Operation of a Rotary-valved Pulse Detonation Rocket Engine Utilizing Liquid-kerosene and Oxygen

The pulse detonation rocket engine (PDRE) requires periodic supply of oxidizer, fuel and purge gas. A rotary-valve assembly is fabricated to control the periodic supply in this research. Oxygen and liquid aviation kerosene are used as oxidizer and fuel respectively. An ordinary automobile spark plug, with ignition energy as low as 50 mJ, is used to initiate combustion. Steady operation of the PDRE is achieved with operating frequency ranging from 1 Hz to 10 Hz. Experimentally measured pressure is lower than theoretical value by 13% at 1 Hz and 37% at 10 Hz, and there also exists a velocity deficit at different operating frequencies. Both of these two phenomena are believed mainly due to droplet size which depends on atomization and vaporiza-tion of liquid fuel.     

旋转阀脉冲爆震发动机电控共轨式燃油系统

为提高旋转阀脉冲爆震发动机(RVPDE)燃油系统性能,增强电磁阀的高频适应性,应用汽车行业领先的共轨技术,设计满足RVPDE性能要求的共轨式燃油系统(Common Rail System of PDE,CRP),并对系统控制性能、流量特性和动态响应特性进行实验研究。研究结果表明:CRP喷射时间可控制到微秒级,所有爆震管每次喷射之间的差别可控制在5%以内,电磁阀开启、关闭的动态响应时间均在1ms以内。     

吸气式脉冲爆震发动机壁温试验

为了探索各频率下管壁温度随时间的变化趋势及爆震管外壁面的温度分布规律,对爆震室内径68mm,长2 000mm,以汽油为燃料、空气为氧化剂的吸气式脉冲爆震发动机进行试验,用热成像仪对稳定工作在10Hz,20Hz,40Hz下的管壁温度进行了监测。结果表明:同一频率下随时间的增加壁面温度增加速度减小;热平衡时壁面温度随频率的增加而增长,10Hz,20Hz,40Hz热平衡时外壁面最高温度分别在726℃,1011.5℃,1159.5℃以上;热平衡前管壁温度的增长速度随频率的增加而增加,管壁温度的增长速度跟频率约成正比;爆震室上沿着压缩波叠加至形成爆震的方向,温度在外壁面上递增分布,在爆震形成区温度最高,从爆震形成区到发动机出口处,温度在外壁面上逐渐降低;各频率下最高温度区位置基本不变,距点火位置1 350mm左右;同一轴向位置上的外壁面温度随频率的增加而增加,温度的增长幅度随频率的增加而减小。     

粉末爆轰发动机的粉末燃料供应特性研究

为研究粉末爆轰发动机的粉末燃料供应特性,通过搭建一套流化仓内气固流动状态可视化的实验系统,采用称重传感器和静态压力传感器对粉末流化质量和流化仓内部压力进行实时监测,并采用电子天平精确测量粉末流化质量,对不同预压压力下粉末流化的时间均匀性,不同活塞速度下粉末流化的空间均匀性、粉末流化的流化能力特性展开分析。结果表明：粉末爆轰发动机的最佳工作时间为流化仓的压力稳定阶段和压力保持阶段;粉末在0.4-2MPa的预压压力下,其流化的时间均匀性几乎不变,且明显优于无预压下的粉末流化;粉末流化在空间上具有一定的均匀性,但其随着活塞速度的增大而逐渐减弱;粉末爆轰发动机燃料供应系统的气固比具有一个临界值,当实际气固比处于临界值以下时,会造成粉末来不及被流化气带走从而在流化仓中进行堆积最终堵塞流化仓;而当实际气固比高于临界值时,粉末流化能力随着活塞速度的增大而增大。     

近圆低轨卫星星座相位保持方法

主要研究无轨道高度保持要求的近圆低轨卫星星座相位保持方法.首先根据轨道摄动理论，推导了考虑J2摄动和大气阻尼摄动的卫星相位漂移模型，分别给出基于固定基准星和基于虚拟基准星的相位偏差两种表达方法.在此基础上，按照星座各星轨道衰减一致和不一致两种情况，分别提出两种表示方法理论的和考虑实际控制误差的相位保持策略.通过一个walker星座仿真算例验证了两种方法的有效性.仿真结果显示，两种方法在各星轨道衰减一致和不一致两种情况均可有效完成相位维持任务，当各星轨道衰减一致时两种方法在控制次数和控制总量上无明显差异；在各星轨道衰减不一致情况下，基于固定基准星的相位保持策略更优.     

