宝坻王4井水氡高值变化的原因探讨

天津市宝坻玉４井从１９８３年４月开始观测水氡，观测值相对稳定。１９９１年１０月２日该井水氡测值出现大于２７．０Ｂｑ／Ｌ的成丛高值突跳，最高值达５７．０Ｂｑ／Ｌ，为正常值的两倍多，水氡值由平稳型变为离散型，至今已两年多时间，高值出现后，天津地震局分析预报中心、监测中心先后组织人员到现场落实达２０多次，做了大量的调查研究和实验工作排除了有关干扰，认为王４井的水氡高值高化主要是附近王２井长期抽水影响的结     

在石油渗透过程的模拟中单芳烃和双芳烃组分的变化

进行了原油在砂质－粉砂质岩石中渗透的模拟，研究了石油在岩石中的运移对单芳烃和双芳烃的系列组分及单一组分变化的影响。指出最终滤液中的积累的环烷酸盐转换化合物能反映在渗透时单芳烃和芳烃中撮大“残留物”。烷基苯中，Ｃ１９－Ｃ２７成分的高分子正烷基苯（Ｈ－烷基苯），１，２－和１，３－甲基烷苯在岩石中具有高的保留率。在相同成分的烷基萘中，２，６－，２，７－和１，７－二甲基萘最活跃。提出了计算石油经过岩石运移     

华北强震水化学参量变化的模糊识别及方法评价

利用模糊识别方法对１９６９￣１９９８年发生在华北地区的渤海,海城,唐山３次强震及其强余震以及大同,包头西,张北３次中强震之前,该地区５０多口观测井的水氡和部分井孔的Ｈｅ,Ｈ２,ＣＯ２,Ｈｇ等水化学组分８万多个观测数据进行了全面处理,取得了华北地区强震前水氡,气体和水质组分前兆变化的时空分布特征,并提出了该地区强震和中强地震水化学参量中期和短期的异常指标,最后对模糊识别方法的地震预报效能提出评价。     

Large-Scale Mapping Observations of the C i (3P1-3P0) and CO (J = 3-2) Lines toward the Orion A Molecular Cloud

Large-scale mapping observations of the 3P1-3P0 fine-structure transition of atomic carbon (C i, 492 GHz) and the J=3-2 transition of CO (346 GHz) toward the Orion A molecular cloud have been carried out with the Mount Fuji submillimeter-wave telescope. The observations cover 9 deg2 and include the Orion Nebula M42 and the L1641 dark cloud complex. The C i emission extends over almost the entire region of the Orion A cloud and is surprisingly similar to that of 13CO (J=1-0). The CO (J=3-2) emission shows a more featureless and extended distribution than C i. The C i/CO (J=3-2) integrated intensity ratio shows a spatial gradient running from the north (0.10) to the south (1.2) of the Orion A cloud, which we interpret as a consequence of the temperature gradient. On the other hand, the C i/13CO (J=1-0) intensity ratio shows no systematic gradient. We have found a good correlation between the C i and 13CO (J=1-0) intensities over the Orion A cloud. This result is discussed on the basis of photodissociation region models.     

TRACE and Yohkoh Observations of High-Temperature Plasma in a Two-Ribbon Limb Flare

The ability of the Transition Region and Coronal Explorer (TRACE) to image solar plasma over a wide range of temperatures (Te approximately 104-107 K) at high spatial resolution (0&farcs;5 pixels) makes it a unique instrument for observing solar flares. We present TRACE and Yohkoh observations of an M2.4 two-ribbon flare that began on 1999 July 25 at about 13:08 UT. We observe impulsive footpoint brightenings that are followed by the formation of high-temperature plasma (Te greater, similar10 MK) in the corona. After an interval of about 1300 s, cooler loops (Te<2 MK) form below the hot plasma. Thus, the evolution of the event supports the qualitative aspects of the standard reconnection model of solar flares. The TRACE and Yohkoh data show that the bulk of the flare emission is at or below 10 MK. The TRACE data are also consistent with the Yohkoh observations of hotter plasma (Te approximately 15-20 MK) existing at the top of the arcade. The cooling time inferred from these observations is consistent with a hybrid cooling time based on thermal conduction and radiative cooling.