多维动态参数的多层Bayes融合估计

在多维动态参数的分层模型下，运用多层Bayes估计方法和离散线性模型状态估计方法，给出了动态参数的Bayes融合估计，并以飞行器试验分析的一些例子，说明方法的运用。     

D/H and Nearby Interstellar Cloud Structures

Analysis of UV spectra obtained with the HST, FUSE and other satellites provides a new understanding of the deuterium abundance in the local region of the galactic disk. The wide range of gas-phase D/H measurements obtained outside of the Local Bubble can now be explained as due to different amounts of deuterium depletion on carbonaceous grains. The total D/H ratio including deuterium in the gas and dust phases is at least 23 parts per million of hydrogen, which is providing a challenge to models of galactic chemical evolution. Analysis of HST and ground-based spectra of many lines of sight to stars within the Local Bubble have identified interstellar velocity components that are consistent with more than 15 velocity vectors. We have identified the structures of 15 nearby warm interstellar clouds on the basis of these velocity vectors and common temperatures and depletions. We estimate the distances and masses of these clouds and compare their locations with cold interstellar clouds.     

《建筑结构》课程教学改革实践

为了在《建筑结构》课程教学中，体现高职教育的高等性和职业性，突出高职教育的职业特色，笔者在准确定位课程的教学目标、优化教学内容结构方面进行了探讨，并提出增加实践教学环节，创新教育手段，改革成绩评定方法等建议。     

环境专业教学体系结构改革探索——以就业市场需求为导向

通过对西安航专2006与2007年环境监测与治理技术专业毕业生就业情况的对比分析，认为目前环境类专业的就业形势发生良性转变，需求范围增加，同时就业单位对毕业生的专业技术能力、技术管理能力等也提出了更高的要求。据此，我们从专业发展方向、课程体系结构以及实验实训三个方面进行建设与调整来满足就业单位的需求。     

煤油超燃冲压发动机两相流场数值研究 (Ⅲ)煤油在超燃流场中的多步化学反应特征

深入分析了煤油代用燃料C12H23的17组分30步反应模型在超燃冲压发动机流场内的细观化学反应动力学特征,结果表明：(1)该化学反应模型比较合理地描述了煤油在超燃流场内的裂解、点火、裂解产物的燃烧以及和NOx的生成等基本规律和特征,其中对于OH分布特征的预示和文献的利用PLIF的物理观测结果一致。不过,其单步裂解机制对温度场的预估偏高。(2)对导流型凹槽内的化学动力学特征分析表明,导流槽由于加强了凹槽外氧气向凹槽内的输运,使得凹槽内的燃烧得以强化,生成的CO2偏多。(3)煤油的化学反应动力学过程对于准确预示和评价煤油在超燃发动机内的燃烧状况及发动机整体性能有重要影响。     

高职高专土建类专业创新教学模式的探讨

针对高职高专教改中存在的问题，从能力培养要求，教学体系的改革，实践教学的改革，创新能力的培养等方面进行论述，提出构建模块化实践教学体系，加强专业实践教学改革的思路及可操作性的建议。     

高硅氧增强塑料烧蚀模型中热解层厚度的探讨

通过小型实验固体火箭发动机的多次热试车,对喷管扩散段截面上高硅氧酚醛材料的色变厚度进行了观察,对该截面上材料采用红外光谱成份分析和导电性测量,确认了热解层厚度与碳化层厚度具有相同的数量级,可达2.5mm左右.因此,在作高硅氧酚醛喷管材料的烧蚀与温度场计算时,不宜采用热解面模型,而应采用热解层模型.     

点火能量等因素对脉冲爆震室压的影响实验

以汽油／空气两相混气为可爆混合物，采用汽油机点火和半导体高能点火系统，实验研究了不同点火频率对脉冲爆震室中不同位置脉冲爆震波压力的影响，结果发现，充满度大，产生的紊流强度大，有利于爆震波的形成；在大多数情况下，用低能量（50mJ）的点火系统点火时，点火频率大于实际产生的爆震频率；用高能（IJ）点火系统时，可缩短烯向爆震转变（DDT）的距离，易产生爆震，所得爆震波的峰值压力明显增大，所得结果可为脉冲爆震发动机的设计、爆震点火系统选型提供重要参考。     

Observations of loops and prominences

We review recent observations by the Yohkoh-SXT in collaboration with other spacecraft and ground-based observatories of coronal loops and prominences. These new results point to problems that SoHO will be able to address. With a unique combination of rapid-cadence digital imaging (32 s full-disk and 2 s partial-frame images), high spatial resolution (2.5 arcsec pixels), high sensitivity (EM 10⁴² cm^–3), a low-scatter mirror, and large dynamic range, SXT can observe a vast range of targets on the Sun. Over the first 21 months of Yohkoh operations, SXT has taken over one million images of the corona and so is building up an invaluable long-term database on the large-scale corona and loop geometry. The most striking thing about the SXT images is the range of loop sizes and shapes. The active regions are a bright tangle of magnetic field lines, surrounded by a network of large-scale quiet-Sun loops stretching over distances in excess of 10⁵ km. The cross-section of most loops seems to be constant. Loops displaying significant increase in the ratio of the footpoint to loop-top diameter () are the exception, not the rule, implying the presence of widespread currents in the corona.All magnetic structures show changes. Time scales range from seconds to months. The question of how these structures are formed, become filled with hot plasma, and are maintained is still open. While we see the propagation of brightenings along the length of active-region loops and in X-ray jets with velocities of several hundred km/s, much higher velocities are seen in the quiet Sun. In XBP flares, for example, velocities of over 1000 km/s are common. Active-region loops seem to be in constant motion, moving slowly outward, carrying plasma with them. During flares, loops often produce localized brightenings at the base and later at the apex of the loop. Quiescent filaments and prominences have been observed regularly. Their coronal manifestation seems to be an extended arcade of loops overlying the filament. Reliable alignment of the ground-based data with the X-ray images make it possible to make a detailed intercomparison of the hot and cold plasma structures over extended periods. Hence we are able to follow the long-term evolution of these structures and see how they become destabilized and erupt.     

一种新颖的瞬时浮点放大器

介绍了瞬时浮点放大器的原理及构成，并给出一种结构新的具有２５６阶的瞬时浮点放大器，可有效地提高数据采集系统的测量范围。