临沭县城乡建设用地增减挂钩试点具体实施分析

对临沭县自2008年实施城乡建设用地增减挂钩工作以来的具体做法、取得的经验教训进行认真分析,特别是从项目区立项申报、组织实施和资金使用管理等方面进行深入研究,指出了存在的共性问题,总结了行之有效的经验做法,并就如何正确实施、高效组织、加快推进增减挂钩试点工作提出几点建议,希望对健康平稳推进增减挂钩工作有所裨益。     

塔河油田十二区奥陶系油气分布规律及控制因素

塔河油田十二区奥陶系油藏为碳酸盐岩岩溶缝洞型油藏,油气水分布规律复杂。对原油的物理性质、平面及纵向上的分布特征、油水界面等的分析表明,区内主要为高黏度、含蜡、高含硫的超重质原油。平面上密度分布呈西部和东部低、中部高的特点;纵向上原油密度与深度关系不大。高产油区多沿主断裂带分布。油水界面不统一,但从东向西随中奥陶统顶面的降低而降低。认为该区油气分布不受现今构造位置高低的控制,而是受区域构造背景、断裂带的分布、储集层的发育程度、成藏演化过程以及不整合面等因素综合控制。     

基于SPE与SPATT的水体中麻痹性贝类毒素检测方法构建与应用

为实现麻痹性贝类毒素(paralytic shellfish poisoning,PSP)的实时监控与提前预警,本研究构建了基于固相萃取技术(solid phase extraction,SPE)与固相吸附毒素跟踪技术(solid phase adsorption toxin tracking,SPATT)的水体中PSP检测方法,重点优化了吸附材料及前处理方法,评价了回收率、检出限等指标,并将方法应用于2019年春季秦皇岛山海关海域PSP消长过程的监测中,比较评估了两种方法的监控预警效果。结果表明:SPE方法选用ENVI-Carb 500mg/6mL固相萃取柱,过样体积为50mL,13种PSP组分的平均回收率为82.2%±10.0%、检出限为4.0-20.0ng/L;SPATT方法选用SP207大孔吸附树脂,洗脱时间为静置Id最佳,整体回收率约为9.2%;在实际应用中,结合产毒藻密度及贻贝富集毒素含量的变化,发现SPE方法的检测结果可实时表征海域PSP风险状况,对于贻贝中PSP的预警效果也显著优于SAPTT方法,后者不仅因监控方式相对滞后一个监测周期,且灵敏度及准确性均较差。对于秦皇岛...     

冲绳海槽南部沉积层序的粒度特征

对取自冲绳海槽南部的A2 3孔经前处理后的沉积物样品进行了粒度测试,探讨了陆源沉积层序的粒度特征。沉积物平均粒径、分选系数、偏态、峰态等粒度参数的变化显示出A2 3孔的沉积层序以 4 0 0cm为界可分为上、下两段,下段各参数稳定,代表了比较稳定的水动力条件的沉积环境;上段则波动较大,小规模浊流沉积频繁发育,暗示了不稳定的沉积环境。浊流层内粗粒与细粒组分含量及粒度分布的变化具有明显的规律性。通过分析A2 3孔陆源沉积层序的各沉积参数特征,认为冲绳海槽南部的沉积环境和动力在时间尺度上有较大的变化,东海陆架物质向南部海槽的输运可能是以峡谷为通道的重力作用引起的床底沉积作用为主。另外,对陆源碎屑和全样粒度结果的对比,显示了前处理方法对于海洋沉积物粒度分析的重要性.     

Solar Type III Bursts and the Generation of Backward Langmuir Wave

It is generally believed that the conversion of Langmuir wave (LW) to electromagnetic wave is the generating mechanism of solar type III bursts. The Langmuir wave can be easily excited by the instability of the electron-beam current, and the interaction of the forward and backward Langmuir waves is considered to be the cause for the second harmonic of a type III burst, but, so far, the dispersion equation and generating mechanism of the backward Langmuir wave have not yet been thoroughly studied. For the equation of two-stream instability with temperature included, an analytical solution is derived. It is found that the dispersion relation of the forward LW strongly depends on the beam-current speed, while that of the backward LW depends only on the thermal velocity, when the other parameters are fixed. These analytical results are partially confirmed by particle-in-cell (PIC) simulations. With the PIC simulation, the generating mechanism of the backward LW is studied, and it is revealed that the backward LW can not be excited directly by the electron-beam current, and that its energy is obtained basically from the scattering of the forward LW. However, the electron-beam current does cause a direct amplification of the second harmonic of the forward LW.     

