Gamma-ray bursts and their links with supernovae and cosmology     

Peter Meszairos  Neil Gehrels 《天体物理学报》2012,(8):1139-1161

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怀4井气体取样对水位观测干扰的解决措施     

张帆  宋晓煜  陈其峰  王锐锋  王志敏  程德庆 《地震地磁观测与研究》2021,42(5):158-165

怀4井水位观测一直存在取气样所造成的干扰,其表现为水位分钟值曲线每天出现有规律的向上脉冲式突跳且持续时间较长,这使得数据连续率及完整率降低。为改变怀4井长期存在的取气样影响水位观测的现状,减少水位观测数据突跳次数,提高观测质量精度,针对取气样方式进行改进,采用球胆排水真空脱气法进行溶解气样品的采集与脱气,避开直接在泄流口采样时的压力效应,从而解决了水位观测中遇到的实际问题。  相似文献   

论与核电厂址安全有关的自然灾害调查——以福建长乐漳港仙岐显应宫遗址埋没原因调查为例     

鄢家全  游良斌  吴健  郝玉芹 《震灾防御技术》2007,2(1):25-31

本文以福建长乐显应宫遗址埋没原因调查为例,论述了对于可能影响核电站厂址安全的自然灾害,开展调查评价的技术思路和内容。希望对类似灾害的调查评价有所帮助。  相似文献   

煤的吸附性能及影响因素   总被引：22，自引：0，他引：22  

钟玲文 《地球科学》2004,29(3):327-332,368

为了研究煤的储气性能,笔者对124个煤样进行等温吸附试验、煤岩测试、工业分析、压汞试验和低温液氮测试．研究表明：(1)煤变质对煤吸附能力具有控制作用,反射率从0．3％～4．25％,可燃基的Langmuir体积是11．25～47．16cm^2／g;(2)平衡水煤样吸附量与镜质组含量呈正相关、与惰质组含量呈负相关、与孔隙比表面积、微孔比表面积、微孔孔体积呈正相关;(3)水分、温度对煤的吸附能力有负面影响．煤变质程度不同,吸附曲线的变化趋势不同：气煤随着温度和压力增加吸附量一直增大,说明压力的影响起主导作用;无烟煤在温度小于60℃、压力小于15MPa之前,随着温度和压力同时增加吸附量增大,说明压力的影响起主导作用,之后,吸附量减小,说明温度的影响大于压力的影响。  相似文献   

基于GIS技术的"数字油田"建设与应用   总被引：2，自引：0，他引：2  

毛锋  艾丽双  何生厚 《地理信息世界》2004,2(1):34-38

石油石化工业是我国的支柱能源工业,石油石化企业的信息化不仅需求迫切,且因其研究对象是地下流动的物体而变得极其复杂：油田是其企业的主体和利润的主要来源,“数字油田”的建设是石油石化企业信息化成功的关键,由于油田一般空间跨度大、地上地下资料多而复杂,GIS技术是“数字油田”建设的关键技术;现主要介绍基于GIS技术建设“数字油田”的技术、方法和应用。  相似文献   

成藏过程对天然气地球化学特征的控制作用   总被引：3，自引：0，他引：3  

赵孟军  潘文庆  张水昌  韩剑发 《沉积学报》2004,22(4):683-688

克拉2和阿克1天然气都具有组分明显偏干、碳同位素明显偏重的特征,如克拉2和阿克1天然气的干燥系数都接近于1.0,克拉2天然气的δ13C₁为-27.3‰～-31.1‰,阿克1天然气的δ13C₁为-21.9‰～-25.2‰,从“源控”的角度似乎这些天然气应该属于过成熟煤成气,这样计算所得到的天然气成熟度远大于实测和模拟计算的源岩成熟度。因此在解释克拉2和阿克1天然气数据的时候,除了“源控”的因素外,更应强调成藏过程的影响。分析认为晚期阶段聚气是造成克拉2和阿克1天然气都具有组分明显偏干、碳同位素明显偏重的主要因素。  相似文献   

Carbon and Noble Gas Isotopes in the Tengchong Volcanic Geothermal Area, Yunnan, Southwestern China   总被引：1，自引：0，他引：1  

Shun''ichi NAKAI  Hiroshi WAKITA 《《地质学报》英文版》2004,78(5):1122-1135

Carbon and noble gas isotope analyses are reported for bubbling gas samples from the Tengchong volcanic geothermal area near the Indo-Eurasian suture zone. All samples contain a resolvable component of mantle-derived 3He. Occurrence of mantle-derived 3He coincides with surface volcanism. However, 3He occurs over a larger geographic areathan do surface volcanics. δ13C values for CO2 and CH4 vary from -33.4‰ to 1.6 ‰ and from -52.8‰ to -2.8‰, respectively. He and C isotope systematics indicate that CO2 and CH4 in the CO2-rich gases originated predominantly from magmatic component mixed with crustal CO2 produced from carbonate. However, breakdown of organic matter and near-surface processes accounts for the CH4 and CO2 in N2-rich gases. 3He/4He ratio distribution pattern suggests that mantle-derived He and heat sources of high-temperature system in central Tengchong originate from a hidden magma reservoir at subsurface. CO2-rich gases with the highest 3He/4He ratio (5.2 Ra) may be representative of the  相似文献   

