用亚稳态正电子素研究络合的瞬态反应（Ⅲ）

本文用自制的装有 BaF_2探头的高探测效率的正电子湮没寿命谱仪测量了在室温下正电子素 o-Ps 与 p-RPhG 及 m-RPhG(R=NO_2,Cl,H,CH_3,cH_3O)在20%(V/V)二氧六环水溶液中的络合形成速度常数。实验结果表明,这些o-Ps-M 络合形成速度常数 K 值均与作为配位体的 p-RPhG、m-RPhG 的碱性解离常数 K 的负对数 pK_2 呈线性函数。这表明上述瞬态络合反应满足线性自由能关系,由此可推断出上述络合反应的一些重要性质。     

Sustained data recording system based on disk array

Most sustained data recording systems in many real-time fields are based on tape equipments. We have developed an innovative sustained data recording system based on disk array which consists of Array Controller Module (ACM), String Controller Module (SCM) and Main Controller Module (MCM). This system has a better performance and higher reliability than the traditional tape recorder and can be used conveniently in many areas of data recording, storing, playback, and remote backup. This novel recording system has been used in radar data recorder for spacecraft orbit tracking and satellite remote sensing data recording successfully.     

Ionospheric behavior of the F2 peak parameters foF2 and hmF2 at Hainan and comparisons with IRI model predictions

Monthly median values of foF2, hmF2 and M(3000)F2 parameters, with hourly time interval resolution for the diurnal variation, obtained with DPS-4 digisonde observations at Hainan (19.4°N, 109.0°E) are used to study the low latitude ionospheric variation behavior. The observational results are compared with the International Reference Ionospheric Model (IRI) predictions. The time period coverage of the data used for the present study is from March 2002 to February 2005. Our present study showed that: (1) In general, IRI predictions using CCIR and URSI coefficients follow well the diurnal and seasonal variation patterns of the experimental values of foF2. However, CCIR foF2 and URSI foF2 IRI predictions systematically underestimate the observed results during most time period of the day, with the percentage difference ΔfoF2 (%) values changing between about −5% and −25%, whereas for a few hours around pre-sunrise, the IRI predictions generally overestimate the observational ones with ΔfoF2 (%) sometimes reaching as large as ∼30%. The agreement between the IRI results and the observational ones is better for the year 2002 than for the other years. The best agreement between the IRI results and the observational ones is obtained in summer when using URSI coefficients, with the seasonal average values of ΔfoF2 (%) being within the limits of ±10%. (2) In general, the IRI predicted hmF2 values using CCIR M(3000)F2 option shows a poor agreement with the observational results. However, when using the measured M(3000)F2 as input, the diurnal variation pattern of hmF2 given by IRI2001 has a much better agreement with the observational one with the detailed fine structures including the pre-sunrise and post-sunset peaks reproduced reasonably well. The agreement between the IRI predicted hmF2 values using CCIR M(30,000)F2 option and the observational ones is worst for the afternoon to post-midnight hours for the high solar activity year 2002. During daytime hours the agreement between the hmF2 values obtained with CCIR M(30,000)F2 option and the observational ones is best for summer season. The discrepancy between the observational hmF2 and that obtained with CCIR M(30,000)F2 option stem from the CCIR M(3000)F2 model, which does not produce the small scale structures observed in the measured M(3000)F2.     

On the impulsiveness of the Hα emission from a flaring atmosphere

Emissions from solar flares may reveal fast fluctuations, which can be attributed to small-scale injections of energetic electrons. In this paper, we perform numerical calculations of the Hα emission from a flaring atmosphere bombarded by a pulsating electron beam. We assume that the variation of the electron beam flux consists of two components: a fluctuation component and a background component. The results show that the amplitude of Hα fluctuations varies depending on the magnitude of the background flux of the electron beam. In the case of a higher background flux, the Hα fluctuations are more significant than in the case of a lower background flux. This result is compatible with the observations in which the Hα fluctuations appear preferentially near the hard X-ray maximum.     

Chase observations from spacelab 2 — the chase team

The Coronal Helium Abundance Spacelab Experiment (CHASE) was designed and built in the UK by groups at the Rutherford Appleton Laboratory and at the Mullard Space Science Laboratory. The main objective of the experiment was to improve the measurement of the abundance of helium in the Sun, which currently is uncertain by a factor of approximately three. Since most of this helium must be of primordial origin, being formed within a few minutes of the big bang, such a measurement would also have significant cosmological implications.The instrument consisted of a grazing incidence telescope feeding a 1200 lines mm⁻¹ diffraction grating. Parts of the dispersed spectrum were then observed around the Rowland circle with channel electron multipliers and a channel multiplier array plate. During the flight, good observations were made of the Lyman-α lines of hydrogen at 1216 A and of ionised helium at 304 A, both in the corona, where the lines are formed by resonance scattering, and on the solar disc where excitation of the lines is much more complex.The spectrometer was also able to observe many other transition region and coronal lines in ions of O, S and Fe. Images in these lines clearly show how the magnetic fields in active regions constrain the material in arch-shaped loops with the hot material towards the top.     

振动系统反共振点的力谱预示

通过结构模态试验和小量级振动试验,获得有效反应真实结构特性的有限元模型,并利用简化的两自由度振动系统和小量级试验数据分析,预示出振动系统在反共振点进行力限(加速度带谷)的条件。为工程中抑制过试验问题,进行力限条件控制提供了重要依据和参考。     

三元共掺杂对YSZ热障涂层热物理性能的影响

采用NiO、Er_2O_3、Yb_2O_3、Y-2O_3、ZrO_2粉末为原料,用高温固相合成法制备复合陶瓷材料,研究该复合陶瓷材料的比热、热扩散系数、热导率等热物理性能,并与传统8YSZ热障涂层材料进行对比。利用XRD测定所制备的陶瓷样块的晶体结构和物相组成,分析该陶瓷试样的物相组成及高温相稳定性。结果表明:NiO、Er_2O_3、Yb_2O_3共掺YSZ后,室温至1500℃范围内的热扩散系数为0.36～0.56 mm^2/s,与8YSZ相比,降低了约20%;室温至1500℃的热导率为1.45～1.55 W/(m·K),比8YSZ降低了18%;2EYNYSZ陶瓷材料具有单一的相结构,经1500℃热处理100 h之内不发生相变。     

基于分段常滑翔角的长航时纵向远程滑翔飞行方程近似解

提出用包含地球旋转效应的n个常滑翔角飞行段近似实际滑翔飞行轨迹的方法。基于该方法推导了长航时纵向远程滑翔飞行轨迹近似解，并给出了各段常滑翔角、滑翔时间的求解方法及整个滑翔轨迹近似计算步骤。文中算例结果表明，该近似求解方法计算得到的滑翔航程和滑翔时间与实际值相差很小，航程误差率约为0．7％，时间误差率约为0．6％，因此该方法在近似小初始滑翔角的长航时远程纵向滑翔飞行时是有效的、可行的，尤其针对航程在地球半圈以上的滑翔飞行轨迹。