FY-1C/D极轨气象卫星空间粒子成分监测器及其在轨探测结果

介绍了风云一号(FY-1)C，D极轨气象卫星空间粒子成分监测器的任务目标、主要功能和工程指标。以及数据的获取和处理方法。给出了空间环境宁静期、地磁扰动事件、太阳质子事件、与太阳活动的关系和粒子长期变化等探测结果，并进行了相应的分析。对C，D星空间粒子成分监测器分别进行的5年和第二次在轨测试结果表明，两星监测器工作正常、性能稳定，探测数据可靠。     

水反应金属燃料发动机比冲性能与燃烧室长度设计理论研究

运用热力计算原理,计算并分析了两相流影响条件下水反应金属燃料发动机的比冲性能。采用经验公式,对发动机中金属颗粒燃烧时间进行了计算分析,估算了金属颗粒燃烧长度,为燃烧室长度设计提供了依据。结果表明,存在最佳水燃比,使发动机达到最优比冲性能;两相流影响下比冲损失较大,金属颗粒燃烧时间随水燃比、雷诺数增加而显著减少;通过对颗粒燃烧时间的计算,可初步设计燃烧室长度。     

超音速喷流DPIV瞬时速度场实验测量

介绍了采用数字式互相关粒子图像测速系统(DPIV)在测量超音速喷流实验中的应用;实验给出了设计马赫数Ma=1.5的小型拉瓦尔喷管在不同总压和反压比条件下,喷流速度场、流线、涡量分布等定量信息.实验结果显示出流场中激波前后流体速度,涡量分布的明显变化,波系的结构和不同于一维管流的流动特性.     

实用化图像式油液污染实时检测系统研究

针对油液实时分析的应用需求,分析了基于显微图像的全采样式油液分析系统的各种特征参数,提出了系统改进的若干关键措施,建立了基于分流采样原理的实用化油液污染分析系统。同时根据实用化系统的特点,提出了结合图像运动特征和自动阈值选取的颗粒识别方法,分析了流场速度分布,解决了污染度计算的问题,并进行了与传统仪器的对比实验,获得较好的效果。     

X-ray measurements of the dark matter distribution in clusters of galaxies with Chandra

We investigate the dark matter distributions in the central region of two clusters of galaxies (A1835 and MKW3S) using Chandra data. N-body simulations in the standard cold dark matter (CDM) model predict the dark matter distribution shows a cuspy dark matter profile: ρ(r) ∝ r, with in the range 1–2, while observations of dwarf and low surface brightness galaxies seem to favor the presence of a relatively flat core: 0 <  < 1. To investigate the dark matter distributions in the central region of clusters of galaxies, we analyze the Chandra data of A1835 and MKW3S with a deprojection method. We derive the mass profiles without the assumption of analytical models. We examine the inner slope of derived mass profiles assuming the dark matter profile is described with a power-law expression. The values of the slope are 0.95 ± 0.10 for A1835 and 1.33 ± 0.12 for MKW3S within the radius of 200 kpc. These are consistent with the result of the CDM simulations. However, within the radius of 100 kpc, the value of is less than unity for A1835 (0.47 ± 0.31). Our result implies that the central dark matter profile of some clusters cannot be described by CDM halos.     

Studying the evolution of the hot universe with the X-ray evolving universe spectroscopy mission – XEUS