中国冰川积累与水汽来源补给分析   总被引：9，自引：4，他引：5  

张忠林  何元庆  庞洪喜  卢爱刚  顾娟 《冰川冻土》2004,26(6):729-735

利用冰川编目数据和NCEP/NCAR再分析资料, 对中国及周边地区水汽通量、中国冰川地理分布情况、大气环流途径和降水分布进行分析, 发现中国冰川水汽来源复杂, 不同地区各季节存在不同的大气环流控制. 这说明不同地理位置的冰川所指示的气候信息是不同的, 大约以30° N和100° E为界, 中国西北部主要受西风环流影响, 冰川发育的水汽主要源于西风环流. 以横断山脉为界, 横断山脉以西, 即30° N以南和100° E以西的区域, 主要受印度季风控制, 冰川发育水汽主要源于印度洋、阿拉伯海和孟加拉湾; 横断山脉以东区域, 受东亚季风控制, 冰川发育水汽主要来源于太平洋和南海; 横断山脉、念青唐古拉和青藏高原东部地区受印度季风和东亚季风共同控制, 冰川发育水汽主要来源于孟加拉湾和南海. 不同地区冰芯积累量的变化与该地区夏季季风环流指数的变化具有较好的一致性.  相似文献   

Ion and neutral sources and sinks within Saturn's inner magnetosphere: Cassini results     

E.C. Sittler Jr.  N. Andre  M. Burger  A. Coates  D. Reisenfeld  A. Persoon  H.T. Smith  R.E. Hartle  M.D. Shappirio  D.J. McComas 《Planetary and Space Science》2008,56(1):3-18

Using ion-electron fluid parameters derived from Cassini Plasma Spectrometer (CAPS) observations within Saturn's inner magnetosphere as presented in Sittler et al. [2006a. Cassini observations of Saturn's inner plasmasphere: Saturn orbit insertion results. Planet. Space Sci., 54, 1197-1210], one can estimate the ion total flux tube content, N_IONL², for protons, H⁺, and water group ions, W⁺, as a function of radial distance or dipole L shell. In Sittler et al. [2005. Preliminary results on Saturn's inner plasmasphere as observed by Cassini: comparison with Voyager. Geophys. Res. Lett. 32(14), L14S04), it was shown that protons and water group ions dominated the plasmasphere composition. Using the ion-electron fluid parameters as boundary condition for each L shell traversed by the Cassini spacecraft, we self-consistently solve for the ambipolar electric field and the ion distribution along each of those field lines. Temperature anisotropies from Voyager plasma observations are used with (T_⊥/T_∥)_W⁺∼5 and (T_⊥/T_∥)_H⁺∼2. The radio and plasma wave science (RPWS) electron density observations from previous publications are used to indirectly confirm usage of the above temperature anisotropies for water group ions and protons. In the case of electrons we assume they are isotropic due to their short scattering time scales. When the above is done, our calculation show N_IONL² for H⁺ and W⁺ peaking near Dione's L shell with values similar to that found from Voyager plasma observations. We are able to show that water molecules are the dominant source of ions within Saturn's inner magnetosphere. We estimate the ion production rate S_ION∼10²⁷ ions/s as function of dipole L using N_H⁺, N_W⁺ and the time scale for ion loss due to radial transport τ_D and ion-electron recombination τ_REC. The ion production shows localized peaks near the L shells of Tethys, Dione and Rhea, but not Enceladus. We then estimate the neutral production rate, S_W, from our ion production rate, S_ION, and the time scale for loss of neutrals by ionization, τ_ION, and charge exchange, τ_CH. The estimated source rate for water molecules shows a pronounced peak near Enceladus’ L shell L∼4, with a value S_W∼2×10²⁸ mol/s.  相似文献   

The pressure of an equilibrium interstellar medium in galactic disks     

A. V. Kasparova  A. V. Zasov 《Astronomy Letters》2008,34(3):152-162

Based on an axisymmetric galactic disk model, we estimate the equilibrium gas pressure P/k in the disk plane as a function of the galactocentric distance R for several galaxies (MW, M33, M51, M81, M100, M101, M106, and the SMC). For this purpose, we solve a self-consistent system of equations by taking into account the gas self-gravity and the presence of a dark pseudo-isothermal halo. We assume that the turbulent velocity dispersions of the atomic and molecular gases are fixed and that the velocity dispersion of the old stellar disk corresponds to its marginal stability (except for the Galaxy and the SMC). We also consider a model with a constant disk thickness. Of the listed galaxies, the SMC and M51 have the highest pressure at a given relative radius R/R ₂₅, while M81 and the Galaxy has the lowest pressure. The pressure dependence of the relative molecular gas fraction confirms the existence of a positive correlation between these quantities, but it is not so distinct as that obtained previously when the pressure was estimated very roughly. This dependence breaks down for the inner regions of M81 and M106, probably because the gas pressure has been underestimated in the bulge region. We discuss the possible effects of factors other than the pressure affecting the relative content of the molecular gas in the galaxies under consideration.  相似文献