Detection of high-energy solar neutrons and protons by ground level detectors on April 15, 2001

In association with the large solar flare of April 15, 2001, the Chacaltaya neutron monitor observed a 3.6σ enhancement of the counting rate between 13:51 and 14:15 UT. Since the enhancement was observed beginning 11 min before the GLE, solar neutrons must be involved in this enhancement. The integral energy spectrum of solar neutrons can be expressed by a simple power law in energy with the index γ=-3.0±1.0. On the other hand, an integral energy spectrum of solar protons has been obtained in the energy range between 650 MeV and 12 GeV. The spectrum can also be expressed by a power law with the power index γ=-2.75±0.15. The flux of solar protons observed at Chacaltaya (at 12 GeV) was already one order less than the flux of the galactic cosmic rays. It may be the first simultaneous observation of the energy spectra of both high-energy protons and neutrons. Comparing the Yohkoh soft X-ray telescope images with the observed particle time profiles, an interesting picture of the particle acceleration mechanism has been deduced.     

Climatic and biological simulations in a two-way coupled atmosphere–biosphere model (CABM)

Today, most land surface process models have prescribed seasonal change of vegetation with regard to the exchange processes between land and the atmosphere. However, in order to consider the real interaction between vegetation and atmosphere and represent it best in a climate model, the vegetation growth process should be included. In other words, “life” should be brought into climate models. In this study, we have coupled the physical and biological components of AVIM (Atmosphere–Vegetation Interaction Model), a land surface model including plant ecophysiological processes, into the IAP/LASG L9 R15 GOALS GCM. To exhibit terrestrial vegetation information, the vegetation is given a high resolution of 1.5° by 1.5° to nest and couple the fine grid cells of land with the coarse grid cells of atmosphere, which is 7.5° longitude and 4.5° latitude. The simulated monthly mean surface air temperature and precipitation is close to the observations. The monthly mean Leaf Area Index (LAI) is consistent with the observed data. The global annual mean net primary production (NPP) simulation is also reasonable. The coupled model is stable, providing a good platform for research on two-way interaction between land and atmosphere, and the global terrestrial ecosystem carbon cycle.     

H3 as a trap for noble gases: 1—The case of Argon

The possibility of H₃⁺ playing a role as a sink for noble gases has been investigated in the case of Argon. Elaborate quantum methods (ab initio Coupled Cluster and density functional BH&HLYP levels of theory) have been shown to reproduce the rotational constants within 0.3% together with the only known IR frequency on the test case of Ar…D₃⁺. Dissociation energies of (Ar)_n…H₃⁺ as a function of cluster size, i.e. 7.2 (n=1), 3.7 (n=2), 3.6 (n=3), 1.6 (n=4), 1.7 (n=5) kcal/mol, follow the pattern established experimentally for (Ar)_n…H₃⁺ and (H₂)_n…H₃⁺ series. Rotational constants and harmonic frequencies of (Ar)_n…H₃⁺ (n=1-3) are presented.     

The lower mass function of young open clusters: clues to (sub)stellar formation

We report the present day mass functions (PDMFs) of 4 young open clusters over a mass range from 30 Jupiter masses to 3M_ . Three of these clusters have been chosen to have a similar age of ∼100 Myr. Their PDMFs are remarkably similar and are comparable to the field mass function. This suggests little impact of initial conditions (stellar density, metallicity) on the mass distribution and raises some issues concerning the currently debated star and brown dwarf formation theories. The fourth cluster is older (600 Myr) which allow us to investigate the effect of the cluster dynamical evolution on the shape of the mass function. (© 2005 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)