中心喷注支板同时喷油方式在保持高燃烧效率的同时会扩大整个燃烧室的燃烧区域;当采用单独壁面喷油方式时,凹腔内静温分布会随着当量比的变化发生相应的改变,同时会在当量比为0.51~0.74时达到相对较高的燃烧效率。     

环形先进旋涡燃烧室流动、燃烧和污染物排放特性

为了给先进旋涡燃烧技术实际应用提供理论依据,采用实验和数值模拟相结合方法,对环形先进旋涡燃烧室流动和燃烧特性开展研究。首先采用粒子图像测速技术,对三对钝体布置先进旋涡燃烧室,进行冷态流动特性实验。在此基础上,对燃氢螺旋布置18对钝体的环形先进旋涡燃烧室的燃烧特性,开展了数值模拟。结果表明:(1)有后钝体存在,可以抑制气流在前钝体后面形成旋涡脱落,从而减小了流通气流的流动阻力;(2)在凹腔喷射气流的作用下,相对于无喷射条件下凹腔内形成的旋涡结构拉长,而且占据了整个凹腔;(3)随着主气流当量比增加,流经环形AVC气流在前、后钝体间的凹腔内的旋涡结构更加趋于对称,出口平均温度、燃烧效率、NOx质量分数和总压损失系数也增大,出口温度分布系数减小。(4)喷射角在45°范围内,随着喷射角的增加,燃烧效率和出口平均温度增加,NOx质量分数、总压损失系数和出口温度分布系数减小。     

超燃冲压发动机燃烧室的准一维计算与分析

在考虑有限速率化学反应的准一维Euler方程基础上,通过增加截面面积变化、壁面摩擦和添质的源项,发展了适用于超燃燃烧室性能分析的准一维计算方法。依次以中国空气动力研究与发展中心(CARDC)和日本国家航空与航天实验室(NAL)的氢燃料燃烧室模型作为验证算例,分别采用传统的一步反应模型和发展的有限速率反应模型,模拟了燃烧室流场,并基于NAL燃烧室,计算分析了不同当量比和进口压强对燃烧室流动特性的影响。结果表明:两种方法都能得到与实验数据吻合良好的结果;和一步反应模型相比,有限速率反应模型不仅可以更细致地捕捉流场细节,而且能够初步分析化学非平衡效应的影响;对于NAL燃烧室,当量比≥0.6时,压强随当量比的升高而增大,当达到1.0时,反压已推进隔离段,且推进速度随当量比增大而增加;进口压强不大于110.444kPa时,反压随进口压强增大而升高,且当反压不小于82.833kPa时,反压被隔离在等直段燃烧室入口处;过小的当量比和过大的进口压强均会导致燃烧室出口马赫数严重下降,甚至出现亚声速出流状态。     

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。      

Cross Field Diffusion of Cosmic Rays in a Two-Dimensional Magnetic Field Turbulence

Cross field diffusion of energetic particles (cosmic rays) in a two-dimensional static magnetic field turbulence is studied performing test particle simulations. Qualitatively different diffusion processes are observed depending on the ratio of Larmor radius (ρ) to the correlation length (λ) of the magnetic field fluctuations. The diffusion is found to be composed of several regimes with distinct statistical properties, which can be characterized using Levy statistics. This revised version was published online in August 2006 with corrections to the Cover Date.     

液滴喷射过程流场和温度场的数值模拟

 建立了液滴喷射过程流场和温度场的计算模型，研究了在外加周期性正弦扰动作用下，石蜡液滴形成过程的流场和温度场及其变化情况，给出了不同扰动频率下所形成液滴的形态及其变化规律，得出了比较均匀的液滴流，指出扰动频率对液滴的形成及其均匀性具有重要影响。模拟结果与文献中的实验结果吻合较好。     

提高旋转式电场仪测量电场特性的方法研究

在介绍旋转式电场仪测量电场强度的机理及测量系统构成的基础上,针对在特高压直流输电线路下地面合成电场测量中,各电场仪的输出电压与被测电场强度的特性曲线不一致,外场较恶劣测量环境对测量结果造成干扰影响测量准确度等问题,提出了相应的解决方法（特性曲线归一化处理和双路消噪差动测量法）。所述方法便于用户现场使用,提高了旋转式电场仪抗干扰能力和测量准确度。     

Millennial Variations of the Geomagnetic Field: from Data Recovery to Field Reconstruction

Variations of the geomagnetic field over past millennia can be determined from archeomagnetic data and paleomagnetic sediment records. The resolution and validity of any field reconstruction depends on the reliability of such indirect measurements of past field values. Considerable effort is invested to ensure that the magnetic minerals carrying the ancient magnetization are good, if not ideal, recorders of the magnetic field. This is achieved by performing a wide array of rock magnetic and microscopy investigations, many of which are outlined here. In addition to data quality, the spatial and temporal distributions of archeomagnetic and sediment records play a significant role in the accuracy of past field reconstruction. Global field reconstructions enable studies of dynamic processes in Earth’s core. They rely on data compilations which ideally include information about the quality of a measurement and provide a useful archive for selecting data with the best characteristics. There is, however, a trade off between the total number of reliable data and the geographic or temporal coverage. In this review we describe the various types of paleomagnetic recorders, and the kind of measurements that are performed to gather reliable geomagnetic field information. We show which modeling strategies are most suitable, and the main features of the field that can be derived from the resulting models. Finally, we discuss prospects for progress in this kind of research.     

