燃烧室燃烧与排放特性试验与数值计算

为了探寻燃烧室进口空气温度、压力以及油气比对点熄火边界、温升、燃烧效率以及主要排放物摩尔分数的影响规律， 对航空发动机燃烧室在多工况下的点熄火特性、出口温度分布与主要排放物摩尔分数进行了试验测试。分别采用正癸烷的简化 反应机理与C 12 H 23 燃料的单步反应机理，对该燃烧室火焰筒内流场结构、温度场、中间组分与主要排放物摩尔分数分布特性进行了 数值计算，并与相应试验数据进行了对比分析。结果表明：随着燃烧室进口空气温度、压力以及油气比的提高，燃烧室燃烧效率、 温升、出口平均温度与NO X 摩尔分数逐渐提高，而UHC与CO摩尔分数逐渐降低；与采用C 12 H 23 燃料单步反应机理相比，采用正癸 烷的简化反应机理计算得到的火焰筒内流场与温度场分布更为合理，火焰筒出口温度场分布以及主要排放物摩尔分数与相应试 验数据更为接近，计算精度得到较大提高。     

Length scales for September 14, 2005 solar noise storm

Source length scales are estimated for the September 14, 2005 solar noise storm from the spectral and temporal observed characteristics of the background continuum fluctuations and clusters of Type I bursts. The characteristic height of the magnetic structure where the noise storm source is located and the size of the source where Type I bursts clustering takes place were calculated. A lower limit for the height of the magnetic structure supporting the noise storm at 237 MHz was estimated too.     

场致发射电推力器发射尖端理论模型及机理

为了研究铟场致发射电推力器的发射过程及机理,对椭球顶喷流柱模型离子发射区流柱的形状及尺寸进行了数学描述并通过数值计算加以验证,结果表明,椭球顶喷流柱模型具有合理性,从Taylor理论出发,结合电磁场理论、流体力学理论以及场致发射理论,讨论了离子形成的机理,发现场蒸发是离子产生的重要原因。     

Solar Radio Bursts with Drifting Stripes in Emission and Absorption

This review covers fairly comprehensively experimental and theoretical research on the fine structure of types zebra pattern (ZP) and fiber bursts (FB) in solar type II + IV radio bursts. The basic attention is given to the latest experimental data. A comparative analysis of several recent solar type IV radio outbursts with these fine structure in dynamical radio spectra is carried out using available ground-based and satellite data (Yohkoh, SOHO, TRACE, RHESSI). New data on microwave zebra structures and fiber bursts testifies that they are analogous to similar structures observed at meter wavelengths. The discovery of the superfine structure, in the form of millisecond spikes is the most significant new effect in the cm range. All basic theoretical models of the zebra pattern and fiber bursts are discussed critically. Two main models are studied for their interpretation: (i) interactions between electrostatic plasma waves and whistlers, (ii) radio emission at double plasma resonance (DPR). The relative significance of several possible mechanisms remains uncertain.     

Observation of Transition Region Fine Structures with Soho/Sumer

We present a preliminary analysis of two quiet Sun transition region areas observed with the SOHO/SUMER spectrometer, using lines from oxygen, nitrogen and silicon. The average quiet Sun physical parameters are studied as a function of line intensity. Systematic variations of line position and width with increasing intensity are found. A large number of small-scale active points have been observed, and preliminary analysis of the physical properties and dynamics of these active features is presented. A jet-like structure, found in an active point, is also investigated and its velocity along the line of sight determined. This revised version was published online in June 2006 with corrections to the Cover Date.     

Radio Emissions from Solar Active Regions

Solar active region coronae are known for strong magnetic fields permeating tenuous plasma, which makes them an ideal astronomical laboratory for magnetohydrodynamics research. It is, however, relatively less known that this physical condition also permits a very efficient radiation mechanism, gyro-resonant emission, produced by hot electrons gyrating in the coronal magnetic field. As a resonant mechanism, gyro-emission produces high enough opacity to fully reveal the coronal temperature, and is concentrated at a few harmonics of the local gyrofrequency to serve as an excellent indicator of the magnetic field. In addition, the polarization of the ubiquitous free–free emission and a phenomenon of depolarization due to mode coupling extend the magnetic field diagnostic to a wide range of coronal heights. The ability to measure the coronal temperature and magnetic field without the complications that arise in other radiative inversion problems is a particular advantage for the active region radio emissions available only at these wavelengths. This article reviews the efforts to understand these radiative processes, and use them as diagnostic tools to address a number of critical issues involved with active regions.     

On the Differences in Composition between Solar Energetic Particles and Solar Wind

Although the average composition of solar energetic particles (SEPs) and the bulk solar wind are similar in a number of ways, there are key differences which imply that solar wind is not the principal seed population for SEPs accelerated by coronal mass ejection (CME) driven shocks. This paper reviews these composition differences and considers the composition of other possible seed populations, including coronal material, impulsive flare material, and interplanetary CME material.     

混合微波集成电路及其应用

近期来，由于科学技术的发展，混合微波集成电路几乎进入所有实用的微波装备。本文对其结构、工艺材料以及在微波系统中的应用作了介绍。     

典型海上热发射动力学效应及影响因素分析

考虑海上发射环境特殊性,分析了发射船承受的典型海浪以及风环境,针对陆基发射时运载火箭直接坐落在发射台上的裸箭热发射方式,分析了该支撑形式在海上动态环境下的射前稳定性,获得海上裸箭热发射方式的承受晃动极限。为解决陆基热发射支撑方式不满足三级海况发射稳定性的问题,提出运载火箭的框架式扶稳措施,通过框架内的柔性支撑保证运载火箭的射前稳定性。构建由火箭、等效甲板、导向框架、导轨、柔性支撑、发射台等组成的发射系统动力学仿真模型,开展复杂海况条件下的发射动力学分析,获得了框架式热发射方式在典型海况条件下,不同因素对火箭出框过程飞行姿态、安全间隙等影响规律,可为运载火箭框架式热发射的海上动基座发射动力学安全性评估提供技术支撑,并用于框架式热发射方式的海上动基座环境适应性的综合评价。     

Flaring loop parameters estimated from solar decimeter type U-like and type J-like fine structures

This work presents the analysis of five fine structures in the solar radio emission, observed between June 2000 and October 2001 by the Brazilian Solar Spectroscope (BSS), in the decimeter frequency band of 950–2500 MHz. Based on their morphological characteristics identified in the dynamic spectra, the fine structures had been classified as type U-like or type J-like bursts. Such emissions are variants of the type III bursts. They support the hypothesis of generation by plasma emission mechanism, from interaction of electron beams accelerated during solar flares, propagating along closed magnetic structures, within the trapped plasma of the solar corona. The spectral and temporal characteristics of the five fine structures had been obtained from the dynamic spectra and the parameters of the agent and the emitting source have been determined, assuming both fundamental and harmonic emissions. The analysis revealed the flux density of the structures is less than 20–80 s.f.u. For assumption of harmonic emission, the interval of values for the source parameters estimated are: the loop size is (0.3–5.1) × 10¹⁰ cm; the electron beam velocity is in the range of 0.16–0.53 c; the temperature of coronal loop top is of the order of (0.25–1.55) × 10⁷ K; and the low limit for the magnetic field is of 7–26 G. These results are in agreement with previous determinations reported in the literature.