海面与海底地磁日变化差异及其对海洋磁力测量的影响

给出了海面与海底地磁日变化的计算公式,仿真分析了海面与海底地磁日变化差异,探讨了其对海洋磁力测量地磁日变改正的影响。结果表明:对于不同的地磁日变,海面与海底的地磁日变存在着较大的差异,且其随着地磁倾角的变化而变化,对磁测有一定的影响。为此,远海区海洋磁力测量中,建议联合采用地面日变站和海底日变站来减小或消除海面与海底地磁日变差异对磁测的影响,提高地磁日变改正的精度。     

Numerical simulation of random wave slamming on structures in the splash zone

The numerical investigation of random wave slamming on superstructures of marine structures in the splash zone is presented in this paper. The impact pressures on the underside of the structure are computed based on the improved volume of fluid method (VOF). The governing equations are Reynolds time-averaged equations and the two equation k– model. The third order upwind difference scheme is applied to the convection term to reduce the effect of numerical viscosity. The numerical wave flume with random wave-maker suitable for VOF is established. Appropriate moving contact-line boundary conditions are introduced to the model wave in contact with and separated from the underside of structure. Parametric studies have been carried out for different incident waves, structure dimensions and structure clearance. The numerical results are verified by the experimental results.     

燕山地区重、磁场特征分析与构造分区

本文对燕山地区的重、磁异常进行了处理与分析，根据重力场和磁场特征提出整个研究区分为4个部分。由北往南为：丰宁-隆化断裂带以北地区；丰宁-隆化断裂带至密云平泉之间的地区；密云-平泉至三河-昌黎之间的地区；三河-昌黎以南的平原区。丰宁-隆化断裂带为内蒙地轴（即华北地台北缘隆起带）南部边缘的界线。丰宁-隆化和三河-昌黎密度陡变带，以及密云-半壁山密度陡变带可能延深至中地壳。承德县-平泉密度陡变带延深比前面的密度陡变带略浅一些。     

武汉市汤逊湖沉积物重金属垂向变化的磁响应特征及环境意义

对武汉汤逊湖湖泊沉积物T06-1样芯进行了磁性测量、重金属分析和粒度分析,探讨了利用磁参数追踪、指示城市湖泊重金属污染的可行性.结果表明,低矫顽力的亚铁磁矿物主导了沉积物的磁性特征.磁参数χ,SIRM和ARM与重金属Cr,Zn,Cu和Pb呈现较为一致的垂向变化特征:55cm之下,磁参数值和重金属的含量均较低且稳定;在50～10 cm之间,两者基本呈现随深度的减小而增加的趋势,其中在20～10 cm区间,出现小范围内波动;而10cm至表层,元素含量和磁参数值随深度减小而急剧增加.选取粘土(＜4μm)对沉积物中Cr,Zn,Cu和Pb进行粒度校正的结果显示:校正后元素的变化趋向于平稳,但在表层的10cm处Cr,Pb,Zn和Cu的含量仍然较高,表明了表层沉积物中金属元素的含量主要受人类活动的影响.相关分析也表明了磁参数χ,SIRM和ARM与重金属Cr,Pb,Zn和Cu之间均呈显著相关关系(0.62≤R≤0.86),表明磁参数可以用于追踪和指示汤逊湖湖泊沉积物重金属污染.     

泥河湾盆地磁性地层定年与早期人类演化

主要评述了近年来泥河湾盆地磁性地层学的研究进展,包括建立泥河湾组的磁性地层年代格架、厘定泥河湾动物群的时代和确定华北地区早期人类活动年代序列.研究表明:第一,泥河湾组河湖相沉积序列记录了高斯正极性时末期以来的地磁极性特征(松山和布容极性时),即沉积时代始于约2.6Ma.早期人类至少在1.66～0.78Ma期间的大约90万年的时间内长期持续地占据高纬度的泥河湾盆地.泥河湾动物群(包括广义和狭义)的时代为2.0～0.8 Ma.第二,华北地区早期人类已经能够适应东亚高纬度地区冬季风增强、夏季风减弱和干旱化趋势增强的复杂环境变化,尤其能适应中更新世气候转型前后中国北方多变而且不稳定气候条件和生态环境.因此,气候和生态环境的多变性与不稳定性是促进人类进化的重要因素.第三,早期人类走出非洲以后,可能沿不同的路径并以较快的速度扩散到东亚地区.向南越过印度尼西亚的赤道地区,向北至少扩散到40°N的泥河湾盆地.     

