叠前正演模拟与偏移的网络并行计算

在叠前深度偏移和非零炮检距声波方程正演计算过程中包含了大量的可并行计算的成分。作者在本文中提出叠前正演模拟与偏移的网络并行计算算法，并基于TCP／IP协议，将该算法设计成网络并行处理程序，极大地提高了计算效率。实际运算结果证明，本文提出的并行算法和技术路线是切实可行的。     

Petrological features of a Numidian section in the Lucanian Apennine (southern Italy)

A continuous section of Numidian sandstones cropping out along the eastern margin of the Lucanian Apennine (southern Italy) has been studied in relation to its petrographic and geochemical aspects. Owing to their simple mineralogy, both chemical and petrographic classifications indicate that the sandstones are subarkoses. They are characterized by high mineralogical maturity, poor sorting, abundant siliciclastic matrix and subangular quartz grains. The principal composition is Q_80–94 F_6–20 L_0–1 corresponding to SiO₂/Al₂O₃ and Fe₂O₃/K₂O ratios ranging from 37·216 to 17·124 and from 1·182 to 0·514 respectively. Two quartz grain types were distinguished: deformed and undeformed quartz grains, the former generally subangular in shape and the latter rounded. Two distinct origins of detritus can be suggested; (i) the undeformed and rounded quartz grains derive from arenaceous continental sequences; (ii) the siliciclastic matrix, the deformed subangular quartz grains, the heavy minerals and the large crystals of K-feldspar probably derive from a crystalline basement formed by low–medium–high grade metamorphic rocks and granitoids. The Numidian subarkoses represent the mixing of these two components. Both kinds of detritus can be referred to the African Craton where crystalline basement is extensively overlain by Palaeozoic and Mesozoic sandstones. The different proportions of the two components in the mixture account for the variability of the sandstone composition and might explain the mixed Numidian successions cropping out in various sectors of the Mediterranean area. Copyright © 1998 John Wiley & Sons, Ltd.     

夹皮沟金矿深部成矿预测研究

系统研究了夹皮沟地区二道沟、庙岭、大猪圈、下戏台和东坨腰子等矿床矿体和近矿围岩微量元素、矿石矿物组合和黄铁矿热电系数等的垂直变化特征,认为三者具有相互一致的变化规律,即：与热液金矿床通常的分带性相比,具有逆向分带的现象,这种特征被认为是多层次正常分带上下叠加的产物,反映夹皮沟地区金矿床在垂向上普遍存在着多个富集地段.据此预测二道沟、庙岭、大猪圈、下戏台和东坨腰子等矿床在目前的开采深度下部仍有发现深部矿体的可能.     

西北地区水资源若干问题探讨

在对我国西北地区水资源及开发利用现状进行分析的基础上,针对如何认识西北地区的缺水问题,如何评价西北地区地下水资源的重要性,怎样看待深层地下水资源以及开采地下水可能引起的环境地质问题等,进行了较深入的分析论述。指出进一步查清西北地区地下水资源,尤其是中深层地下水资源,并加以科学、适度的开发和合理利用,是解决西北地区水资源短缺问题的重要途径之一。     

The Relationship between Tectono-metamorphic Evolution and Argon Isotope Records in White Mica: Constraints from in situ 40Ar-39Ar Laser Analysis of the Variscan Basement of Sardinia

The basement of Sardinia represents a nearly complete sectionof a segment of the Variscan belt that experienced a polyphasetectono-metamorphic evolution and Barrovian metamorphism. Thisbasement is well suited to investigate the relationship betweentectono-metamorphic evolution and argon isotope records in whitemica. Micaschists from the garnet zone (maximum T of up to 520–560°C)contain two texturally and chemically resolvable generationsof white mica: (1) deformed celadonite-rich flakes, defininga relict S₁ foliation preserved within the main S₂ foliationor enclosed in rotated albite porphyroblasts; (2) celadonite-poorwhite micas aligned along the main S₂ foliation. The S₁ foliationdeveloped earlier and at a deeper crustal level with respectto that at which the thermal peak was reached. From the staurolitezone (T of up to 590–625°C) to the sillimanite + K-feldsparzone, white mica is nearly uniform in composition (muscovite)and is predominantly aligned along the S₂ foliation or is oflater crystallization. In situ ⁴⁰Ar–³⁹Ar laser analysesof white mica yielded ages of     

The potassium abundance in the solar photosphere

High precision center-limb spectrograms of the K i resonance doublet line at λ 7699 Å were used to study the line formation and to determine the abundance of potassium in the solar atmosphere. The LTE assumption is not valid for these lines. Synthetic profiles computed in NLTE reproduce very well the observed center-limb line behaviour and yield log? _K = 5.14±0.10 for the solar abundance of potassium (on the scale of log? _H = 12 for Hydrogen).     