The Cassini Magnetic Field Investigation

The dual technique magnetometer system onboard the Cassini orbiter is described. This instrument consists of vector helium and fluxgate magnetometers with the capability to operate the helium device in a scalar mode. This special mode is used near the planet in order to determine with very high accuracy the interior field of the planet. The orbital mission will lead to a detailed understanding of the Saturn/Titan system including measurements of the planetary magnetosphere, and the interactions of Saturn with the solar wind, of Titan with its environments, and of the icy satellites within the magnetosphere.This revised version was published online in July 2005 with a corrected cover date.     

The Juno Magnetic Field Investigation

The Juno Magnetic Field investigation (MAG) characterizes Jupiter’s planetary magnetic field and magnetosphere, providing the first globally distributed and proximate measurements of the magnetic field of Jupiter. The magnetic field instrumentation consists of two independent magnetometer sensor suites, each consisting of a tri-axial Fluxgate Magnetometer (FGM) sensor and a pair of co-located imaging sensors mounted on an ultra-stable optical bench. The imaging system sensors are part of a subsystem that provides accurate attitude information (to ～20 arcsec on a spinning spacecraft) near the point of measurement of the magnetic field. The two sensor suites are accommodated at 10 and 12 m from the body of the spacecraft on a 4 m long magnetometer boom affixed to the outer end of one of ’s three solar array assemblies. The magnetometer sensors are controlled by independent and functionally identical electronics boards within the magnetometer electronics package mounted inside Juno’s massive radiation shielded vault. The imaging sensors are controlled by a fully hardware redundant electronics package also mounted within the radiation vault. Each magnetometer sensor measures the vector magnetic field with 100 ppm absolute vector accuracy over a wide dynamic range (to 16 Gauss = \(1.6 \times 10^{6}\mbox{ nT}\) per axis) with a resolution of ～0.05 nT in the most sensitive dynamic range (±1600 nT per axis). Both magnetometers sample the magnetic field simultaneously at an intrinsic sample rate of 64 vector samples per second. The magnetic field instrumentation may be reconfigured in flight to meet unanticipated needs and is fully hardware redundant. The attitude determination system compares images with an on-board star catalog to provide attitude solutions (quaternions) at a rate of up to 4 solutions per second, and may be configured to acquire images of selected targets for science and engineering analysis. The system tracks and catalogs objects that pass through the imager field of view and also provides a continuous record of radiation exposure. A spacecraft magnetic control program was implemented to provide a magnetically clean environment for the magnetic sensors, and residual spacecraft fields and/or sensor offsets are monitored in flight taking advantage of Juno’s spin (nominally 2 rpm) to separate environmental fields from those that rotate with the spacecraft.     

The Magnetic Field of Mercury

The magnetic field strength of Mercury at the planet’s surface is approximately 1% that of Earth’s surface field. This comparatively low field strength presents a number of challenges, both theoretically to understand how it is generated and observationally to distinguish the internal field from that due to the solar wind interaction. Conversely, the small field also means that Mercury offers an important opportunity to advance our understanding both of planetary magnetic field generation and magnetosphere-solar wind interactions. The observations from the Mariner 10 magnetometer in 1974 and 1975, and the MESSENGER Magnetometer and plasma instruments during the probe’s first two flybys of Mercury on 14 January and 6 October 2008, provide the basis for our current knowledge of the internal field. The external field arising from the interaction of the magnetosphere with the solar wind is more prominent near Mercury than for any other magnetized planet in the Solar System, and particular attention is therefore paid to indications in the observations of deficiencies in our understanding of the external field. The second MESSENGER flyby occurred over the opposite hemisphere from the other flybys, and these newest data constrain the tilt of the planetary moment from the planet’s spin axis to be less than 5°. Considered as a dipole field, the moment is in the range 240 to 270 nT-R _M ³ , where R _M is Mercury’s radius. Multipole solutions for the planetary field yield a smaller dipole term, 180 to 220 nT-R _M ³ , and higher-order terms that together yield an equatorial surface field from 250 to 290 nT. From the spatial distribution of the fit residuals, the equatorial data are seen to reflect a weaker northward field and a strongly radial field, neither of which can be explained by a centered-dipole matched to the field measured near the pole by Mariner 10. This disparity is a major factor controlling the higher-order terms in the multipole solutions. The residuals are not largest close to the planet, and when considered in magnetospheric coordinates the residuals indicate the presence of a cross-tail current extending to within 0.5R _M altitude on the nightside. A near-tail current with a density of 0.1 μA/m² could account for the low field intensities recorded near the equator. In addition, the MESSENGER flybys include the first plasma observations from Mercury and demonstrate that solar wind plasma is present at low altitudes, below 500 km. Although we can be confident in the dipole-only moment estimates, the data in hand remain subject to ambiguities for distinguishing internal from external contributions. The anticipated observations from orbit at Mercury, first from MESSENGER beginning in March 2011 and later from the dual-spacecraft BepiColombo mission, will be essential to elucidate the higher-order structure in the magnetic field of Mercury that will reveal the telltale signatures of the physics responsible for its generation.     

多级会切磁场等离子体推力器研究进展

多级会切磁场等离子体推力器是一种电推进装置。在对此类推力器的基本概念、性能优势进行总结的基础上,系统性地回顾了国内外各研究机构不同功率级推力器的发展历程,并介绍了推力器离子加速及电子传导相关物理机制的研究过程。历经21年的发展,多级会切磁场等离子体推力器表现出显著的性能优势,在未来航天推进领域表现出了巨大的发展潜力。德国泰雷兹形成了以HEMP3050推力器为代表的工程化应用产品。我国微观物理机制的研究提升了推力器的认知水平,不同功率级推力器的研究均取得突破性进展,为推力器未来的快速发展奠定了基础。