云南水汞群体非均匀度异常与成组强震活动关系

阐述了一种前兆群体异常信息提取新方法前兆群体非均匀度的数学原理,并以云南水汞群体异常信息为例进行了具体计算。结果表明该方法以群体异常分布特征的变化为异常标准(ID≥1),达到异常即自动识别报警。该方法能克服个人经验的局限,易为他人进行检验,可成为本地区成组强震预测对应概率较高的新指标。     

影响黄土湿陷系数因素的分析

在工程地质勘察及土工试验资料的基础上，分析影响黄土湿陷性的主要因素，应用数理统计方法．系统研究了不同深度黄土湿陷系数随天然含水量和干密度的变化规律：黄土的湿陷系数δs随深度的增加而减小；天然含水量ω和干密度γd与黄土的湿陷系数δs均呈直线负相关关系。通过回归分析建立了黄土湿陷系数与其主要影响因素间的线性回归方程：δs=-0．00038ω-0．1022γd＋0-1839。     

空间数据库课程教学实践与思考

空间数据库课程是GIS专业的核心课程,对GIS人才培养具有非常重要的作用。但由于种种原因,空间数据库课程在课程体系、课程内容、教学模式等方面仍然存在许多问题和不足。本文首先分析了大学本科空间数据库课程在教学内容、实验与实习及教学手段等方面存在的问题,然后针对这些问题根据自己的教学体会提出了一些相应的解决办法与建议。     

Metals content in sediments of ephemeral streams with small reservoirs(the Negev Desert)

The content of 19 metals(chromium,cobalt,nickel,strontium,arsenic,magnesium,barium,cesium,gallium,rubidium,uranium,vanadium,zinc,lead,copper,cadmium,iron,manganese,and aluminum) in sediment in three ephemeral streams(Nahal Sansana,Nahal Revivim and Nahal Pura) with reservoirs in the Negev Desert is studied herein.The study was done in September 2016.The samples were collected from the surface layer of sediment(up to 10 cm) in the reservoirs and in the channels upstream and downstream of the reservoirs.Silt,which on average,accounted for 72% dominated in the sediment.In the spatial distribution of the particle size,sand and gravel fractions were deposited in the reservoirs.Aluminum,iron,and magnesium accounted for 99% of all analyzed metals.The Principal Component Analysis(PCA) and Hierarchical Cluster Analysis(HCA) showed that sediment in the Negev Desert channel upstream of the reservoirs had similar concentrations of metals.Similarities were also found between the analyzed reservoirs.The bottom sediment in reservoirs had higher concentrations of metals than sediment upstream and downstream of the reservoirs.The comparison of concentrations in upstream and downstream locations did not show any unambiguous trends because metal concentrations downstream from the reservoirs were not always lower than upstream of the reservoirs.The analysis of the sediment enrichment factor(EF) showed the highest value in the reservoirs and the lowest downstream of the reservoirs.The concentrations of most analyzed metals did not indicate the possibility of potential ecological risk(SQG).     

Early star formation and the evolution of the stellar initial mass function in galaxies

It has frequently been suggested in the literature that the stellar IMF in galaxies was top-heavy at early times. This would be plausible physically if the IMF depended on a mass-scale such as the Jeans mass that was higher at earlier times because of the generally higher temperatures that were present then. In this paper it is suggested, on the basis of current evidence and theory, that the IMF has a universal Salpeter-like form at the upper end, but flattens below a characteristic stellar mass that may vary with time. Much of the evidence that has been attributed to a top-heavy early IMF, including the ubiquitous G-dwarf problem, the high abundance of heavy elements in clusters of galaxies, and the high rate of formation of massive stars in high-redshift galaxies, can be accounted for with such an IMF if the characteristic stellar mass was several times higher during the early stages of galaxy evolution. However, significant variations in the mass-to-light ratios of galaxies and large amounts of dark matter in stellar remnants are not as easily explained in this way, because they require more extreme and less plausible assumptions about the form and variability of the IMF. Metal-free 'population III' stars are predicted to have an IMF that consists exclusively of massive stars, and they could help to account for some of the evidence that has been attributed to a top-heavy early IMF, as well as contributing importantly to the energetics and chemical enrichment of the early Universe.     

