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     

不同层序岩相中的不稳定带和岩石的特征变化

盆地形成的原因包括；构造圈深部地带物质的不稳定状态、软流圈厚度的增加和继而地壳厚度的减小。大多数沉积盆地均有一些高能不稳定层，反映了岩石特征的非线性交换。在不同岩石类型的不同深度，密度、孔隙度、水饱和度等的异常均不相同。决定异常存在的主要作用是岩石的构造一组分特征和导热性、导电性。采用与深度和ＰＴ因子一致的温度计算法来建立不同岩石类型和不同地球动力条件和热力条件下岩石特征变化的计算机模型或许是重要的。密度、孔隙度等的非线性变化决定了不同流体循环的环型流动的存在，不稳定层的预测是矿产预测之关键。     

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.     

中尺度预报

许多作者（Browning1980；Doswell1986；Austin等1987）都提出过图1，该图表示各种预报方法对于作为预报提前时间函数的预报过程的相对重要性。标有“大尺度模式”的曲线表示传统预报，它做出的预报，事实上是一般性的预报，而且尽管它也能用主观解释或用模式输出统计方法给出具体地．大和参数的预报，但这样的预报大多只适用于12小时以上的时效。中尺度预报的研究内容涉及从0—12小时时效，使用的是线性对叫江法、中尺度模式、气候学方法和图1中称为“气象学知识”的方法。下面各小节依次考察这些方法。（1）节讨论观测到中尺度特征的几…     

Raman Spectroscopy of Garnet—group Minerals

The Raman spectra of the natural end members of the garnet-group minerals,which include pyrope, almandine and spessarite of Fe-Al garnet series and grossularite ,andradite and uvarovite of Ca-Fe garnet series, have been strdied.Measured Raman spectra of these minerals are reasonably and qualitatively assigned to the internal modes, translational and rotatory modes of SiO4 tetrahedra, as well as the translational motion of bivalent cations in the X site.The stretch and rotatory A1g modes for the Fe-Al garnet series show obvious Raman shifts as compared with those for the Ca-Fe garnet series ,owing to the cations residing in the Xsite connected with SiO4 tetrahedra by sharing the two edges.The Raman shifts of all members within either of the series are attributed mainly to the properties of cations in the X site for the Fe-Al garnet series andin the Y site for the Ca-Fe garnet series.