泥底辟/泥火山流体热效应及其对天然气水合物赋存的影响     

杨晓璐  钟思玲  万志峰 《海洋地质前沿》2018,(7)

泥底辟/泥火山流体热效应对天然气水合物赋存的影响是探索泥底辟/泥火山发育区水合物赋存规律的关键问题。笔者在分析总结国外泥底辟/泥火山流体热异常及其对天然气水合物赋存之影响的基础上,重点探讨了我国南海北部陆坡珠江口盆地神狐海域SH5站位未钻获水合物的原因及泥底辟/泥火山流体热效应对天然气水合物赋存的影响。当初寄予厚望的位于泥底辟之上的SH5站位未成功钻遇水合物的原因是晚期泥底辟刺穿水合物稳定带使深部高温流体沿着泥底辟和断裂通道上侵,该过程致使水合物稳定带温度场升高进而导致早期形成的水合物发生分解,因此,泥底辟/泥火山的流体热效应会直接制约水合物的赋存。探索泥底辟/泥火山流体热效应及其对水合物成藏的影响,不仅为丰富和完善流体渗漏构造环境下天然气水合物成藏动力学研究与勘探提供了热力学理论依据,而且对天然气水合物勘探开发及资源潜力评价等具有重要的指导意义。  相似文献   

Forearc ophiolite in Havana-Matanzas, Western Cuba: evidence from serpentinized mantle peridotite REE geochemistry and Cr-spinel composition     

LLANES CASTRO Angélica Isabel  PROENZA Joaquín Antonio  CRUZ GáMEZ Esther María 《《地质学报》英文版》2018,92(Z2):19-21

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特细水泥浆用于混凝土裂隙注浆的试验和应用     

Budel.  H 张伟 《探矿工程译丛》1996,(3):26-28

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东海进入赤潮高发期     

董立万 《海洋世界》2001,(10)

国家海洋局东海分局连连通告用海单位:密切注意赤潮动态,积极采取防范措施,尽量减少灾害损失! 东海正受到赤潮频频侵袭负责东海海洋环境保护的国家海洋局东海分局,根据其“中国海监”飞机和“中国海监”船近两个月来的巡航监视、监测报告,接连向东海区的海洋管理部门及用海单位发出《通报》。  相似文献   

5个新发现的X选BL Lac天体   总被引：1，自引：0，他引：1  

谢光中  茶光伟  白金明  张雄  Ｗ．Ｂｒｉｎｋｍａｎｎ 《中国天文和天体物理学报》1997,(3)

利用ＲＯＳＡＴＶＬＡ方法筛选，从ＲＯＳＡＴＸ射线源中选出了一批新的ＢＬＬａｃ天体和类星体的候选体．１９９６年１２月８日至１７日，利用北京天文台２．１６ｍ望远镜和新从美国引进的ＯＭＲ摄谱仪，对这批新候选体进行了光谱认证．经ＳＵＮ工作站处理，又发现了５个新的Ｘ选ＢＬＬａｃ天体．此外，还对去年作者在ＯＭＲ引进之前发现的ＢＬＬａｃ天体进行了检验，结果发现，去年发现的７个ＢＬＬａｃ天体中，２３２２＋３４３的ＣａＩＩＨ＆Ｋ“Ｂｒｅａｋｓｔｒｅｎｇｔｈ”为２６．９％，稍大于判据２５％，因此，２３２２＋３４３到底是ＢＬＬａｃ天体还是射电星系还有待于进一步测光及偏振观测的验证．  相似文献   

加拿大地盾板块构造和矿产资源     

Pouls.  H 陈铁华 《河南地质情报》1993,(3):33-35

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双管双动内钻头超前硬质合金钻具在复杂地层中的应用          下载免费PDF全文

万海田 《地质与勘探》1993,29(5):58-59

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用解析摄影测量仪器对SPOT图象的评价     

Konec.  G 曹垣平 《测绘译丛》1989,(5):22-29

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局部大地水准面的确定和与GPS结果的比较     

Denker  H 杨震岱 《测绘译丛》1989,(6):11-18,42

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Magnetic Field Strengths and Structures from Radio Observations of Solar Active Regions     

Chang－XiZhang  G.B.Gelfreikh 《中国天文和天体物理学报》2002,2(3):266-276

Radio observations of some active regions (ARs) obtained with the Nobeyama radioheliograph at λ=1.76cm are used for estimating the magnetic field strength in the upper chromosphere, based on thermal bremsstrahlung. The results are compared with the magnetic field strength in the photosphere from observations with the Solar Magnetic Field Telescope (SMFT) at Huairou Solar Observing Station of Beijing Astronomical Observatory. The difference in the magnetic field strength between the two layers seems reasonable. The solar radio maps of active regions obtained with the Nobeyama radioheliograph, both in total intensity (I-map) and in circular polarizations (V-map), are compared with the optical magnetograms obtained with the SMFT. The comparison between the radio map in circular polarization and the longitudinal photospheric magnetogram of a plage region suggest that the radio map in circular polarization is a kind of magnetogram of the upper chromosphere. The comparison of the radio map in total intensity with the photospheric vector magnetogram of an AR shows that the radio map in total intensity gives indications of magnetic loops in the corona, thus we have a method of defining the coronal magnetic structure from the radio I-maps at λ=1.76 cm. Analysing the I-maps, we identified three components: (a) a compact bright source; (b) a narrow elongated structure connecting two main magnetic islands of opposite polarities (observed in both the optical and radio magnetograms); (c) a wide, diffuse, weak component that corresponds to a wide structure in the solar active region which shows in most cases an S or a reversed S contour, which is probably due to the differential rotation of the Sun. The last two components suggest coronal loops on different spatial scales above the neutral line of the longitudinal photospheric magnetic field.  相似文献