Dark haloes of spiral galaxies: ISO photometry

We exclude hydrogen-burning stars, of any mass above the hydrogen-burning limit and any metallicity, as significant contributors to the massive haloes deduced from rotation curves to dominate the outer parts of spiral galaxies. We present and analyse images of four nearly edge-on bulgeless spiral galaxies (UGC 711, NGC 2915, UGC 12426, UGC 1459) obtained with ISOCAM (The CAMera instrument on board the Infrared Space Observatory ) at 14.5 and 6.75 μm. Our sensitivity limit for detection of any diffuse infrared emission associated with the dark haloes in these galaxies is a few tens of μJy per 6 × 6 arcsec² pixel, with this limit currently set by remaining difficulties in modelling the non-linear behaviour of the detectors. All four galaxies show zero detected signal from extended non-disc emission, consistent with zero halo-like luminosity density distribution. The 95 per cent upper limit on any emission, for NGC 2915 in particular, allows us to exclude very low mass main-sequence stars ( M  > 0.08 M⊙) and young brown dwarfs (≲1 Gyr) as significant contributors to dark matter in galactic haloes. Combining our results with those of the Galactic microlensing surveys, which exclude objects with M  < 0.01 M⊙, excludes almost the entire possible mass range of compact baryonic objects from contributing to Galactic dark matter.     

A ROSAT survey of Wolf–Rayet galaxies — II. The extended sample

We present results from an ongoing X-ray survey of Wolf–Rayet (WR) galaxies, a class of objects believed to be very young starbursts. This paper extends the first X-ray survey of WR galaxies by Stevens &38; Strickland by studying WR galaxies identified subsequent to the original WR galaxy catalogue of Conti.   Out of a sample of 40 new WR galaxies a total of 10 have been observed with the ROSAT PSPC, and of these seven have been detected (NGC 1365, NGC 1569, I Zw 18, NGC 3353, NGC 4449, NGC 5408 and a marginal detection of NGC 2366). Of these, all are dwarf starbursts except for NGC 1365, which is a barred spiral galaxy possibly with an active nucleus. We also report on observations of the related emission-line galaxy IRAS 0833+6517.   The X-ray properties of these galaxies are broadly in line with those found for the original sample; they are X-ray overluminous compared with their blue luminosity and have thermal spectra with typically kT  ∼ 0.4 − 1.0 keV. There are some oddities: NGC 5408 is very overluminous in X-rays, even compared with other WR galaxies; I Zw 18 has a harder X-ray spectrum; NGC 1365, although thought to contain an active nucleus, has X-ray properties that are broadly similar to other WR galaxies, and we suggest that the X-ray emission from NGC 1365 is due to starburst activity.   A good correlation between X-ray and blue luminosity is found for the WR galaxy sample as a whole. However, when just dwarf galaxies are considered there is little evidence of correlation. We discuss the implications of these results on our understanding of the X-ray emission from WR galaxies and suggest that the best explanation for the X-ray activity is starburst activity from a young starburst region.     

IODINE CONTENT OF SARCASSUM IN SOUTHERN CHINA

SeaweedsareAnownas"elementaccUrnulabe",eSPeCiallyforiwhneandbrodrine.AiIgassumwasusedtoPreVntgoiterinancientChina.TheSpeCiesreconledinMQteriaMedica,SampsumthunbergiiandSampsum~lhaun,arewidelydistributedinNorth-ernChina.Chinesescientistsdetendnedtheiwhnecontentsinsomeseaweedsincludinghampsum(Jietal.,lwn).forumresoareesinSOuthernChinaaremoreabundantthanthoseintheNorth.MorethanoosPeCiesaremeOnledinliterathe.Mostspecieslist-edin"CommnSeaWeedsOfChina"(TSeng,l983)aresouthemsPeCies.Iwh…