Calculation of the Intensity Ratio and Intrinsic Redshift Ratio of the Cerenkov Iron Kα and Kβ Lines and Its Possible Application in the Study of AGNs

We have pointed out that, when thermal relativistic electrons with an isotropic velocity distribution move through a region of dense gas or impinge upon its surface, the Cerenkov effect will produce a particular kind of atomic or ionic emission line, which we have called the “Cerenkov line-like radiation”. This prediction for the optical wavebands has been verified by laboratory experiments. In this paper, we extend this line-like radiation theory to the X-ray waveband and give the basic formulae for calculating the intensity ratio and intrinsic redshift ratio of the Cerenkov iron K_α and K_β lines, for different ionization orders of iron. Potential application of this calculated result may be found in the study of AGNs. The recent observations of NGC3783 show that besides the iron K_α line at ∼6.4 keV, there is also a very strong iron Kβ line at ∼7.0 keV, and that the ratio of equivalent widths between the two is anomalous: EWK_α/EWK_β ≈ 3.43. It is difficult to explain this by the conventional mechanism of “photoelectric absorption-fluorescence emission”. We suggest that the mechanism of Cerenkov line-like radiation can provides a way of solving this puzzle. Besides, we expect that the calculated intrinsic redshift ratio of Cerenkov iron K_α and K_β lines could be tested in future observations. If our suggestion is further supported by observations, then our view on the physical environment around the central massive black hole of an AGN will be greatly modified: the activity becomes more energetic and violent, and the gas, much denser than previously thought.     

Detection of CO Outflow in Rotating Cores

We investigate the effect of bulk motion on the detection of molecular outflows in the sources S 146, GGD27, and IRAS 22566 5830. The traditional techniques do allow for bulk motions or systematic VLSR shifts of the core emissions, which may cause contamination of the high velocity gas emissions, and outflows may either fail to be detected or have their properties miscalculated. We used a program to follow the systematic shift of VLSR and better results have been obtained.     

The Effect of AGN and SNe Feedback on Star Formation, Reionization and the Near Infrared Background

Feedback from supernovae (SNe) and from active galactic nuclei (AGN) accom-panies the history of star formation and galaxy evolution. We present an analytic model to explain how and when the SNe and AGN exert their feedback effects on the star formation and galaxy evolution processes. By using SNe and AGN kinetic feedback mechanisms based on the Lambda Cold Dark Matter (LCDM) model, we explore how these feedback mecha-nisms affect the star formation history (SFH), the Near-Infrared Background (NIRB) flux and the cosmological reionization. We find the values of the feedback strengths, ∈AGN =1.0+0.50.3and ∈SN=0.04+0.02-0.02, can provide a reasonable explanation of most of the observational re-suits, and that the AGN feedback effect on star formation history is quite different from the SNe feedback at high redshifts. Our conclusions manifest quantitatively that these feedback effects decrease star formation rate density (SFRD) and the NIRB flux (in 1.4 - 4.0μm), and postpone the time of completion of the cosmological reionization.     

Static pressure of hot gas: Its effect on the gas disks of galaxies

The static pressure of the hot gas that fills clusters and groups of galaxies can affect significantly the volume density and thickness of the gas disks in galaxies. In combination with the dynamic pressure, the static pressure allows several observed peculiarities of spiral galaxies surrounded by a hot medium to be explained.     

三门组的内涵及其意义

黄河三门峡水库北岸的山西省平陆县黄底沟剖面 ,较完整地保存着古三门湖湖相沉积记录。经磁性地层研究结果表明 ,古三门湖沉积起始于吉尔伯特负极性时中期 ,大约在 5MaB .P .;结束于布容正极性时晚期 ,结合热释光年龄 ,大约在 1 5 0kaB .P .。鉴于这套地层均属古三门湖沉积地层 ,按照岩石地层学的命名原则 ,依然称之为三门组 ,并根据岩性特征自上而下划分为三段 :上段以砂层为主 ;中段以粘土层为主 ;下段为底砾石层。黄底沟剖面是已知的记录古三门湖发育起始时间最早、结束年代最晚的地层剖面     

The formation of the Oort cloud in open cluster environments

We study the influence of an open cluster environment on the formation and current structure of the Oort cloud. To do this, we have run 19 different simulations of the formation of the Oort cloud for 4.5 Gyrs. In each simulation, the Solar System spends its first 100 Myrs in a different open cluster environment before transitioning to its current field environment. We find that, compared to forming in the field environment, the inner Oort cloud is preferentially loaded with comets while the Sun resides in the open cluster and that most of this material remains locked in the interior of the cloud for the next 4.4 Gyrs. In addition, the outer Oort cloud trapping efficiencies we observe in our simulations are lower than previous formation models by about a factor of 2, possibly implying an even more massive early planetesimal disk. Furthermore, some of our simulations reproduce the orbits of observed extended scattered disk objects, which may serve as an observational constraint on the Sun's early environment. Depending on the particular open cluster environment, the properties of the inner Oort cloud and extended scattered disk can vary widely. On the other hand, the outer portions of the Oort cloud in each of our simulations are all similar.     

