GNSS多径反射探测海平面变化初探   总被引：1，自引：0，他引：1  

南阳  张双成  张勤  戴凯阳  李振宇 《测绘科学》2015,(12):125-129

随着GNSS研究与应用的不断深入,GNSS多径反射技术用于地表环境监测已成为一种新兴的遥感手段。针对目前国内对GNSS多径反射技术开展海平面变化探测研究较少的现状,该文通过分析信噪比值的变化特性,详细给出了基于信噪比观测值的GNSS多径反射技术探测海平面变化的基本原理。利用布设在美国华盛顿州Friday Harbor岸边的GPS连续运行跟踪站SC02观测数据反演了海平面变化,并与该站相距359m的Friday Harbor验潮站的监测数据进行了对比分析,误差均值为0.091m,相关系数为0.99。实验结果进一步验证了基于大地测量型GPS接收机用于海平面变化监测的有效性。  相似文献   

达州独立坐标系平面控制网测量方法探讨     

黄堰 《测绘与空间地理信息》2015,(11)

达州市独立坐标系GNSS网测量中,联测6个IGS参考站点,按B级网的要求解算出了4个控制点在CGCS2000椭球下的独立坐标,并将此作为GNSS控制网的起算数据对剩余23个GNSS控制点进行了平差处理,经过实例分析,该方法可以满足独立坐标系建立要求。  相似文献   

Radio emission at 1.4 GHz from luminous compact galaxies     

S. L. Parnovsky  I. Y. Izotova 《Astronomische Nachrichten》2015,336(3):276-283

We analyse the properties of the 1.4 GHz continuum emission in 52 star‐forming compact luminous galaxies (LCGs). The fluxes of the 1.4 GHz thermal (free‐free) component are derived from the extinction‐ and aperture‐corrected fluxes of the Hα emission line. The fraction of the thermal 1.4 GHz emission is shown tobe in the range of 2–52 % with a median value of about 15–17 %, and its distribution is close to a log‐normal one. Both the thermal and non‐thermal radio continuum luminosities are shown to be proportional to the masses of the young stellar population of the LCGs. We discuss the approximation of the ratio of the 1.4 GHz luminosity‐to‐the mass of the young stellar population as a function of starburst age. The derived approximation is shown to be similar but less clearly defined compared to ones obtained previously for LCGs from their Hα and UV continuum luminosities. (© 2015 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)  相似文献   

利用FY-3C气象卫星GNSS掩星估计全球重力波变化与分析     

金双根  高超  李君海 《南京气象学院学报》2020,12(1):57-67

大气重力波是地球大气层中广泛存在的重要大气动力学扰动,研究其分布和变化规律对理解大气物理、大气结构以及大气动力学等具有重要意义.传统大气重力波探测手段,如雷达和探空气球等,均存在探测时间短、有效探测高度低等缺点,全球卫星导航系统（GNSS）掩星观测具有全天候、低成本、高精度等优点,被广泛应用于地球大气探测和研究,为研究区域或全球重力波变化和活动特征提供了新的观测手段.本文利用中国第一颗搭载GNSS掩星设备气象卫星——风云3C （FY-3C）获得的掩星数据,反演得到2014年8月—2016年12月大气温度轮廓线,并首次估计重力波参数分布,分析了重力波参数的时空变化分布特征.结果表明,海陆季节性对流导致冬夏两季的重力波势能强于春秋两季,赤道对流作用导致赤道区域重力波强于两极,夏季南半球中低纬度地区重力波活动频繁,冬季北半球中低纬度区域重力波活动频繁.重力波随着高度的上升,势能逐渐下降.另外,地形是低层大气重力波的主要来源.  相似文献   

Precision measurement of cosmic magnification from 21-cm emitting galaxies     

Pengjie Zhang  Ue-Li Pen 《Monthly notices of the Royal Astronomical Society》2006,367(1):169-178

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Molecular line intensities as measures of cloud masses – I. Sensitivity of CO emissions to physical parameter variations     

