黄土高原东部夏半年降水稳定同位素特征及水汽来源分析

大气降水氢氧稳定同位素的组成可以指示降水过程的气候环境变化,分析大气降水稳定同位素的变化,对于研究气候条件下的水文循环过程具有重要意义。本文基于2019年夏半年（4—10月）黄土高原东部8个站点采集的152个降水样本的δ²H和δ¹⁸O的测定,系统分析δ²H和δ¹⁸O的时空分布特征及与气象参数、云下蒸发的关系,并利用HYSPLIT模型分析了水汽来源及运移路径。结果表明：① 研究区夏半年降水δ²H¹和δ¹⁸O存在显著的季节变化,其中5—7月逐渐富集、8—9月逐渐贫化;研究区降水δ²H和δ¹⁸O亦表现出显著的空间差异,整体上呈现由东南向西北逐渐增加的趋势。② 区域大气降水线的结果表明,该区整体上降水受云下蒸发作用较为显著,但位于盆地地区（赵城、阳泉、长治）降水过程受局地内循环影响较明显。③ 该区域降水中δ¹⁸O并未表现出显著温度效应和降水量效应,仅汾河谷地的介休站存在温度效应而介休、临汾站存在降雨量效应。④ 云下蒸发过程对太行山土石山区中部的阳泉站、北部的大同站以及汾河谷地的临汾站影响较为显著,其云底与地表降水的氢氧稳定同位素差异较显著。⑤ 水汽来源分析的结果显示,该区域夏季降水的主要来源为近地及东南方向下的渤海等地,远距离下的西方路径水汽含量占比较小。本文的结果对于增进区域水循环的认识及水资源的合理优化配置具有重要意义。     

三种方法测试岩溶水样氢氧同位素的对比研究

通过高温热转换元素-同位素比值质谱法（TC/EA-IRMS）、多用途气体制备仪-同位素比值质谱法（GasbenchⅡ-IRMS）以及激光光谱法对岩溶水样进行对比检测,其结果显示:对于氢同位素,TC/EA-IRMS的精密度达到0.3 ‰,激光光谱法的精密度达到0.1 ‰,均优于GasbenchⅡ-IRMS的精密度1.4 ‰;对于氧同位素,GasbenchⅡ-IRMS的精密度达到0.02 ‰,激光光谱法的精密度达到0.04 ‰,优于TC/EA-IRMS的精密度0.16 ‰。使用激光光谱法测定岩溶水样的氢氧同位素,所需要的样品量少,精密度高,能够满足岩溶区样品的高精度测试要求。      

Interaction of the supernova remnant HB3 with the ambient interstellar gas

The well-known shell supernova remnant (SNR) HB3 is part of a feature-rich star-forming region together with the nebulae W3, W4, and W5. We study the HI structure around this SNR using five RATAN-600 drift curves obtained at a wavelength of 21 cm with an angular resolution of 2′ in one coordinate over the radial-velocity range ?183 to +60 km s^?1 in a wider region of the sky and with a higher sensitivity than in previous works by other authors. The spatial-kinematic distribution of HI features around the SNR clearly shows two concentric expanding shells of gas that surround the SNR and coincide with it in all three coordinates (α, δ, and V). The outer shell has a radius of 133 pc, a thickness of 24 pc, and an expansion velocity of 48 km s^?1. The mass of the gas in it is ≈2.3 × 10⁵M_⊙. For the inner shell, these parameters are 78 pc, 36 pc, 24 km s^{? 1}, and 0.9 × 10⁵M_⊙, respectively. The inner shell is immediately adjacent to the SNR. Assuming that the outer shell was produced by the stellar wind and the inner shell arose from the shock wave of the SNR proper, we estimated the age of the outer shell, ≈1.7 × 10⁶ yr, and the mechanical luminosity of the stellar wind, 1.5 × 10³⁸ erg s^?1. The inner shell has an age of ≈10⁶ yr and corresponds to a total supernova explosion energy of ≈10⁵² erg.     

