太阳风高速流能流分布

根据Ylysses观测,比较完整地计算了高纬行星际空间太阳风能流分布．计算表明,行星际空间的高速流能流密度约为2．1×10-3J·m-2·s-1（日心距离r＝1AU）,主要来自于太阳风离子所携带的动能流（占58％）和克服太阳引力的势能流（占39％）．要驱动高速流,需要在日冕底部高速流源区（日心距离r=1Rs）向外输出到太阳风的能流密度为7．1×102J·m-2·s－1·分析表明,由日冕底部向外可能输出两种形式的能流,其中一种具有较短的耗散长度,被耗散在很短的空间区域（～1—2Rs）,使日冕温度迅速提高。另一种储藏在连续向外传播的太阳风中,不断耗散用以加速太阳风（＞2Rs）．     

Testing the blast wave model with Swift GRBs

The complex structure of the light curves of Swift GRBs (e.g. superimposed flares and shallow decay) has made their interpretation and that of the blast wave caused by the burst, more difficult than in the pre-Swift era. We aim to constrain the blast wave parameters: electron energy distribution, p, density profile of the circumburst medium, k, and the continued energy injection index, q. We do so by comparing the observed multi-wavelength light curves and X-ray spectra of a Swift sample to the predictions of the blast wave model.     

An experimental investigation on static directional stability

A generic aircraft usually loses its static directional stability at moderate angle of attack (typically 20–30?). In this research, wind tunnel studies were performed using an aircraft model with moderate swept wing and a conventional vertical tail. The purpose of this study was to investigate flow mechanisms responsible for static directional stability. Measurements of force, surface pressure and spatial flow field were carried out for angles of attack from 0? to 46? and sideslip angles from ?8? to 8?. Results of the wind tunnel experiments show that the vertical tail is the main contributor to static directional stability, while the fuselage is the main contributor to static directional instabil-ity of the model. In the sideslip attitude for moderate angles of attack, the fuselage vortex and the wing vortex merged together and changed asymmetrically as angle of attack increased on the wind-ward side and leeward side of the vertical tail. The separated asymmetrical vortex flow around the vertical tail is the main reason for reduction in the static directional stability. Compared with the wing vortices, the fuselage vortices are more concentrated and closer to the vertical tail, so the yaw-ing moment of vertical tail is more unstable than that when the wings are absent. On the other hand, the attached asymmetrical flow over the fuselage in sideslip leads to the static directional instability of the fuselage being exacerbated. It is mainly due to the predominant model contour blockage effect on the windward side flow over the model in sideslip, which is strongly affected by angle of attack.     

高湍流度对平板边界层传的热影响

在雷诺数为１０６—１０７之间对０．１％—２５％湍流度的自由来流流过平板边界层传热问题进行了实验与数值研究。实验是在吸入式风洞内进行，用自由来流冷却加热平板，自由来流的湍流度可高达３０％。计算模型针对二维定常流，采用代数应力（热流）湍流模型，用ＳＩＭＰＬＥ算法进行计算。结果表明：高湍流度自由来流可使平板的平均Ｓｔａｎｔｏｎ数增加８５％。     

对复杂平面连杆机构运动分析的研究

本文提出了用转化机构法进行单自由度复杂平面连杆机构的运动分析.基本思想是通过改变机构的原动件或机架或同时改变原动件和机架,以简化机构的运动分析.这种方法对常见的平面复杂连杆机构的运动分析非常有效,无需进行复杂的试凑或迭代.同时本文提出的这种解法有较为广泛的意义,对加深认识机构的组成以及对机构其它问题的研究都是+分重要的.     

Changes in radio emission from PSR J0737–3039B

The double pulsar system, J0737–3039, provides a unique probe of a pulsar magnetosphere due to its edge-on viewing geometry, a tight orbit and a significant rate of advance of the angle of periastron. In this paper, we report on the changes in radio emission from the long period pulsar in this system, J0737–3039B, over a period of 9 months. Observations of this system with Giant Metrewave Radio Telescope (GMRT) show that the duration of the first bright phase of the pulsar centered at 210° orbital longitude from the ascending node is shrinking. These observations will be useful to constrain the proposed models for this system.     

一种新型无机耐烧蚀复合材料固化机理的研究

在特定温度下，采用一定比例的氢氧化铝和磷酸合成出磷酸铝基体，对玻璃纤维或织物处理后，采用手糊工艺（固化温度低于220℃）制备了新型耐烧蚀复合材料——织物增强磷酸铝基复合材料。借助XRD和TG—DTA等测试技术，详细研究了材料的固化机理，发现材料可采用加热固化和常温固化。其热固化机理为：在加热时，酸式磷酸铝脱水形成聚合状的磷酸铝，然后转变为线型聚磷酸铝或环状偏磷酸铝；常温固化机理为：在常温下，酸式磷酸铝与活性适中的固化剂反应而获得强度。     

K4169高温合金组织细化研究

研究了 K4 1 6 9高温合金在不同浇注温度及向熔体中加入细化剂时的晶粒组织。结果表明 ,降低浇注温度可以明显细化凝固后基体的晶粒和提高铸件断面等轴晶的比例。在通常的浇注温度 1 4 0 0℃和 1 4 2 0℃下 ,并对合金熔体进行均匀化处理时 ,加入所研制的复合细化剂可使圆柱锭的晶粒分别细化至 ASTM1 .7级和 ASTMM1 0 .5级 ;断面等轴晶的比例分别达 96 %和 90 %以上。本文提出了晶粒细化的机理并分析了晶粒细化后断面等轴晶比例增大的现象     

Time variations of the total electron content in the Southeast Asian equatorial ionization anomaly for the period 2006–2011

This study presents the time variations of the total electron content in the South East Asian equatorial ionization anomaly. The time variation of the TEC is analyzed through the period 2006–2011 by using a latitudinal chain of GPS stations extending in the northern and southern hemisphere. The data shows that the shape of the diurnal variation of the TEC depends on the latitude: a plateau is observed at the stations near the equator and a Gaussian at the station distant from the equator. We observe a semiannual pattern in all the stations with maxima at equinox. In both hemispheres, the amplitude of the crest is larger in spring than autumn from 2006 to 2008 and smaller in spring than in autumn from 2009 to 2011. We also observe an asymmetry between the amplitude and the position of the two crests of ionization. There is a very high level of correlation between the amplitude of the TEC at the two crests and the sunspot number: ∼0.88. During the deep solar minimum 2008–2009, the amplitude of crests of ionization becomes small during several months in summer and winter. The results show that both crests move significantly equatorward in winter than other seasons and there is a tendency for both crests to appear earlier in winter and later in summer.