Drag and energy accommodation coefficients during sunspot maximum

Conditions appropriate to gas-surface interactions on satellite surfaces in orbit have not been successfully duplicated in the laboratory. However, measurements by pressure gauges and mass spectrometers in orbit have revealed enough of the basic physical chemistry that realistic theoretical models of the gas-surface interaction can now be used to calculate physical drag coefficients. The dependence of these drag coefficients on conditions in space can be inferred by comparing the physical drag coefficient of a satellite with a drag coefficient fitted to its observed orbital decay. This study takes advantage of recent data on spheres and attitude stabilized satellites to compare physical drag coefficients with the histories of the orbital decay of several satellites during the recent sunspot maximum. The orbital decay was obtained by fitting, in a least squares sense, the semi-major axis decay inferred from the historical two-line elements acquired by the US Space Surveillance Network. All the principal orbital perturbations were included, namely geopotential harmonics up to the 16th degree and order, third body attraction of the Moon and the Sun, direct solar radiation pressure (with eclipses), and aerodynamic drag, using the Jacchia-Bowman 2006 (JB2006) model to describe the atmospheric density. After adjusting for density model bias, a comparison of the fitted drag coefficient with the physical drag coefficient has yielded values for the energy accommodation coefficient as well as for the physical drag coefficient as a function of altitude during solar maximum conditions. The results are consistent with the altitude and solar cycle variation of atomic oxygen, which is known to be adsorbed on satellite surfaces, affecting both the energy accommodation and angular distribution of the reemitted molecules.     

分隔板形式对多爆震管间相互作用的影响分析

为研究共用喷管多爆震管间爆震流场的相互作用,以氢气和氧气混合物为例,对采用不同形式分隔板的共用喷管多爆震管间的相互作用过程进行了数值模拟,并对其性能进行了比较与分析。计算结果表明,采用斜分隔板能有效地减小多爆震管间的相互影响,并且加长分隔板长度可以进一步减小多爆震管间的相互影响,同时还可以通过控制分隔板的长度来控制折射激波到达上爆震管封闭端的时间。     

Particle acceleration and gamma rays in solar flares: Recent observations and new modeling

Experiments on SMM, GAMMA, Yohkoh, GRANAT, Compton GRO, INTEGRAL, RHESSI and CORONAS-F satellites over the past three decades have provided copious data for fundamental research relating to particle acceleration, transport and energetics of flares and to the ambient abundance of the solar corona, chromosphere and photosphere. We summarize main results of solar gamma-astronomy (including some results of several joint Russian–Chinese projects) and try to appraise critically a real contribution of those results into modern understanding of solar flares, particle acceleration at the Sun and some properties of the solar atmosphere. Recent findings based on the RHESSI, INTEGRAL and CORONAS-F measurements (source locations, spectrum peculiarities, ³He abundance etc.) are especially discussed. Some unusual features of extreme solar events (e.g., 28 October 2003 and 20 January 2005) have been found in gamma-ray production and generation of relativistic particles (solar cosmic rays, or SCR). A number of different plausible assumptions are considered concerning the details of underlying physical processes during large flares: (1) existence of a steeper distribution of surrounding medium density as compared to a standard astrophysical model (HSRA) for the solar atmosphere; (2) enhanced content of the ³He isotope; (3) formation of magnetic trap with specific properties; (4) prevailing non-uniform (e.g., fan-like) velocity (angular) distributions of secondary neutrons, etc. It is emphasized that real progress in this field may be achieved only by combination of gamma-ray data in different energy ranges with multi-wave and energetic particle observations during the same event. We especially note several promising lines for the further studies: (1) resonant acceleration of the ³He ions in the corona; (2) timing of the flare evolution by gamma-ray fluxes in energy range above 90 MeV; (3) separation of gamma-ray fluxes from different sources at/near the Sun (e.g., different acceleration sources/episodes during the same flare, contribution of energetic particles accelerated by the CME-driven shocks etc.); (4) asymmetric magnetic geometry and new magnetic topology models of the near-limb flares; (5) modeling of self-consistent time scenario of the event.     