Stable isotopic evidence for fluid infiltration during contact metamorphism in a multiply-metamorphosed terrane: the Reynolds Range, Arunta Block, central Australia

The Lander Rock Beds form the local basement of the Reynolds Range in the Arunta Inlier of central Australia. These dominantly quartzose and pelitic lithologies underwent low-grade ( c.   400  °C) regional metamorphism prior to contact metamorphism ( c.   2.5  kbar) around S-type megacrystic granitoids at 1820–1800  Ma. The Lander Rock Beds are overlain by metasediments of the Reynolds Range Group, which were subsequently intruded by granitoids at c. 1780  Ma. Regional metamorphism at 1590–1580  Ma produced grades varying from greenschist (400  °C at 4–5  kbar) to granulite (750–800  °C at 4–5  kbar) from north-west to south-east along the length of the Reynolds Range. Oxygen isotope ratios of the Lander Rock Beds were reset from 13.4±0.8 to as low as 6.7 adjacent to the contacts of the larger plutons, and to 10.3±1.1 around the smaller plutons. Biotite in all the major rock types found in the aureoles has δD values between −52 and −69, probably reflecting resetting by a cooling igneous+metamorphic fluid near the plutons. Sapphirine-bearing and other Mg- and Al-rich rock types have low δ¹⁸O values (4.0±0.7). The precursors to these rocks were probably low-temperature ( c. 200  °C) diagenetic–hydrothermal deposits of Mg-rich chlorite, analogous to those in Proterozoic stratiform precious metal and uranium deposits that form by the infiltration of basin brines or seawater. As in the overlying Reynolds Range Group, regional metamorphism involved little fluid–rock interaction and isotopic resetting.     

Neutral hydrogen in nearby 3C radio galaxies

Observations of three nearby 3C radio galaxies, 3C430, 3C449, and 3C465, with the Nan?ay radio telescope (France) reveal for the first time the 21 cm absorption line of neutral hydrogen. The line is blue shifted by several hundred km/s in all three objects. This can probably be explained by an outflow of neutral hydrogen from the parent galaxies. Translated from Astrofizika, Vol. 51, No. 4, pp. 535–542 (November 2008).     

The structure of Galactic gas at high latitudes: The southern polar cap

We analyze the angular structure of the 21-cm interstellar neutral hydrogen emission at six and seven declinations in the northern (published previously) and southern polar caps of the Galaxy (Galactic latitudes from ?40° to ?90°), respectively, with an extent of 90° in right ascension. The RATAN-600 radio telescope has a beam width averaged over these regions of 2.′0×30′. One-dimensional power spectra for the angular distribution of interstellar neutral hydrogen emission were computed in each 6.3-km s^?1-wide spectral channel by using the standard Fast Fourier Transform (FFT) code and were smoothed over 1^h in right ascension. The Galactic latitude dependence of the mean parameters for the sky distribution of H I line emission at high latitudes was found to correspond to the distribution of gas in the form of a flat layer only in the northern region, while in the southern cap, the gas distribution is much less regular. In addition, the mean H I radial velocities are negative everywhere (?3.7±3.0 km s^?1 in the north and ?6.0±2.4 km s^?1 in the south). The power spectra of the angular fluctuations in the range of angular periods from 10′ to 6° appear as power laws. However, the spectral indices change greatly over the sky: from ?3 to ?1.2; on average, as the Galactic latitude increases and the H I column density decreases, the fluctuation spectrum of the interstellar gas emission becomes flatter. In the northern polar region, this behavior is much more pronounced, which probably stems from the fact that the gas column density in the south is generally a factor of 2 or 3 higher than that in the north. Therefore, the spectra are, on average, also steeper in the south, but the dependence on Galactic latitude is weaker. Using simulations, we show that the observed power-law spectrum of the H I emission distribution can be obtained in terms of not only a turbulent, but also a cloud model of interstellar gas if we use our previous spectra of the diameters and masses of H I clouds.     

