Mars

Mars is the fourth planet out from the sun. It is a terrestrial planet with a density suggesting a composition roughly similar to that of the Earth. Its orbital period is 687 days, its orbital eccentricity is 0.093 and its rotational period is about 24 hours. Mars has two small moons of asteroidal shapes and sizes (about 11 and 6 km mean radius), the bigger of which, Phobos, orbits with decreasing semimajor orbit axis. The decrease of the orbit is caused by the dissipation of tidal energy in the Martian mantle. The other satellite, Deimos, orbits close to the synchronous position where the rotation period of a planet equals the orbital period of its satellite and has hardly evolved with time. Mars has a tenous atmosphere composed mostly of CO with strong winds and with large scale aeolian transport of surface material during dust storms and in sublimation-condensation cycles between the polar caps. The planet has a small magnetic field, probably not generated by dynamo action in the core but possibly due to remnant magnetization of crustal rock acquired earlier from a stronger magnetic field generated by a now dead core dynamo. A dynamo powered by thermal power alone would have ceased a few billions of years ago as the core cooled to an extent that it became stably stratified. Mars' topography and its gravity field are dominated by the Tharsis bulge, a huge dome of volcanic origin. Tharsis was the major center of volcanic activity, a second center is Elysium about 100° in longitude away. The Tharsis bulge is a major contributor to the non-hydrostaticity of the planet's figure. The moment of inertia factor together with the mass and the radius presently is the most useful constraint for geophysical models of the Martian interior. It has recently been determined by Doppler range measurements to the Mars Pathfinder Lander to be (Folkner et al. 1997). In addition, models of the interior structure use the chemistry of the SNC meteorites which are widely believed to have originated on Mars. According to the models, Mars is a differentiated planet with a 100 to 200 km thick basaltic crust, a metallic core with a radius of approximately half the planetary radius, and a silicate mantle. Mantle dynamics is essential in forming the elements of the surface tectonics. Models of mantle convection find that the pressure-induced phase transformations of -olivine to -spinel, -spinel to -spinel, and -spinel to perovskite play major roles in the evolution of mantle flow fields and mantle temperature. It is not very likely that the -spinel to perovskite transition is present in Mars today, but a few 100 km thick layer of perovskite may have been present in the lower mantle immediately above the core-mantle boundary early in the Martian history when mantle temperatures were hotter than today. The phase transitions act to reduce the number of upwellings to a few major plumes which is consistent with the bipolar distribution of volcanic centers of Mars. The phase transitions also cause a partial layering of the lower mantle which keeps the lower mantle and the core from extensive cooling over the past aeons. A relatively hot, fluid core is the most widely accepted explanation for the present lack of a self-generated magnetic field. Growth of an inner core which requires sub-liquidus temperatures in the core would have provided an efficient mechanism to power a dynamo up to the present day. Received 10 May 1997     

Radio Emission from Galactic Disks

This paper gives a short overview of the observational results on galactic magnetic fields. Interstellar magnetic fields, as deduced from multi-frequency polarization observations, show a well-ordered structure largely following the spiral arms. In some galaxies an axisymmetric spiral pattern dominates (the field being directed inwards), while others exhibit a dominant bisymmetric spiral field or mixed modes, as predicted from non-linear dynamo theory. As long as star formation activity is low, the magnetic fields are rather regular. Strong star formation leads to turbulent cloud motions and supernova explosions, which tangle the field, so that the radio emission is only weakly polarized. As a consequence the highest fractional polarizations and polarized intensities at centimeter wavelengths are found in interarm regions. At decimeter wavelengths, galactic disks become optically thick for polarized emission. In NGC 6946 the regular field is concentrated in narrow magnetic arms located in between the optical spiral arms. The field cannot simply be frozen into the gas and oriented by a density-wave flow. A galactic dynamo may provide a stable spiral pattern of the field, but non-axisymmetric models are still being developed.     

