与1989年伊豆半岛近海地震和火山活动有关的水文和地球化学变化

我们对伊豆市一个温泉的水位，中伊豆的温泉水氡浓度以及伊豆－大岛火山喷发气体的温度变化进行了监测。在伊豆半岛东面近海１９８９年６月３０日地震和火山活动之前和活动时期，这些观测数据都发生了变化。本文将这些观测结果和其他报道的水文变化一加以概述，这些变化可以分成两种类型；一种是震群当中最大地震发生时震时变化，这种变化是在离Ｔｅｉｓｉ喷发中心２０－３０ＫＭ的几个温泉中观测到的。另一种是在靠近喷发中心地区和     

Some Aspects of the Characteristics of Monsoon Disturbances Using a Combined Barotropic－Baroclinic Model

ＳｏｍｅＡｓｐｅｃｔｓｏｆｔｈｅＣｈａｒａｃｔｅｒｉｓｔｉｃｓｏｆＭｏｎｓｏｏｎＤｉｓｔｕｒｂａｎｃｅｓＵｓｉｎｇａＣｏｍｂｉｎｅｄＢａｒｏｔｒｏｐｉｃ－ＢａｒｏｃｌｉｎｉｃＭｏｄｅｌ￥Ｎ．Ｒ．ＰａｒｉｊａａｎｄＳ．Ｋ．Ｄａｓｈ（ＣｅｎｔｒｅｆｏｒＡ...     

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     

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.