Core formation in giant gaseous protoplanets

Sedimentation rates of silicate grains in gas giant protoplanets formed by disk instability are calculated for protoplanetary masses between 1 MSaturn to 10 MJupiter. Giant protoplanets with masses of 5 MJupiter or larger are found to be too hot for grain sedimentation to form a silicate core. Smaller protoplanets are cold enough to allow grain settling and core formation. Grain sedimentation and core formation occur in the low mass protoplanets because of their slow contraction rate and low internal temperature. It is predicted that massive giant planets will not have cores, while smaller planets will have small rocky cores whose masses depend on the planetary mass, the amount of solids within the body, and the disk environment. The protoplanets are found to be too hot to allow the existence of icy grains, and therefore the cores are predicted not to contain any ices. It is suggested that the atmospheres of low mass giant planets are depleted in refractory elements compared with the atmospheres of more massive planets. These predictions provide a test of the disk instability model of gas giant planet formation. The core masses of Jupiter and Saturn were found to be ∼0.25 M_⊕ and ∼0.5 M_⊕, respectively. The core masses of Jupiter and Saturn can be substantially larger if planetesimal accretion is included. The final core mass will depend on planetesimal size, the time at which planetesimals are formed, and the size distribution of the material added to the protoplanet. Jupiter's core mass can vary from 2 to 12 M_⊕. Saturn's core mass is found to be ∼8 M_⊕.     

季节性Kendall检验及其在三门峡水库水质趋势分析中的应用

选择1997—2002年三门峡库区的龙门、潼关和三门峡3个断面的水质监测资料,运用季节性Kendall检验方法分析三门峡水库水质趋势,结果显示：龙门断面,CODMn、NO2-N及Hg的变化趋势不明显,NH3-N呈显著上升趋势,As、Cd和Cu呈显著下降趋势,而Pb则呈高度显著下降趋势;潼关断面,NH3-N、NO2-N和Hg的变化趋势不明显,CODMn呈显著上升趋势,As、Cd和Pb呈显著下降趋势,而Cu则呈高度显著下降趋势;三门峡断面,CODMn、NO2-N、As及Hg的变化趋势不明显,NH3-N污染呈显著上升趋势,Cd呈显著下降趋势,而Cu和Pb则呈高度显著下降趋势。     

太平洋水下海山磷酸盐的成因及形成环境

笔者首次对太平洋与大洋富钴结壳密切相关的海山磷酸盐的成因及形成环境进行了比较深入的研究。研究发现 ,各种产出形态的磷酸盐都不同程度地交代碳酸盐等含钙物质 ,而呈现出交代生物结构、交代凝灰结构、交代角砾状结构及交代填间结构等各种交代结构 ,反映了磷酸盐的交代成因。此外 ,其δ13 C值 (变化于 0 .7‰～ 2 .0‰之间 )也证实其属于交代成因。磷酸盐中Na、Mg、Sr、F、P2 O5含量以及Na/P2 O5、Mg/P2 O5、Sr/P2 O5、F/P2 O5的比值 ,特别是晶格中结构CO2 的含量 (变化于 5 .7%～ 6 .2 %之间 ) ,与形成于氧化环境下的Blakeplateau、ChathamRise、AgulhasBank等处的磷酸盐相近 ,表明调查区磷酸盐亦形成于氧化环境。氧同位素测定结果表明 ,磷酸盐的形成温度为 5 .8～ 14 .8℃ ,平均为 11.5℃ ,显示其形成于正常的海水温度环境。西、中太平洋海山磷酸盐形成环境十分接近的事实暗示 ,西、中太平洋广大区域内的成磷事件存在着时间上和成因上的统一性和相似性。     

鲁中山区新生代沉积盆地古近系含水层富水性分析

正前人研究结果认为,鲁中山区新生代沉积盆地古近系为一套碎屑岩孔隙裂隙含水层,单井涌水量小于100 m~3/d,长期作为弱富水含水层出现,不具有供水意义(康凤新等,2010)。2016年以来,中国地质调查局启动的沂蒙山革命老区1:5万水文地质调查项目,在大汶河流域中上游鲁中山区实施古近系钻孔8眼,涌水量达10800 m~3/d,直接解困人口1.1万。其中在莱芜盆地西北缘实