High Excitation ISM and Gas

An overview is given of ISO results on regions of high excitation ISM and gas, i.e. HII regions, the Galactic Centre and Supernova Remnants. IR emission due to fine-structure lines, molecular hydrogen, silicates, polycyclic aromatic hydrocarbons and dust are summarised, their diagnostic capabilities illustrated and their implications highlighted. Based on observations with ISO, an ESA project with instruments funded by ESA Member States (especially the PI countries: France, Germany, The Netherlands, and the United Kingdom), and with the participation of ISAS and NASA.     

某型发动机高原起动过程数学模型建立

针对某型发动机高原起动过程具有危险性大和变化规律复杂的特点,提出了一种变记忆长度的小波变换多分辨分析方法。该方法将辨识的数据分解到不同频段,然后针对各不同频段采用不同的记忆长度进行辨识,从而可以建立起该型发动机高原起动过程的数学模型,为高原起动试验提供理论参考。      

基于特征的蒙皮镜像铣加工残区刀轨优化方法

镜像铣加工装备及其加工工艺是蒙皮零件加工的有效手段,其特殊工艺对加工刀轨提出了等步距、无交叉、无抬刀且无残留等特殊要求。针对蒙皮零件加工特征的复杂形状,在满足等步距、无抬刀、无交叉的条件下对加工残留区域进行刀轨优化是一个难题。为解决以上难题,本文提出了一种基于特征的蒙皮镜像铣加工残区刀轨优化方法。该方法基于特征将蒙皮零件的工艺信息与几何信息相关联,自动提取加工特征的加工面及其对应的刀轨,将刀轨分割成若干段子刀轨,并构建子加工区域,再利用布尔并运算得到最终可加工区域。然后对加工面区域与最终可加工区域求布尔差识别出加工残留区域,并根据加工残区位置自适应生成满足蒙皮镜像铣特殊要求的优化刀轨。以典型复杂蒙皮零件验证本文提出的方法,结果表明,基于特征的蒙皮镜像铣加工残区刀轨优化方法可自动识别加工残区,并生成满足蒙皮镜像铣特殊要求的加工残区优化刀轨,为提高蒙皮零件数控编程效率提供技术支撑。     

基于面板数据模型的中西部地区加工贸易升级研究

我国经济高速发展,劳动力、土地等要素随之发生转变,加工贸易从东部地区向中西部地区转移,中西部地区加工贸易急需升级以适应发展。利用2001-2011年中西部地区部分省份的面板数据建立计量模型,通过检验对混合估计模型、固定效应模型和随机效应模型进行选择,并对选定模型的估计结果进行具体分析,提出中西部地区加工贸易升级的对策及建议。     

Establishment of atmospheric weighted mean temperature model in the polar regions

Due to the special geographical location and extreme climate environment, the polar regions (Antarctic and Arctic) have an important impact on global climate change. Atmospheric weighted mean temperature (Tm) is a crucial parameter in the retrieval of precipitable water vapor (PWV) from the zenith wet delay (ZWD) of ground-based Global Navigation Satellite System (GNSS) signal propagation. In this paper, the correlation between weighted mean temperature and surface temperature (Ts) is studied firstly. It is shown that the correlation coefficients between Tm and Ts are 0.93 in the Antarctic and 0.94 in the Arctic. The linear regression Tm model and quadratic function Tm model of the Antarctic and the Arctic are established respectively using the radiosonde profiles of 12 stations in the Antarctic and 58 stations in the Arctic from 2008 to 2015. The accuracies of the linear regression Tm model, the quadratic function Tm model and GPT2w Tm model which is a state-of-the-art global Tm model are verified using the radiosonde profiles from 2016 to 2018 in the Antarctic and Arctic. Root Mean Square (RMS) errors of the linear regression Tm model, the quadratic function Tm model and GPT2w Tm model in the Antarctic are 3.07 K, 2.87 K and 4.32 K respectively, and those in the Arctic are 3.53 K, 3.38 K and 4.82 K, which indicates that the quadratic function Tm model has a higher accuracy compared to linear regression Tm model, and the accuracies of the two regional Tm models are better than that of GPT2w Tm model in the polar regions. In order to better evaluate the accuracy of Tm in the PWV retrieval, the PWV values of radiosondes are used for comparisons as the reference value. The RMS errors of PWV derived from the two Tm models are similar for 1.28 mm in the Antarctic and 1 mm in the Arctic respectively. In addition, the spatial and temporal variation characteristics of Tm are analyzed in the polar regions by spectral analysis of Tm data using fast Fourier transform. The results show that the Tm has obvious seasonality and annual periodicity in the polar regions, and the maximum difference between warm season and cold season is about 63 K. After comparing and analyzing the influences of latitude, longitude and elevation on the Tm in the polar regions, it is found that latitude and elevation have a greater influence on the Tm than the longitude. As the latitude and elevation increase, the Tm decreases, and vice versa in the polar regions.     