T. A. Bell  E. Roueff  S. Viti  D. A. Williams 《Monthly notices of the Royal Astronomical Society》2006,371(4):1865-1872

A reliable estimate of the molecular gas content in galaxies plays a crucial role in determining their dynamical and star-forming properties. However, H₂, the dominant molecular species, is difficult to observe directly, particularly in the regions where most molecular gas is thought to reside. Its mass is therefore commonly inferred by assuming a direct proportionality with the integrated intensity of the  ¹²CO( J = 1 → 0)  emission line, using a CO-to-H₂ conversion factor, X . Although a canonical value for X is used extensively in such estimates, there is increasing evidence, both theoretical and observational, that the conversion factor may vary by over an order of magnitude under conditions different from those of the local neighbourhood. In an effort to understand the influence of changing environmental conditions on the conversion factor, we derive theoretical estimates of X for a wide range of physical parameters using a photon-dominated region (PDR) time-dependent chemical model, benchmarking key results against those of an independent PDR code to ensure reliability. Based on these results, the sensitivity of the X factor to change in each physical parameter is interpreted in terms of the chemistry and physical processes within the cloud. In addition to confirming previous observationally derived trends, we find that the time-dependence of the chemistry, often neglected in such models, has a considerable influence on the value of the conversion factor.  相似文献   

Six months of mass outflow and inclined rings in the ejecta of V1494 Aql     

S. P. S. Eyres  I. Heywood  T. J. O'Brien  R. J. Ivison  T. W. B. Muxlow  V. G. Elkin 《Monthly notices of the Royal Astronomical Society》2005,358(3):1019-1024

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A MERLIN survey of 4.7-GHz excited OH masers in star-forming regions     

L. Harvey-Smith  R. J. Cohen 《Monthly notices of the Royal Astronomical Society》2005,356(2):637-646

Phase-referenced observations of 13 star-forming regions in the  ²Π_1/2, J = 1/2  transition of rotationally excited OH at 4765 MHz have been carried out using MERLIN. Two of the regions were also observed at 4750 MHz and one at 4660 MHz. There were 10 maser detections at 4765 MHz and three non-detections. There were no detections at 4750 and 4660 MHz. The 4765-MHz masers have brightness temperatures of  ∼10⁷ K  at MERLIN resolution (∼50 mas). Several cases of 4765-MHz masers overlapping in position and velocity with 1720- and 1665-MHz masers are reported. There are also isolated 4765-MHz masers with peak flux densities ≥30 times that of any ground-state counterpart. Most of the 4.7-GHz maser spots are unresolved at 50-mas angular resolution, but in four of the nearest sources the maser spots are resolved, indicating a characteristic size for 4765-MHz maser regions of ∼100 au. In W3(OH) we discovered that 20 per cent of the 4765-MHz emission comes from a narrow low-brightness filament that stretches north–south for ∼1.0 arcec (∼2200 au) between two previously known 4765-MHz maser spots. The filament appears in projection against the H  ii region and has a brightness temperature of  ∼4 × 10⁵ K  . There are matching absorption features in mainline transitions of highly excited OH. The filament may trace a shock front in a rotating disc.  相似文献   

Dense Gas Diagnostics: Maser Excitation and Variability     

Malcolm Gray 《Astrophysics and Space Science》2005,295(1-2):309-318

I review a number of diagnostic techniques, based upon the excitation and variability of astrophysical masers, which can be applied to dense gas. In each case, I consider the observations necessary and the amount of interpretation, or modelling, required to complete the analysis of a source, presenting examples of each diagnostic method.  相似文献   

On the origin of the wide HI absorption line towards Sgr A*     

K. S. Dwarakanath  W. M. Goss  J. H. Zhao  C. C. Lang 《Journal of Astrophysics and Astronomy》2004,25(3-4):129-141

We have imaged a region of ∼ 5′ extent surrounding Sgr A* in the HI 21 cm-line absorption using the Very Large Array. A Gaussian decomposition of the optical depth spectra at positions within ∼ 2′ (∼ 5 pc at 8.5 kpc) of Sgr A* detects a wide line underlying the many narrow absorption lines. The wide line has a mean peak optical depth of 0.32 ± 0.12 centered at a mean velocity of V_1sr = −4 ± 15 km s{−1}. The mean full width at half maximum is 119 ± 42 km s⁻¹. Such a wide line is absent in the spectra at positions beyond ∼ 2′ from Sgr A*. The position-velocity diagrams in optical depth reveal that the wide line originates in various components of the circumnuclear disk (radius ∼ 1.3′ ) surrounding Sgr A*. These components contribute to the optical depth of the wide line in different velocity ranges. The position-velocity diagrams do not reveal any diffuse feature which could be attributed to a large number of HI clouds along the line of sight to Sgr A*. Consequently, the wide line has no implications either to a global population of shocked HI clouds in the Galaxy or to the energetics of the interstellar medium as was earlier thought.  相似文献