Coronal changes associated with a disappearing filament

This paper describes Skylab/ATM observations of the events associated with a disappearing filament near the center of the solar disk on January 18, 1974. As the filament disappeared, the nearby coronal plasma was heated to a temperature in excess of 6 × 10⁶K. A change in the pattern of coronal emission occurred during the 11/3 hr period that the soft X-ray flux was increasing. This change seemed to consist of the formation and apparent expansion of a loop-like coronal structure which remained visible until its passage around the west limb several days later. The time history of the X-ray and microwave radio flux displayed the well-known gradual-rise-and-fall (GRF) signature, suggesting that this January 18 event may have properties characteristic of a wide class of X-ray and radio events.In pursuit of this idea, we examined other spatially-resolved Skylab/ATM observations of long-duration X-ray events to see what characteristics they may have in common. Nineteen similar long-lived SOLRAD X-ray events having either the GRF or post-burst radio classification occurred during the nine-month Skylab mission. Sixteen of these occurred during HAO/ATM coronagraph observations, and 7 of these 16 events occurred during observations with both the NRL/ATM slitless spectrograph and the MSFC-A/ATM X-ray telescope. The tabulation of these events suggests that all long-lived SOLRAD X-ray bursts involve transients in the outer corona and that at least two-thirds of the bursts involve either the eruption or major activation of a prominence. Also, these observations indicate that long-lived SOLARD events are characterized by the appearance of new loops of emission in the lower corona during the declining phase of the X-ray emission. However, sometimes these loops disappear after the X-ray event (like the post-flare loops associated with a sporadic coronal condensation), and sometimes the loops remain indefinitely (like the emission from a permanent coronal condensation).Visiting Scientist, Kitt Peak National Observatory, Tucson, Ariz. 85726, U.S.A. operated by the Association of Universities for Research in Astronomy, Inc., under contract with the National Science Foundation.Presently located at NASA/MSFC, Space Sciences Laboratory, Marshall Space Flight Center, Ala. 35812, U. S.A.     

Criterion for propagation of magnetohydrodynamic waves: An equivalence

It is shown that the requirement that a magnetohydrodynamic wave propagate over a distance equal to a large number of wavelengths without substantial attenuation is equivalent to the requirement that the lateral velocity of displacement of the field lines far exceed a characteristic velocity. This latter velocity is the velocity of slippage of the field lines with respect to the medium.     

Fast Segmentation of Solar Extreme Ultraviolet Images

A segmentation scheme for identifying large-scale structures (coronal holes, active regions, etc.) in solar extreme ultraviolet images, is presented. Unlike standard approaches, both the image intensity and the relative contribution of different wavelengths are used. Spectral information is important for compensating luminosity changes. The approach is illustrated with images taken in the extreme ultraviolet by the EIT telescope onboard SOHO. This supervised segmentation scheme, which incorporates a Bayesian classifier, is computationally simple, and can easily be used to track in near-real time structures, such as coronal holes.     

On the Dynamics of Dust Grains in a Hierarchical Environment

Most main sequence stars are binaries or higher multiplicity Systems and it appears that at birth most stars have circumstellar disks. It is commonly accepted that planetary systems arise from the material of these disks; consequently, binary and multiple systems may have a main role in planet formation. In this paper, we study the stage of planetary formation during which the particulate material is still dispersed as centimetre-to-metre sized primordial aggregates. We investigate the response of the particles, in a protoplanetary disk with radius R_D = 100 AU around a solar-like star, to the gravitational field of bound perturbing companions in a moderately wide (300–1600 AU) orbit. For this purpose, we have carried out a series of simulations of coplanar hierarchical configurations using a direct integration code that models gravitational and viscous forces. The massive protoplanetary disk is around one of the components of the binary. The evolution in time of the dust sub-disk depends mainly on the nature (prograde or retrograde) of the relative revolution of the stellar companion, and on the temperature and mass of the circumstellar disk. Our results show that for binary companions near the limit of tidal truncation of the disk, the perturbation leads to an enhanced accretion rate onto the primary, decreasing the lifetime of the particles in the protoplanetary disk with respect to the case of a single star. As a consequence of an enhanced accretion rate the mass of the disk decreases faster, which leads to a longer resultant lifetime for particles in the disk. On the other hand, binary companions may induce tidal arms in the dust phase of protoplanetary disks. Spiral perturbations with m = 1 may increase in a factor 10 or more the dust surface density in the neighbourhood of the arm, facilitating the growth of the particles. Moreover, in a massive disk (0.01M⊙) the survival time of particles is significantly shorter than in a less massive nebula (0.001M⊙) and the temperature of the disk severely influences the spiral-in time of particles. The rapid evolution of the dust component found in post T Tauri stars can be explained as a result of their binary nature. Binarity may also influence the evolution of circumpulsar disks. This revised version was published online in July 2006 with corrections to the Cover Date.