Latitudinal distribution of solar coronal active regions

We studied the cyclic evolution of the latitudinal distribution of solar coronal active regions based on daily images from SOHO EIT for the period 1995–2017. Fully automated software was used, which included the following steps: initial preparation of images in the data series, normalization of histograms and correction of limb brightening, segmentation of images using threshold intensity values obtained from their histograms, scanning of segmented images in heliographic coordinates and obtaining profiles of latitudinal distribution of coronal active regions for each image of the data series. From the output data, we obtained a temporary change in the latitudinal distribution profiles and the migration of activity centers on the solar disk. From the period of minimum activity to the next minimum in both hemispheres, activity centers begin to migrate from high latitudes towards the equator. At the same time, the general center of activity repeatedly changes the direction of migration. The latitudinal distribution of the so-called presence factor of coronal active regions closely resembles the magnetic butterfly diagram, which proves their direct causal relationships. Variations in the presence factor of coronal active regions are correlated with cyclic variations in the sunspot daily numbers.     

两极地区局部点质量模型构建方法

针对两极地区位系数模型计算扰动引力时的奇异问题和点质量模型方程解不稳定问题,分别引入扰动引力去奇异算法和基于换极法的两极地区局部点质量模型构造方法.数值实验结果表明,去奇异算法能有效解决靠近极点处扰动引力计算过程中出现的奇异性问题,基于换极法的点质量模型在两极地区方程结构稳定,精度与位系数模型相当.本文方法可为极区飞行器扰动引力快速赋值提供新的思路.     

Tilts and polarity separation in the sunspot groups and active regions at the ascending and descending phases of the cycle 23

The Solar Feature Catalogues for sunspots and active regions measured with SOHO/MDI instrument and Ca II K3 spectroheliograph of the Paris-Meudon Observatory are analyzed with the automated classification technique for sunspot groups and active region polarities. We report the first classification results for daily variations of tilt angles (normal and trigonometric ones) in sunspot groups (SG) and active (AR) regions in the cycle 23. The average normal tilts are presented for every year at the ascending and descending phases of the cycle 23 which are similar to those deduced by other authors for the cycles 19–22. The normal tilts of both the sunspot groups and active regions are shown to increase in the ascending phase and a decrease in the descending phase. Similar to SG and AR areas, the trigonometric tilts are shown to have the noticeable North–South asymmetry with the Southern hemisphere dominant in the selected ascending and descending periods. The normal tilt variations with latitude follow Joy’s law revealing a periodicity along the meridian of about 10° and reaching the maximum of 14° at the latitude of about 32° corresponding to the top of the ‘royal zone’ where the sunspots appear. The variations of polarity separation with a latitude are in an anti-phase with those of the tilts reaching a maximum at the latitude of 35° and showing a small positive separation for the groups/active regions in a vicinity of the average tilts ±40°. The ratio R of the polarity separation to the trigonometric tilt fits the linear function of a latitude φ as R = −0.0213φ − 0.1245 confirming positive separation for the polarities of active regions with the average tilts, or the dominance of activity in the Southern hemisphere activity, for the selected period of observations.     

不同GNSS在高纬度地区时间传递性能分析

全球卫星导航系统（GNSS）载波相位时间传递技术是高精度时间传递领域的主要研究方法之一，但目前关于该部分的研究主要集中在中低纬度地区，在高纬度地区并不多见。不同GNSS由于星座设计不同，在高纬度地区结构差异较大，因此需要对不同GNSS在高纬度地区的时间传递性能进行分析。实验结果表明，在高纬度地区时间传递中，Galileo稳定度最高，GPS和BDS次之，GLONASS最差。同时因在高纬度地区卫星的高度角普遍偏低，为合理平衡低高度角时可视卫星多和多路径误差大的矛盾，对不同截止高度角下获取的链路时间传递性能进行了分析。结果表明，在5°截止高度角下，高纬度地区的时间传递链路稳定性最好。     

Monopolar structure of the Sun in between polar reversals and in Maunder Minimum

After a polar reversal in one hemisphere the Sun has two polar caps of the same sign, leaving it in a kind of monopolar state. It may take months before a polar reversal occurs in the other hemisphere. The situation may have been extreme in the Maunder Minimum where the northern hemisphere most probably did not have polar reversals during several cycles, while the southern hemisphere may have had some. This may affect the interplanetary field and thus the cosmic rays reaching the Earth. Using the relation between the Wolf number and the speed of the global magnetic field regions the yearly mean Wolf number has to exceed 40 in order to have polar reversals, hence per hemisphere we expect that it must exceed 20. This may be used to give a definition of a deep minimum.