河北蔚县九宫口断层重叠带的断层生长、位移转移和演化

对河北蔚县九宫口断层重叠带进行了地质和地貌观察、年龄测定和断层落差分析。结果表明,伴随重叠带内的断层生长,位移发生转移,而且,原来两个独立的断层段演化成为互相关联的单一断层。岩浆活动和掀斜作用是该重叠带演化的原因     

再论发展方程差分格式的构造和应用

【摘　要】本文把一大类大气、海洋方程归结为一种发展方程,具体构造了若干定时间步长的显式完全平方守恒差分格式。并证明在一定条件下,这类格式也具有能量守恒、“广义能量”守恒和“平均尺度”守恒的特性,它表明这类格式具有较好的计算稳定性和省时性。文中还探讨了显式平方守恒格式与隐式平方守恒格式之间的密切联系。最后给出了令人满意的用四波的R-H波作数值检验的结果。     

贵州泥堡金矿床的流体包裹体和稳定同位素地球化学研究及其矿床成因意义

泥堡金矿床是黔西南台地相区以断控型矿体为主、层状型矿体为辅的复合型金矿床。断控型矿体主要发育于低角度的逆冲断层中,层状型矿体主要发育于断控型矿体之上穹窿构造核部的上二叠统龙潭组和中二叠统大厂层中。根据脉体的穿插关系和矿物共生组合,将成矿过程从早到晚划分为石英-黄铁矿阶段、石英-黄铁矿-毒砂阶段和方解石-石英-多金属硫化物±萤石阶段。泥堡金矿床两类矿体中流体包裹体类型相同,包括水溶液包裹体、CO_2-H_2O包裹体和CO_2包裹体。层状型矿体早阶段石英中流体包裹体均一温度范围为194~305℃,盐度范围为0.70%~7.81%NaC leqv,石英的δ~(18)O_(V-SMOW)为22.7~23.6‰,计算得到的δ~(18)OH 13.5‰,~-62‰;2O为12.6‰~石英中流体包裹体水的δD_(H_2O)为-84‰中阶段石英中流体包裹体均一温度范围为125~278℃,盐度范围为0.53%~6.46%NaC leqv,石英的δ~(18)O_(V-SMOW)为16.6‰~23.5‰,计算得到的δ~(18)O_(H_2O)为4.4‰~11.3‰,石英中流体包裹体水的δDH~-65‰;3~2O为-80‰晚阶段方解石中流体包裹体均一温度范围为13197℃,盐度范围为0.53%~7.45%NaC leqv,萤石中流体包裹体均一温度范围为102~264℃,盐度范围为0.18%~4.49%NaC leqv,方解石的δ~(18)O_(V-SMOW)为20.6‰~22.7‰,计算得到的δ~(18)OH 3‰~10.4‰,2O为8.方解石中流体包裹体水的δD_(H_2O)为-56‰~-47‰,δ13CV-PDB为-6.6‰~-1.6‰。断控型矿体中阶段石英中流体包裹体均一温度范围为126~296℃,盐度范围为0.35%~8.29%NaC leqv,石英的δ~(18)O_(V-SMOW)为21.9‰~23.7‰,计算得到的δ~(18)OH9.8‰~11.6‰,2O为石英中流体包裹体水的δDHNaC leqv,2O为-85‰;晚阶段方解石中流体包裹体均一温度范围为118~236℃,盐度范围为0.53%~7.02%方解石的δ~(18)O_(V-SMOW)为19.8‰~21.5‰,计算得到的δ~(18)OH~10.4‰,2O为8.7‰方解石中流体包裹体水的δDH‰~-55‰,2O为-67δ13CV-PDB为-7.0‰~-4.7‰。流体包裹体和稳定同位素研究结果表明,两类矿体成矿流体性质和来源一致,且具有相似的演化过程。泥堡金矿床的成矿流体来源于大气降水和海水的混合,并且从早阶段到晚阶段,海水所占的比例逐渐增大,碳主要来自海相碳酸盐岩的溶解。     

