紧凑拉伸试样应力强度因子的统一公式

 本文通过简单的力学分析,导得了紧凑拉伸试样应力强度因子的统一的表达式（公式（5）,（7）,（8））,可以适用于相当宽的H/W和a/W的范围,与边界配置法结果相比,误差小于1％（大多数数据的误差小于O.5％）。 本文采用的基本函数K_b和K_s,均为Srawley^[1、2]等用边界配置法得到的结果拟合而求得的。在拟合过程中发现文献[1、2]内有五个数据异乎寻常,证实了文献[3]中重新计算的结果。 利用本文的表达式还可以方便地计算试样的柔度,结果也是令人满意的。     

机动襟翼的气动特性

 机动襟翼是现代战斗机提高机动格斗能力的常用措施。本文根据风洞实验结果,讨论了机动襟翼减阻的能力和原因,襟翼弦长和展长的影响,前缘襟翼和后缘襟翼的配合使用问题,机翼边条和机翼平面形状对机动襟翼减阻的影响,以及机动襟翼对大迎角飞行品质的改善情况。讨论表明,机动襟翼是提高战斗机空战格斗能力的有效措施。它能控制气流分离和减小大迎角时的阻力,提高抖振边界和降低抖振强度,改善大迎角的飞行品质。为了得到最佳的综合效果,机动襟翼的参数选择必须考虑对飞机结构和系统的影响。     

X-Ray spectroscopic investigation of the coronal structure of capella

The binary system Capella (G6 III + F9 III) has been observed on 1979 March 15 and on 1980 March 15–17 with the Objective Grating Spectrometer (OGS) onboard theEinstein Observatory. The spectrum measured with the 1000 l/mm grating covers the range 5–30 Å with a resolution < 1 Å. The spectra show evidence for a bimodal temperature distribution of emission measure in an optically thin plasma with one component 5 million degrees and the other one 10 million degrees. Spectral features can be identified with line emissions from O VIII, Fe XVII, Fe XVIII, Fe XXIV, and Ne X ions. Good spectral fits have been obtained assuming standard cosmic abundances. The data are interpreted in terms of emission from hot static coronal loops rather similar to the magnetic arch structures found on the Sun. It is shown that the conditions required by this model exist on Capella. Mean values of loop parameters are derived for both temperature components.     

The Rosat mission

The primary scientific objective of the ROSAT mission is to perform the first all sky survey with an imaging X-ray telescope leading to an improvement in sensitivity by several orders of magnitude compared with previous surveys. Consequently a large number of new sources (> 10⁵) will be discovered and located with an accuracy of 1 arcmin. After completion of the survey which will take about half a year the instrument will be used for detailed observations of selected targets.The X-ray telescope consists of a fourfold nested Wolter type I mirror system with 80 cm aperture and 240 cm focal length, and three focal plane detectors. In the baseline version these will be imaging proportional counters (0.1 – 2 keV) providing a field of view of 2⁰ × 2⁰.     

“频域最小阶Kx-观测器”的设计

利用受控系统在频域的传递函数矩阵,直接设计频域最小阶Kx-观测器,可以避免状态空间实现这一中间环节,减少研究层次。本文利用多项式向量空间的对偶最小基和多项式矩阵的Popov阶梯形的概念,分析了频域最小阶Kx-观测器的设计问题,做了大量简化,得到一种设计算法,并附有例题说明。层次清楚,方法简便,在工程应用上是可取的。 文中对于频域Kx-观测器的可能最小阶数,也作了一些讨论,得到一些有益的结果。     

断裂力学在直升机桨毂上的应用

 本文用实验方法,得出了计算弯曲载荷下含表面裂纹圆轴、圆筒的应力强度因子（K_I）的表达式,并按照裂纹面积扩展率公式,分析了直升机桨毂转轴轴颈的临界裂纹面积和剩余疲劳寿命。为了校核断裂力学分析的可靠性,模拟飞行状况进行了实际桨毂支臂转轴轴颈的疲劳试验。实验结果与计算结果相当符合。     

Spectra and time variability of GX 5-1

From a short observation of GX 5-1 with EXOSAT we have derived information on spectral and temporal behaviour in the energy range 1–20 keV. The source was found to be variable on time scales from 10 s to 1 h. Describing the spectrum one is forced to assume at least two spectral components. The best fit is reached using a spectrum composed of two blackbody functions with typical temperatures 1 keV and 2 keV, corresponding to apparent blackbody radii of 43 km and 11 km, respectively (for a distance of 10 kpc). With respect to the hot component there is evidence for variability in temperature as well as in apparent blackbody radius. No periodic variability has been found over the period range 0.25 s to 2000 s. There is no evidence for an iron emission line.     

EXOSAT medium energy observations of Cyg X-2

On July 5.–6. 1983, during the EXOSAT performance verification (PV) and calibration phase, a raster scan of Cygnus X-2 was performed. In contrast to the previously observed smooth intensity variations on timescales of hours, the source revealed a behaviour unknown until now: active periods with high energy flares recurring on time scales of 300–500 s were interrupted by quiet periods of several hours. At all intensity levels the source spectra clearly require a two component continuum (blackbody + thermal bremsstrahlung). In addition, a weak iron emission line with equivalent widths between 39 an 70 eV was detected. The source has a much harder spectrum during the flares than during quiet periods, indicating drastic temperature changes within the emission region, while the absolute iron line flux does not vary. From the spectral characteristics it becomes clear that self-comptonization of the thermal bremsstrahlung spectrum plays an important role. The time variability and spectral behaviour in this peculiar state allow Cyg X-2 to be classified as a Low Mass X-ray Binary System (LMXB) very similar to the prototype of this class, Sco X-1.     

The long term variability of 4U 1258-61 (GX304-1)

We present optical spectroscopy and photometry of 4U 1258-61 obtained over the course of six years. Evidence for the evolution of a circumstellar envelope throughout the course of the observations is presented.