影响靖宇地区温带气旋的统计分析

核电站因它不排放如二氧化碳这样的温室气体,核电对降低能源部门的碳密集作出了贡献,因此愈益受到人们的重视.在对核电站地区的天气、气候环境进行分析的基础上,对影响靖宇核电站地区的温带气旋作了研究.结果表明:1949-2007年期间影响靖宇地区的温带气旋计111个;受温带气旋影响的年数有41年(约2/3).影响靖宇地区且产生强降雨的温带气旋,主要发生在6、7、8月这3个月,并且一半以上出现在7月.影响靖宇地区的温带气旋大部分是东北气旋,占总数的65%;蒙古气旋与华北气旋次之.此外,对造成严重影响的温带气旋的个例也从天气学角度进行了分析.     

江淮梅雨的时空变化特征

利用江淮地区37站1954--2001年48a梅雨特征量资料,采用谐波分析、EOF和最大熵谱分析等方法讨论了江淮梅雨的时空变化特征。结果表明：江淮梅雨时空分布不均,梅雨特征量存在显著的年际一年代际变化特征,梅雨特征量年代际变化之间存在明显的负相关或正相关关系;梅雨特征量存在显著不同的多时间尺度振荡周期和长期演变趋势且江淮地区雨季也呈不同的年际和年代际变化特征。     

海南GPS网探测对流层水汽廓线的试验研究

介绍了2005年11月在海南地区进行的一次地基GPS小网观测试验。试验目的是研究利用组网的GPS倾斜路径观测进行对流层水汽层析反演, 给出站点上空水汽的垂直廓线结构信息。概述了试验中GPS原始数据处理方法以及层析反演的方法。将GPS层析得到的水汽垂直廓线与海口站探空观测的水汽廓线进行了对比, 结果表明:二者一致性较好, 均方根误差在0.5g·m-3左右, 层析结果较好地反映出试验期间水汽减少、大气变干的过程。另外, 采用3种不同的先验信息方案测试分析了GPS层析的结果, 表明GPS观测量对水汽先验信息有明显的调整作用。并对GPS水汽层析中可能存在的问题进行了讨论。试验证明高时间分辨率的GPS观测有能力层析出GPS测站上空水汽的廓线信息。     

利用VB语言开发县级MICAPS 2.0资料本地化接收系统

针对县级无法及时、完全接收卫星资料的问题,利用VB语言开发了县级MICAPS2.0资料本地化接收系统,使县级气象台站能够共用地(市)级的卫星单收站接收的资料.     

Observational Study of a Peculiar Solar Limb Event Occurred on 11 January 2002

On 11 January 2002, using the Multi-channel Infrared Solar Spectrograph (MISS) at the Purple Mountain Observatory (PMO), we obtained Hα, Ca ii 8542 Å and He i 10?830 Å spectra and slit-jaw Hα images of a peculiar solar limb event. A close resemblance of its intensity to that of a small flare and the GOES X-ray flux indicates that it was an active prominence. However, its morphological evolution and velocity variation were different from general typical active prominences, such as limb flares, post-flare loops, surges and sprays. It started with the ejection of material from the flare site. In the early phase, the ejecta was as bright as a limb flare and kept rising until reaching the height of (8????10)×10⁴ km at an almost constant velocity of 91.7 km? s ^?1 with its lower part always connected to the solar surface. EUV images in 195 Å show similar structure as in the Hα line, indicating the coexistence of plasmas with temperatures differing by more than two orders of magnitude. Later some material started to fall back to another bright area on the solar surface. The falling material did not show the collimated structure of surges or the arc structure of flaring arches. A red-shift velocity of more than 200 km? s ^?1 was detected in a bright point close to the outer edge of the closed loop system formed later, which dispersed in a few minutes and became a part of the newly formed large loop. The ejected material did not leave the sun, indicating that the magnetic reconnection was not sufficient to remove the overlying field lines during the process. The spectral line profiles showed large widths and variable velocities, and therefore the line-pair method is not applicable to this event for the estimation of physical parameters.     