岩浆包裹体研究在火山岩岩石学中的地位

岩浆包裹体研究已经成为现代火山岩岩石学的一项分支学科。研究方面涉及:重溯火山岩浆结晶演化的热历史,提供有关火山岩浆沿下降液相线的成分数据;查明火山岩浆结晶演化过程中化学成分(包括挥发组分)的变迁规律;查明各种岩浆事件的性质(分离结晶、不混溶、混合、混染),及其发生发展的物理化学条件;帮助探索解决某些疑难问题,如下地壳—上地幔的性质及玄武岩浆起源、细碧岩—角斑岩系的成因、测定蚀变火山岩建造的年龄等。此外,岩浆包裹体的实验岩石学研究,以及利用岩浆包裹体阐明火山建造的含矿性,研究火山沉积作用、地热作用等,对于火     

Dynamic process-response model of river channel development

Feedback mechanisms, which operate upstream through drawdown and backwater effects and downstream through sediment discharge are responsible for channel evolution. By combining these mechanisms with channel processes it euables a dynamic process-response model to be developed to simulate the initial evolution of straight gravel-bed channels. When erosion commences on a land surface, sediment entrained in the headwater reach by hydraulic action is selectively transported, deposited and reworked. This produces a damped oscillation between degradation and aggradation as the channel and valley respond to spatial and temporal variations in sediment calibre and hydraulic conditions. The initial cut and fill phases are responsible for valley incision and floodplain development while secondary and subsequent activity can produce river terraces. Eventually sediment entrainment in the headwaters declines as slopes are reduced. Subsequent channel evolution is relatively insignificant because it is dependent on local weathering activity producing material that can be transported on declining slopes. Therefore landforms produced during the initial phase of development, when local weathering was non-limiting, dominate the landscape.     

Some aspects of the monsoon circulation and monsoon rainfall

Summary The south Asian summer monsoon from June to September accounts for the greater part of the annual rainfall over most of India and southeast Asia. The evolution of the summer and winter monsoon circulations over India is examined on the basis of the surface and upper air data of stations across India. The salient features of the seasonal reversals of temperature and pressure gradients and winds and the seasonal and synoptic fluctuations of atmospheric humidity are discussed. The space-time variations of rainfall are considered with the help of climatic pentad rainfall charts and diagrams. The rainfall of several north and central Indian stations shows a minimum around mid-August and a maximum around mid-February which seem to be connected with the extreme summer and winter positions of the ITCZ and the associated north-south shifts in the seasonal circulation patterns. Attention is drawn to the characteristic features of the monsoon rainfall that emerge from a study of daily and hourly rainfall of selected stations. Diurnal variations of temperature, pressure, wind and rainfall over the monsoon belt are briefly treated.     

黄河中游龙口—天桥段封冻期的河床演变

本文根据黄河河曲段六个封冻期的原型观测资料,对该冰塞河段冰期的河床演变及水内冰花在冰塞下的堆积——冰塞演变,进行了分析研究。总结出冰塞河段的河床演变特点与冰塞演变的相互关系,得出了河床冲淤及水内冰堆积计算的经验关系式及河床冲淤平衡的临界水力参数。文中还对有关冰期输沙的若干问题进行了讨论。     

Heterochronic evolution in the Late Cretaceous echinoid Gauthieria (Echinoidea,Phymosomatidae)

Based on representatives of the Late Cretaceous genus Gauthieria (Gauthieria radiata – Gauthieria spatulifera – Gauthieria princeps), ontogenetic trajectories within the family Phymosomatidae are described for the first time. Due to shared similarities in their ontogenetic development, an intimate evolutionary relationship must be assumed. This interpretation is most supported by analyses of the development in the ambulacral plating pattern (alternation of simple plates and compound plates), which is not commonly found among the Phymosomatoidae. This pattern, however, is present among all three species during development. The developmental trajectories of 8 further characters were included in this study (arrangement of the adapical pore pairs, number of pore pairs, pore pair numbers in ambital ambulacral plates, number of interambulacral plates, peristomal opening, apical opening diameter, test height, radial ornament of the areoles). The evolution in this lineage is characterised by several different heterochronic processes, which suggest a dissociated heterochronic evolution, indicating a developmental modularity. Additionally, the systematic treatment of G. princeps is discussed on account of the presented results.