Estimating apparent thermal diffusivity of soil using field temperature time series

Reliable estimates of soil thermal properties such as heat capacity, thermal conductivity, and diffusivity are important in analysis of heat transmission through soils in applications such as shallow geothermal applications, buried electrical conduits, and in general heat/fluid flow analyses. A number of analytical, numerical and experimental methods are available to determine the soil thermal properties. In this paper, the analytical and numerical methods developed on the basis of one-dimensional heat conduction equation are used to estimate the apparent thermal diffusivity of soil. Three of the four analytical methods, Amplitude, Phase, and Arctangent provide explicit equations for the apparent thermal diffusivity. Two methods, Harmonic and Numerical, make use of large number of temperature measurements to implicitly solve for the apparent thermal diffusivity. The temperature time series data monitored at different depths in two field sites in Melbourne, Australia for more than 2 year period were used to estimate the apparent thermal diffusivity of soil down to 2 m depth. The apparent thermal diffusivity was calculated using all five methods and compared with laboratory experimental results. The effectiveness of each method in predicting the thermal diffusivity was compared and observed discrepancies were discussed. Finally, the observed soil temperature data for a 12 month period are used to model the temperature variation in the ground analytically using Harmonic method and the model prediction for the following 12 month was compared independently with the field measurements. The analytical model prediction is found to be in good agreement with the field monitored data.     

激光同位素光谱法测量水中氢氧同位素组成的实验室间比对研究

激光同位素光谱分析方法是近些年使用较广泛的一种便捷、快速的测试稳定同位素组成的技术,能同时分析出水中δD、δ~(18)O同位素组成,因其操作简单,检测效率高,体积小,野外现场测试携带方便,迅速在环境、地质、生态和能源等领域得到广泛应用,但是该测试分析方法尚没有相应的国家标准,测试结果得不到有效的溯源,在使用过程中缺乏规范和统一。为此,本文通过在全国范围内12家实验室选取8个比对水样(δD值在-189.1‰~-0.4‰内,δ~(18)O值在-24.52‰~0.32‰内),利用激光同位素光谱法测试比对D/H和18O/16O值,探讨激光同位素光谱仪分析水中δD、δ~(18)O值的准确度和精密度。测试结果表明:各个协作实验室数据准确、稳定,方法的重复性和再现性良好;激光光谱法测定的δD精密度为0.4‰(1σ),δ~(18)O精密度为0.05‰(1σ),与传统稳定同位素质谱的精度几乎一致,因此适用于常规水样中δD、δ~(18)O测定,可以开展野外在线实时检测水中氢氧同位素组成。本研究为开展制定激光同位素光谱法测定环境液态水中δD、δ~(18)O同位素组成标准方法的工作推广和应用提供了参考。     

阿克苏断层氢气浓度动态特征及其映震效能

首先对阿克苏断层氢气浓度观测资料的周期成分进行了时频分析,然后分别利用线性回归和互相关方法分析了气温、气压与氢气浓度年周期成分的关系,并利用Molchan图表法对阿克苏断层氢气的映震效能进行了定量检验。结果显示:① 阿克苏断层氢气浓度具有清晰的年周期和半日周期成分;② 阿克苏断层氢气浓度的年周期动态变化与气温具有显著的正相关性,与气压的相关性一般,表明其年周期变化主要受气温影响;③ 阿克苏断层氢气浓度异常对观测点周边中强以上地震的反应较灵敏,映震效果较好。      

蜀南纳溪-合地区嘉陵江组天然气地球化学特征及其气源

通过分析纳溪—合江地区嘉陵江组天然气组分,碳、氢同位素组成以及该区烃源岩发育特征,认为嘉陵江组天然气为混源气,主要为下二叠统栖霞组—茅口组碳酸盐岩烃源岩生成的油型干气,混有下二叠统梁山组和上二叠统龙潭组生成的煤成气,下志留统龙马溪组泥质源岩可能也有贡献.研究区嘉陵江组烷烃气的氢同位素组成较重.纳溪气田烷烃气具有正常的碳...