不同类型沉积物磁化率的比较研究和初步解释

沉积物的磁化率分析以被广泛应用在第四纪古气候研究中,不同类型沉积物磁化率的解释可能存在明显的差异.本文选择了黄土、冲积物、湖积物、风沙堆积和南方红土等五种不同类型的沉积物,进行了磁化率的测试,粒度和孢粉分析,试图通过对沉积物磁化率和相关古环境指标的研究,对不同类型沉积物的磁化率予以对比并进行初步解释.研究结果表明,黄土和湖泊沉积中磁化率的变化主要受气候变化的影响,是指示古气候的重要指标;河流沉积物和风沙沉积物的磁化率主要受粒度的影响;影响南方红土磁化率的因素十分复杂,其磁化率的解释比较困难有待进一步的研究.这一研究表明,鉴于不同沉积物磁化率的影响因素存在明显的不同,因此在运用磁化率进行古环境解释时须持慎重态度.     

The influence of the electromagnetic core-mantle coupling torques on earth's rotation

The electromagnetic core-mantle coupling is one of the most likely hypotheses to explain the connections between both, the decade fluctuations of the Earth rotation and such of the magnetic field of the Earth. Within this paper, the axial and equatorial electromagnetic torques are computed at time intervals of two years from 1903.5 to 1975.5. They are compared with mechanical torques necessary for the excitation of the decade variations of the rotation of the Earth. The comparison is made with regard to the magnitude of the torques, to their time behaviour and to the periods within the time variations of both types of the torques. The computed electromagnetic torques are comparable with that necessary to excite the variations of the rotation of the Earth. But they are two or three orders less than that necessary to excite the decade variations of the polar motion. Some comparable periods were found within the spectra of the electromagnetic and the mechanical torques. This speaks in favour of the core-mantle coupling. But there are differences between both spectra too hinting at other processes which we cannot describe by a simple model of the core-mantle coupling.     

Nonlinear dynamo effects for an inhomogeneously turbulent rotating fluid

Im Rahmen der Magnetohydrodynamik der mittleren Felder werden die turbulenzbedingte elektromotorische Kraft und der turbulenzbedingte Spannungstensor für eine leitende Flüssigkeit mit inhomogener Turbulenz auf einem rotierenden Körper berechnet. Dabei wird der Einflu$sZ des Magnetfeldes auf der Turbulenz berücksichtigt. So erscheinen nichtlineare Effekte bei den Vorgängen, die für das Vorhandensein von Magnetfeld und differentieller Rotation verantwortlich sind; die dafür ma$sZgebenden Koeffizienten sind Funktionen des Magnetfeldes. Die Nichtlinearitäten werden bis zur zweiten Ordnung im mittleren Magnetfeld (d. h. als schwache Nichtlinearitäten) erfa$sZt. Der $aL-Effekt beim $aL$OM-Dynamo erleidet sowohl bei langsamer als auch bei rascher Rotation eine Schwächung durch das Magnetfeld. Es werden einige astrophysikalische Anwendungen der Ergebnisse erörtert. Insbesondere wird auf die Möglichkeit hingewiesen, da$sZ die bei der Sonne beobachteten Torsionsschwingungen als Folge des im Aktivitätszyklus schwankenden magnetischen Einflusses auf den für die differentielle Rotation ma$sZgebenden A-Effekt erscheinen.     

Report on the physical characteristics of Vaidya-Tikekar's exact relativistic model for a superdense star

We report here the results of our examination of the physical properties of Vaidya-Tikekar's model for a relativistic star. Full details will be published elsewhere. The analysis yields a strong indication that the model is stable with respect to infinitesimal radial oscillations. We find that the adiabatic speed of sound is smaller than the speed of light everywhere inside the fluid sphere if the radius of the sphere is larger than 1.46 times its Schwarzschild radius. We also find that the fluid must necessarily be supraluminal somewhere if the speed of sound is decreasing outwards close to the center. We further find that the strong energy condition is fulfilled everywhere if it is fulfilled at the center. Since the ratio of the pressure p and the density ⋅ is decreasing outwards, this indicates that the temperature gradient is negative. We also find that the relativistic adiabatic index is larger than two. Demanding the fluid to be causal, and taking the pressure and the density to be somewhere given by 7.4 ⋅ 10³³ dynes/cm³ and 5.1 ⋅ 10¹⁴ g/cm³, we calculate the maximum mass of the fluid sphere to be 3 solar masses.