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Inference of surface concentrations of nitrogen dioxide (NO2) in Colombia from tropospheric columns of the ozone measurement instrument (OMI)

For the first time, maps of surface concentration of nitrogen dioxide (NO₂) are presented for the Colombian territory. NO₂ surface concentrations for the year 2007 are inferred based on two sources of tropospheric NO₂ column data: (1) a simulation using a three-dimensional global model (GEOS-Chem) and (2) measurements made by the ozone monitoring instrument (OMI) onboard the NASA Aura satellite. Results show monthly averages between 0.1 and 6 ppbv. We compare these inferred values to corrected ground measurements of NO₂. We find correlation coefficients of up to 0.91 between the inferred data and the corrected observational data. A significant source of NO₂ is biomass burning, which can be diagnosed by data of fire radiative power (FRP) from the Monitoring of Atmospheric Composition and Climate (MACC) reanalysis. We find a close relationship between high values of inferred NO₂ surface concentrations and biomass burning for a large area which encompasses the departments of Caquetá, Meta, Guaviare, Vichada, and Putumayo.     

对流层大气温度"蝴蝶形"震前异常

利用美国国家和海洋大气管理局(NOAA)的大气温度数据, 分析陆地地震和海洋地震震前震中上空的大气温度变化, 研究其作为地震短临前兆的可能性.地震样本包括2014年2月12日于田M_s7.3地震、2008年5月12日汶川M_s8.0地震、2011年3月11日日本M_s9.0地震、2014年4月1日智利M_s8.1海洋地震、2013年3月27日台湾南投县M_s6.1地震和2014年5月30日云南盈江M_s6.1地震.结果表明: (1)震前, 震中位置300~1 000 hPa大气温度有较为一致的变化趋势; (2)200 hPa与400 hPa处(根据不同地点可选择其他, 诸如350 hPa、300 hPa等高度数据)温度折线图在震前趋近或者相交, 出现类似蝴蝶翅膀的"蝴蝶形"特殊曲线形状; (3)200 hPa与400 hPa温度差等值线图在(震前数月、数周或数天不等)震中附近区域的数值减小, 温度差等值线图的塌陷最低点对应震中位置.以上规律有望应用于地震短临预测的时间与震中的确定.      

亚洲地区EGNOS天顶对流层延迟模型单站修正与精度分析

以亚洲地区46个IGS站2008-2011年实测的高精度天顶对流层延迟（ZTD）数据为参考值,通过对2008-2010年EGNOS模型计算ZTD的日均偏差进行频谱分析,建立了亚洲地区EGNOS模型的单站修正模型（SSIEGNOS）,对EGNOS和SSIEGNOS模型在亚洲地区的精度和适用情况进行了评估,结果表明：（1）EGNOS模型偏差和RMS在时间分布上呈现明显的季节变化规律,而SSIEGNOS模型偏差和RMS变化较小且平稳;（2）在空间分布上,两种模型的偏差随着经纬度和高程的变化均无明显规律,但随着高程或者纬度的增加RMS总体上都有递减的趋势;（3）SSIEGNOS模型预测ZTD的精度相对于EGNOS模型有明显提高。     

COMPASS三频数据线性组合优化选取分析

以北斗卫星1支路频点为例,从消除或减弱电离层影响、对流层影响和观测噪声与多路径误差3个方面分析COMPASS三频数据线性组合的优化选取问题,并通过MATLAB模拟,给出一些典型的组合,分析它们可能的应用,为COMPASS三频数据线性组合的优化选取提供一些借鉴。     

基于再分析资料ERA5的对流层延迟估计方法及精度评估

提出基于再分析资料ERA5的天顶对流层延迟计算方法,使用中国大陆构造环境监测网络提供的26个GNSS测站2017年全年数据,评估由该方法计算的天顶对流层延迟的精度,并与前一代再分析资料ERA-Interim的计算结果进行对比分析。结果显示,ERA5计算的天顶对流层延迟均方根误差比ERA-Interim计算结果低,表明新一代产品的精度有明显提升。     

W3(OH)致密HⅡ区磁场研究

本文以W3(OH)为实例,建立了与OH脉泽成协的HII区气体-尘埃壳层的磁场模型,由此可见,致密HII区所在分子云核心中的磁场强度,与分子云核心的分子数密度之间存在指数α=1/2的幂律关系;而在HII区气体-尘埃壳层中,磁场强度与分子数密度之间存在α=1的正比关系,根据讨论可知,与OH脉泽成协的HII区,其气体-尘埃壳层的分子数密度为10~6cm~(-3)量级,磁场强度为几个mG;一旦分子数密度达10~7cm~(-3)量级,OH脉泽便将熄灭。     

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

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.     

The brightest OH maser in the sky: A flare of emission in W75 N

A flare of maser radio emission in the 1665-MHz OH line with a flux density of about 1000 Jy was discovered in the star-forming region W75 N in 2003. At the time of its observations, it was the strongest OH maser in the entire history of research since the discovery of cosmic OH masers in 1965. The linear polarization of the flare emission reached 100%. A weaker flare with a flux density of 145 Jy was observed in this source in 2000–2001; this was probably a precursor of the intense flare. The intensity of two other spectral features decreased when the flare emerged. This change in the intensity of the emission from maser condensations (a brightening of some of them and a weakening of others) can be explained by the passage of a magnetohydrodynamic shock through regions of enhanced gas concentration.