利用窄线宽激光测量锶原子束速率分布

利用多普勒频移效应,通过线宽2MHz窄线宽激光与锶原子束在大角度作用下的荧光信号分析,测量了锶原子束速率分布。比较和分析表明,理论结果与实验结果符合较好。     

The causality between the rapid rotation of a sunspot and an X3.4 flare

Using multi-wavelength data of Hinode, the rapid rotation of a sunspot in ac-tive region NOAA 10930 is studied in detail. We found extraordinary counterclockwise rotation of the sunspot with positive polarity before an X3.4 flare. From a series of vector magnetograms, it is found that magnetic force lines are highly sheared along the neu-tral line accompanying the sunspot rotation. Furthermore, it is also found that sheared loops and an inverse S-shaped magnetic loop in the corona formed gradually after the sunspot rotation. The X3.4 flare can be reasonably regarded as a result of this movement. A detailed analysis provides evidence that sunspot rotation leads to magnetic field linestwisting in the photosphere. The twist is then transported into the corona and triggers flares.     

Flare-induced signals in polarization measurements during the X2.6 flare on 2005 January 15

Flare-induced signals in polarization measurements which were manifested as apparent polarity reversal in magnetograms have been reported since 1981. We are motivated to further quantify the phenomenon by asking two questions: can we distinguish the flare-induced signals from real magnetic changes during flares, and what we can learn about flare energy release from the flare-induced signals? We select the X2.6 flare that occurred on 2005 January 15, for further study. The flare took place in NOAA active re-gion (AR) 10720 at approximately the central meridian, which makes the interpretation of the vector magnetograms less ambiguous. We have identified that flare-induced signals during this flare appeared in six zones. The zones are located within an average distance of 5 Mm from their weight center to the main magnetic neutral line, have an average size of (0.6±0.4)×1017 cm2, duration of 13±4 min, and flux density change of 181±125 G in the area of reversed polarity. The following new facts have been revealed by this study: (1) the flare-induced signal is also seen in the transverse magnetograms but with smaller magnitude, e.g., about 50 G; (2) the flare-induced signal mainly manifests itself as apparent polarity reversal, but the signal starts and ends as a weakening of flux density; (3) The flare-induced signals appear in phase with the peaks of hard X-ray emission as observed by the Ramaty High Energy Solar Spectroscopic lmager (RHESSI), and mostly trace the position of RHESSI hard X-ray footpoint sources. (4) in four zones, it takes place cotemporally with real magnetic changes which persist after the flare. Only for the other two zones does the flux density recover to the pre-flare level immediately after the flare.The physical implications of the flare-induced signal are discussed in view of its relevance to the non-thermal electron precipitation and primary energy release in the flare.     

Pressure dependence of viscosity of rhyolitic melts

Viscosity of silicate melts is a critical property for understanding volcanic and igneous processes in the Earth. We investigate the pressure effect on the viscosity of rhyolitic melts using two methods: indirect viscosity inference from hydrous species reaction in melts using a piston cylinder at pressures up to 2.8 GPa and direct viscosity measurement by parallel-plate creep viscometer in an internally-heated pressure vessel at pressures up to 0.4 GPa. Comparison of viscosities of a rhyolitic melt with 0.8 wt% water at 0.4 GPa shows that both methods give consistent results. In the indirect method, viscosities of hydrous rhyolitic melts were inferred based on the kinetics of hydrous species reaction in the melt upon cooling (i.e., the equivalence of rheologically defined glass transition temperature and chemically defined apparent equilibrium temperature). The cooling experiments were carried out in a piston-cylinder apparatus using hydrous rhyolitic samples with 0.8-4 wt% water. Cooling rates of the kinetic experiments varied from 0.1 K/s to 100 K/s; hence the range of viscosity inferred from this method covers 3 orders of magnitude. The data from this method show that viscosity increases with increasing pressure from 1 GPa to 3 GPa for hydrous rhyolitic melts with water content ?0.8 wt% in the high viscosity range. We also measured viscosity of rhyolitic melt with 0.13 wt% water using the parallel-plate viscometer at pressures 0.2 and 0.4 GPa in an internally-heated pressure vessel. The data show that viscosity of rhyolitic melt with 0.13 wt% water decreases with increasing pressure. Combining our new data with literature data, we develop a viscosity model of rhyolitic melts as a function of temperature, pressure and water content.