Europe is one of the major partners building the International Space Station (ISS) and European industry, together with ESA, is responsible for many station components including the Columbus Orbital Facility, the Automated Transport Vehicle, two connecting modules and the European Robotic Arm. Together with this impressive list of contributions there is a strong desire within the ESA Member States to benefit from this investment by utilizing the unique capabilities of the ISS to perform world-class science. XEUS is one of the astronomical applications being studied by ESA to utilize the capabilities of the ISS. XEUS will be a long-term X-ray observatory with an initial mirror area of 6 m² at 1 keV that will be expanded to 30 m² following a visit to the ISS. The 1 keV spatial resolution is expected to be 2–5″ half-energy-width. XEUS will consist of separate detector and mirror spacecraft (MSC) aligned by active control to provide a focal length of 50 m. A new detector spacecraft, complete with the next generation of instruments, will also be added after visiting the ISS. The limiting 0.1–2.5 keV sensitivity will then be 4 × 10⁻¹⁸ erg cm⁻² s⁻¹, around 200 times better than XMM-Newton, allowing XEUS to study the properties of the hot baryons and dark matter at high redshift.     

Ion relaxation processes in the heliospheric interface: how perturbed are ion distribution functions?

Charge-exchange processes between interstellar H-/O-atoms and protons of the bulk of the interstellar plasma flow downstream of the outer bowshock in the heliospheric interface induce secondary ions leading to non-relaxated velocity distribution functions. The relaxation of these freshly induced ions towards an equilibrium distribution occurs due to Coulomb interactions and wave–particle interactions with the background turbulence. Since Coulomb interactions are of low relevance, we study here in detail the effect of wave–particle interactions. To find the turbulence levels in the interface we consider the MHD-wave transformation at the outer shock surface between the interface and the local interstellar plasma. The turbulence in the outer interface region is shown to be dominated by incompressible Alfvén waves both for cases of quasiparallel and quasiperpendicular shocks. Also we show that waves propagating towards the shock are more intensive than those propagating away from it. The level of Alfvén turbulence in the interface is estimated using the recent data on local interstellar turbulence deduced from observations of interstellar scintillations of distant radiosources. Two proton relaxation processes are considered: quasilinear resonant interactions with Alfvén waves and non-linear self-induced wave–particle scattering. The corresponding diffusion coefficients are estimated, and typical time periods for protons and oxygen ions relaxation are shown to be of the same order of magnitude as H-/O-atoms passage time over the extent of the interface. This indicates that perturbed ion distribution functions must be expected there.     

旋转雾场粒子分布的全息测量

介绍了用高斯光束照射光栅而形成的衍射光场照明粒子场的同轴全息方法可以有效地测量旋转流雾化场横截面上的ＳＭＤ分布。文中描述了照明光场的特点；简要地讨论了低噪声，无孪生象的原因；介绍了全息图的显示和判读系统。完成了对１９个喷嘴、７６个截面、１６００多个采样点的测量。为密度较高的粒子场提供了有实用价值的测量结果。最后给出了Ｎｏ．１号喷嘴四个截面上ＳＭＤ分布曲线     

纳米二氧化钛吸入对小鼠肺部和血清生化指标的影响

将成年健康的小鼠(每组8只)暴露在含有1 500 mg/m3纳米二氧化钛气溶胶密闭装置内,以暴露在空气中的小鼠作为对照,研究了纳米二氧化钛对小鼠肺部组织和血清生化指标的影响.经过不同时间的暴露后将小鼠处死,收集血样并取肺部组织进行生化指标分析和组织病理学检验.血清生化指标检测结果显示,在所有的试验组中,乳酸脱氢酶的活性均提高,丙氨酸氨基转移酶的活性和尿素氮在暴露28天组中增加,肌酐在暴露14天组和28天组中均增加,其他血清学指标未见明显异常.组织病理学检测结果显示,暴露28天的肺泡间隙有纳米粒子存在,并且肺部炎症逐渐增强.     

Estimation of the solar proton spectrum in the GLE70 event

The GLE event on December 13, 2006 as observed by network station neutron monitor data is investigated (is considered). The GLE energetic spectrum suggested for this event is estimated taking into account the primary differential spectrum of galactic cosmic rays, coupling coefficients and integral multiplicities of concrete detectors at different latitudes and levels of observation. It is noted that the additional increase of solar protons is also manifested in the ionization chamber ASK-1 data at the Yakutsk station.