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。     

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.     

无/缺水下地形数据的高原堰塞湖水量遥感估算

水量遥感动态监测对于高原堰塞湖风险评估、预报预警和处置决策等具有重要意义。针对高原无资料或缺资料区,充分利用空天遥感技术,文章提出了一种无/缺水下地形数据的高原堰塞湖水量遥感定量估算方法。该方法首先通过遥感水域面积提取,获取堰塞湖淹没空间范围;进而采用不规则复杂多边形中线定位算法,确定堰塞湖中心线位置;然后基于河道中心特定点高程信息,结合局部河道比降估算,生成堰塞湖水下地形河道中线约束因子;再根据河道边坡高程信息和水下地形约束因子自适应拟合出局部堰塞河道的水下未知地形;最后通过三维曲面离散积分实现堰塞湖水量遥感动态定量估算。实验以东帕米尔高原的萨雷兹堰塞湖为研究区,展开遥感水量调查与局部验证研究,结果表明:萨雷兹堰塞湖当前水域面积约为89.09 km²,水量约为162.49亿m³;这一结果与专家预估的水资源量155—165亿m³基本吻合。经局部模拟实验精度对比验证,模拟结果与实际数据动态误差总体控制在10%以内,相关系数达到0.95(P<0.01,双尾),进一步证明了算法的鲁棒性和估算结果的可信度。为无/缺水下地形数据的高原堰塞湖水量遥感估算提供了一种有效的方法,实现了水下地形未知的高原堰塞湖水量遥感快速反演与定量测算。     

MERSI和MODIS卫星监测京津冀及周边地区PM2.5浓度

京津冀及周边地区是中国PM_(2.5)污染最重的区域之一,利用卫星遥感技术监测大范围的PM_(2.5)时空分布变化是一种先进的重要手段。本研究首先基于暗像元算法利用FY-3B/MERSI与AQUA/MODIS对京津冀及周边区域进行了遥感AOT反演和验证分析;然后,引入气象资料和地面观测资料利用GWR模型反演了区域PM_(2.5)浓度,并对遥感反演结果进行了交叉验证评估,综合对比分析了MERSI和MODIS的气溶胶及PM_(2.5)遥感监测能力;最后,利用MERSI数据对2017年第一季度京津冀及周边区域的PM_(2.5)月均浓度时空分布变化情况进行了初步探索分析。结果表明:FY-3B/MERSI在气溶胶及PM_(2.5)遥感监测能力方面略优于AQUA/MODIS,MERSI反演的1 km分辨率AOT和PM_(2.5)与地面站点实测结果的决定系数R2分别为0.76μg/m~3和0.79μg/m~3,均方根误差分别为0.26μg/m~3和28μg/m~3,平均绝对误差分别为0.16μg/m~3和15μg/m~3,能基本满足对京津冀及周边区域PM_(2.5)的精细化监测需要。2017年第一季度京津冀及周边区域PM_(2.5)月均浓度遥感监测结果表明该区域的PM_(2.5)空间分布格局与地形地貌关系密切,高值区整体上沿太行山脉成带成片;从时间变化来看,1—3月呈逐月下降的趋势,其中3月份PM_(2.5)区域浓度较1月和2月有大幅下降。这说明FY-3\MERSI遥感反演产品能为环境质量监测和环境管理工作效果评估提供有效参考,本研究对国产卫星在大气环境遥感业务中的大力发展应用有重要参考意义。     

高速公路用地地籍调查方法和精度研究

介绍高速公路用地的权属调查和地籍测量方法,根据高速公路用地特点,重点讨论了确定高速公路地籍测量精度指标问题,得出高速公路宗地界址点精度统一采用&#177;0．3m比较适宜的结论。最后介绍了RTK技术在高速公路地籍测量的应用情况。