Detection of a new interstellar molecular ion, H2COH+ (protonated formaldehyde)

A new interstellar molecular ion, H2COH+ (protonated formaldehyde), has been detected toward Sgr B2, Orion KL, W51, and possibly in NGC 7538 and DR21(OH). Six transitions were detected in Sgr B2(M). The 1(1,0)-1(0,1) transition was detected in all sources listed above. Searches were also made toward the cold, dark clouds TMC-1 and L134N, Orion (3N, 1E), and a red giant, IRC + 10216, without success. The excitation temperatures of H2COH+ are calculated to be 60-110 K, and the column densities are on the order of 10(12)-10(14) cm-2 in Sgr B2, Orion KL, and W51. The fractional abundance of H2COH+ is on the order of 10(-11) to 10-(9), and the ratio of H2COH+ to H2CO is in the range 0.001-0.5 in these objects. The values in Orion KL seem to be consistent with the "early time" values of recent model calculations by Lee, Bettens, & Herbst, but they appear to be higher than the model values in Sgr B2 and W51 even if we take the large uncertainties of column densities of H2CO into account. We suggest production routes starting from CH3OH may play an important role in the formation of H2COH+.     

ASCA Observation of the Quiescent X-Ray Counterpart to SGR 1627-41

We present a 2-10 keV ASCA observation of the field around the soft gamma repeater SGR 1627-41. A quiescent X-ray source, whose position is consistent both with that of a recently discovered BeppoSAX X-ray source and with the Interplanetary Network localization for this soft gamma repeater, was detected in this observation. In 2-10 keV X-rays, the spectrum of the X-ray source may be fit equally well by a power-law, blackbody, or bremsstrahlung function, with unabsorbed flux approximately 5x10-12 ergs cm-2 s-1. We do not confirm a continuation of a fading trend in the flux, and we find no evidence for periodicity, both of which were noted in the earlier BeppoSAX observations.     

Results of TV imaging of Phobos (Experiment VSK-Fregat)

From February to March 1989 the Phobos 2 spacecraft took 37 TV images of Phobos at a distance of 190-1100 km. These images complement Mariner-9 and Viking data by providing higher-resolution coverage of a large region West of the crater Stickney (40-160 degrees W) and by providing disk-resolved measurements of surface brightness at a greater range of wavelengths and additional phase angles. These images have supported updated mapping and characterization of large craters and grooves, and have provided additional observations of craters' and grooves' bright rims. Variations in surface visible/near-infrared color ratio of almost a factor of 2 have been recognized; these variations appear to be associated with the ejecta of specific large impact craters. Updated determinations of satellite mass and volume allow calculation of a more accurate value of bulk density, 1.90 +/- 0.1 g cm-3. This is significantly lower than the density of meteoritic analogs to Phobos' surface, suggesting a porous interior perhaps containing interstitial ice.     

Methodology for the diagnostics of soil polygenesis on the basis of macro- and micromorphological studies

A methodology for studying soil polygenesis and lithological homogeneity of soil profiles is suggested. This methodology is particularly important for mountain soils, where the lithological heterogeneity of the soil profiles created by denudation and accumulation processes is often observed. The methodology includes several stages： （a） the study of the lithological homogeneity/ heterogeneity of soil profiles by field and laboratory methods, （b） the stage-by-stage macro-, meso-, micro-, and submicromorphological analyses of soil profiles with additional use of the methods of neighboring sciences, and （e） the subdivision of soil features into the groups of recent and inherited （relict） features. In the latter group, the subgroups of lithorelict features inherited from the parent material and pedorelict features inherited from the previous stages of soil formation can be distinguished. Two major models of soil polygenesis are suggested. Simple models describe the soils, in which new features appear due to the changes in the environmental conditions in the course of soil evolution. Complex models describe the soils, in which such changes are combined with deposition of new portions of sediments onto the soil surface with the development of buried soil horizons （the synlithogenie pedogenesis）. The models of continuous and discontinuous synlithogenic pedogenesis can be further distinguished. It is argued that the micromorphological method applied to the studies on soil mierofabrics, microforms of soil humus, soil porosity, coatings, and various pedo- and lithorelict features yields valuable information on polygenetic soils.     

First astronomical detection of the cumulene carbon chain molecule H2C6 in TMC-1

The cumulene carbenes are important components of hydrocarbon chemistry in low-mass star-forming cores. Here we report the first astronomical detection of the long-chain cumulene carbene H2C6 in the interstellar cloud TMC-1, from observations of two of its rotational transitions: J(K,K') = 7(1,7) --> 6(1,6) at 18.8 GHz and 8(1,8) --> 7(1,7) at 21.5 GHz, using NASA's Deep Space Network 70 m antenna at Goldstone, California. In addition we also observed the shorter cumulene carbene H2C4 at the same position. The fractional abundance of H2C6 relative to H2 is about 4.7 x 10(-11) and that of H2C4 is about 4.1 x 10(-9). The abundance of H2C6 is in fairly good agreement with gas-phase chemical models for young molecular cloud cores, but the abundance of H2C4 is significantly larger than predicted.     

中非东部Kibaran带的地球动力学演化

位于中非东部的Kibaran带被解释为大约在1400～950Ma期间发育的碰撞带。碰撞带演化不同阶段的岩浆特征解释如下: 1.大陆裂谷作用阶段(>1400Ma),在东部扎伊尔下Kibaran单元,角闪岩与大陆拉斑玄武岩质的和碱性同源的麻粒岩互层为特征(Shaba,未公布资料;Kivu,参考资料1)。     

英国气象的未来十年(续)

四、主要业务活动在第2.1节中我已谈到了气象局观测资料的收集、全球通信、制作全球范围预报的计算机模式等方面的主要业务活动。在这一部分我将谈谈这些活动的各个组成部分。1.观测和仪器设备不仅全球模式需要全球资料,而且有限区域预报模式的边界条件的建立也需要(如英国区域内)。因此,全球资料的收集和交换系统对于任何预报的成功与否是至关重要的。有必     

对于全球规模的地球构造我们知道多少？

最近5-6年主要由于高质数字地震资料而使得对地球内部构造的了解有了很大的进展。应用地球体波、面波及自由振荡的各种研究阐明了不同深度上的三维构造。然而,任何构造研究都受到对用于探测构造的波长分辨力问题的限制。在这方面,比如由体波得到的模式代表着由面波或自由振荡获得的那些不同尺度的平均值,它应包括了更详细的结果。不过我们经常发现对于各种结果的解释就象它们给出的是对三维地球中地震速度进行的点估计。本文中我们回顾每种类型资料是如何提供给我们有关地球构造的信息以及如何依据其分辨力与误差进行解释。三维构造研究中出现的最明显的特点之一即为与地表地质相对应的近地表速度的变