Solar wind electron density and temperature over solar cycle 23: Thermal noise measurements on Wind

We present the solar wind plasma parameters obtained from the Wind spacecraft during more than nine years, encompassing almost the whole solar cycle 23. Since its launch in November 1994 Wind has frequently observed the in-ecliptic solar wind upstream of the Earth’s bow shock. The WIND/WAVES thermal noise receiver was specially designed to measure the in situ plasma thermal noise spectra, from which the electron density and temperature can be accurately determined. We present and discuss histograms of such measurements performed from 1994 to 2003. Using these large data sets, we study the density and core temperature variations with solar activity cycle and with different regimes of the solar wind. We confirm the anticorrelation of the electron density with the sunspot number, and obtain a positive correlation of the core temperature, with the sunspot number.     

弓高弦长法测量圆直径的研究

弓高弦长法测圆直径的一个重要问题，是如何选取最佳测量点。本文从误差的传递着手，严密推证了弓高及弦长测量的标准差取不同值时最佳测量点的位置。     

某减压阀静态特性分析

建立了某减压阀静态特性模型,并用实验验证了模型的正确性.通过仿真讨论了膜片有效面积、网芯不平衡面积和阀门总刚度对减压阀静态特性的影响.结果表明:阀门总刚度的影响较大,而膜片有效面积和阀芯不平衡面积的影响相对较小.     

低温等离子体放电区长度对点火起爆的影响

为了研究低温等离子体放电区长度,即放电区间隙不变,体积大小对脉冲爆震发动机点火起爆的影响,以丙烷为燃料,空气和纯氧为氧化剂,充分考虑其详细的化学反应动力学机理,将低温等离子体放电区等效为高温高压火核,对放电区长度为20,40,60mm三种结构,利用Fluent软件,对点火起爆过程进行数值模拟,并进行对比分析.结果表明:将低温等离子体放电区等效为高温高压火核是可行的,能够得到完整的点火起爆过程;不同放电区长度,对初始火焰形成、火焰传播速度和缓燃转爆震(DDT)时间有很大影响,对爆震波峰值压力影响不大.      

旋流杯套筒混合段长度对点火特性的影响

为研究旋流杯套筒过长的混合段长度对燃烧室点火特性的影响,设计了两种不同的套筒混合段长度试验件,在常温常压条件下,采用单头部模型燃烧室进行了起动点火性能试验,同时采用马尔文进行了燃油雾化颗粒度测量,并结合Fluent软件的数值模拟对结果进行分析.研究结果表明:套筒混合段长度对燃烧室头部流场和油雾分布有很大影响,过长的套筒混合段长度将造成液雾与套筒壁碰撞,限制旋转射流和液滴的径向运动,造成喷雾锥角减小了32%,贫油起动点火油气比增加了20%左右.      

Turbulent boundary layer separation control using plasma actuator at Reynolds number 2000000

An experimental investigation was conducted to evaluate the effect of symmetrical plasma actuators on turbulent boundary layer separation control at high Reynolds number. Compared with the traditional control method of plasma actuator, the whole test model was made of aluminum and acted as a covered electrode of the symmetrical plasma actuator. The experimental study of plasma actuators' effect on surrounding air, a canonical zero-pressure gradient turbulent boundary, was carried out using particle image velocimetry(PIV) and laser Doppler velocimetry(LDV) in the 0.75 m × 0.75 m low speed wind tunnel to reveal the symmetrical plasma actuator characterization in an external flow. A half model of wing-body configuration was experimentally investigated in the  3.2 m low speed wind tunnel with a six-component strain gauge balance and PIV. The results show that the turbulent boundary layer separation of wing can be obviously suppressed and the maximum lift coefficient is improved at high Reynolds number with the symmetrical plasma actuator. It turns out that the maximum lift coefficient increased by approximately 8.98% and the stall angle of attack was delayed by approximately 2° at Reynolds number2 ×10~6. The effective mechanism for the turbulent separation control by the symmetrical plasma actuators is to induce the vortex near the wing surface which could create the relatively largescale disturbance and promote momentum mixing between low speed flow and main flow regions.     

Propagation of plasma bubbles observed in Brazil from GPS and airglow data

Equatorial spread-F is a common occurrence in the equatorial ionosphere that is associated with large variations in plasma density that often cause scintillation and interference in communication signals. These events are known to result from Rayleigh–Taylor instability, but the day-to-day variability of their occurrence is not well understood. The triggering mechanism of plasma depletions is still a matter of debate, but may be linked to gravity waves that under favorable conditions propagate to the middle atmosphere. Understanding the triggering of ESF was the focus of the SpreadFEx campaign near Brasilia, Brazil in 2005. The campaign provided co-located airglow and GPS observations to study the onset of plasma depletions and their evolution as they traversed the region. Comparisons between the 630.0 nm airglow data and GPS data demonstrate the ability of the compact dual frequency GPS array to detect the plasma bubbles and retrieve reliable propagation characteristics of the depletions. In this case study, a plasma depletion was detected and moved over the array at velocities of 85–110 m/s, slowing as it moved towards the east. Correlation of consecutive airglow images gives consistent estimates of the eastward drift over the same time period. Mapping the airglow data to the GPS line-of-sight geometry allows direct comparison and reveals a resolvable westward tilt of the plasma depletion that may be due to vertical shear. The uniqueness of this study is the ability to resolve locally the characteristics of the plasma depletion without relying on assumptions about the mapping of the depletion along magnetic field lines to large latitudinal distances. It presents new information for understanding ESF development and the development of depletions strong enough to produce scintillation.     

IP组播技术在遥测数据传输中的应用分析

在试验场遥测实时数据传输中,为满足传输数据量大、实时性高的要求,在网络数据传输中应用IP组播技术.通过分析网络性能和传输数据的特点,对传输数据进行设计,实现实时数据不丢帧传输.     

A review of observed variability in the dayside ionosphere of Mars

Recent measurements by Mars Global Surveyor and Mars Express have greatly increased the number of observations of the martian dayside ionosphere available for study. Together with earlier measurements from the Viking era, these datasets have been used to investigate variations in well-known properties of the martian dayside ionosphere and to discover new ionospheric features. The dayside ionosphere includes the main peak, called the M2 layer, and a lower layer, called the M1 layer. In the topside, above the M2 layer, electron densities exponentially decrease with increasing altitude.     

Flux rope passage at the Moon while in the terrestrial magnetotail

The Moon spends 20% of its orbit within the terrestrial magnetosphere. During this time it experiences a dynamic plasma environment, including high-speed streams, flux ropes and a flux of heavy ions from ionospheric outflows. 3D multi-fluid simulations of the Moon within the magnetosphere during a substorm shows that a highly variable plasma flow can develop in the vicinity of the Moon due to the passage of a flux rope. The transit of a flux rope past the Moon potentially leads to a plasma wake that is mis-aligned from the optical wake by nearly 30°$30°$. This will have implications when determining the range of space weathering and surface charging the lunar surface experiences.