燃烧多相流的介尺度动理学建模研究进展

基于求解Navier-Stokes方程组的传统计算流体力学已经在诸多领域取得了巨大的成功,但在航空、航天、微流控等领域也遇到了新的瓶颈与挑战。其原因分为2个方面：①物理建模层面的问题;②离散格式带来的数值精度和稳定性问题。微尺度燃烧等一系列燃烧新概念的研究表明,特征更加丰富但以前知之甚少的热力学非平衡行为蕴含着大量待开发的物理功能。物理模型合理和具备相应功能是数值仿真研究的前提;物理建模层面的问题无法通过数值精度的提高来解决。本文从物理建模与复杂物理场分析角度,介绍了非平衡燃烧系统离散玻尔兹曼建模方法（DBM）的研究进展。DBM是非平衡统计物理学粗粒化建模理论在流体力学领域的具体应用之一,是相空间描述方法在离散玻尔兹曼方程形式下的进一步发展。它选取一个视角,研究系统的一组动理学性质,因而要求描述这组性质的动理学矩在模型简化中保值;以该组动理学矩的独立分量为基,构建相空间,使用该相空间和其子空间来描述系统的非平衡行为特征;研究视角和建模精度随着研究推进而调整。借助DBM可以研究反应过程中不同自由度内能之间的不平衡和相互转换等Navier-Stokes模型无法模拟的动理学过程。在内爆和外爆过程中,几何汇聚与发散效应等效于一个"外场力",在球心处系统始终处于热力学平衡态;在冯·纽曼压强峰处,系统不是偏离平衡最远,而是在平衡态附近;在冯·纽曼峰后反应区以外,Chapmann-Jouguet理论值、Zeldovich-Neumann-Doering （ZND）理论值和DBM结果相互验证;在反应区内DBM结果与ZND结果一致;在冯·纽曼压强峰前的压缩阶段,DBM模拟结果在物理上更合理。在冲击压缩过程中,相对于其他自由度,压缩波所在自由度上的内能先增加,因而这一自由度上的内能总是朝着正向偏离其平衡态值,而横向自由度上的内能总是朝着逆向偏离其平衡态值。在二流体模型视角下,反应物和产物朝着相反的方向偏离热力学平衡态。     

燃烧室宽度对煤油旋转爆震波传播模态的影响

为研究基于煤油的旋转爆震波的传播特性,以煤油和含氧量40%的富氧空气作为燃料和氧化剂,对基于燃烧室外径均为100mm的无内柱燃烧室和燃烧室宽度分别为32,26,20mm的环形燃烧室开展了对比实验。不同氧化剂流量下,共观察到四种燃烧波模态,分别为爆燃模态、准稳定爆震模态、双波对撞模态和稳定旋转爆震模态。无内柱燃烧室中,氧化剂流量较低时无法维持旋转爆震波的稳定传播,出现爆燃模态和准稳定爆震模态;当氧化剂流量超过154g/s时,可以得到稳定旋转爆震模态,旋转爆震波峰值压力超过0.7MPa,平均传播速度为1750m/s。对于环形燃烧室,旋转爆震波的传播速度仅为1245~1465m/s,明显低于无内柱燃烧室中的传播速度。随环形燃烧室宽度减小,对应旋转爆震波模态的工况范围更窄,传播速度更慢。在本研究对应的工况范围内,增大燃烧室宽度,更有利于基于煤油的旋转爆震波的稳定传播。