南海南北缘的构造特征对比

南海南北缘具有不同地球物理特征和地质构造特征。南海北缘新生代盆地为断陷型盆地；南海南缘则发育周缘前陆盆地、板缘拉张盆地。北缘盆地的沉降以两幕发展为特征，南缘的盆地的沉降以三幕发展为特征。南海北缘盆地经历了古新世一始新世盆地形成时期、渐新世一中中新世盆地发展期、晚中新世一第四纪盆地成熟期三个阶段；南海南缘盆地经历了古新世一中始新世初始盆地形成、晚始新世一中中新世盆地发展、中中新世末盆地遭受压扭改造、晚中新世一第四纪盆地定型期四个阶段。造成南北缘差异的原因是边缘性质不同：北缘为拉张型边缘；南缘北侧是拉张型边缘，南缘南侧是挤压型边缘。     

Al decay: Heat production and a revised age for Iapetus

We revisit the appropriate energies to be used for computing heat production from ²⁶Al decay. Due to the complexity of the decay scheme of this radioisotope, previous geophysical studies have used values ranging from 1.2 to 4 MeV per decay. The upper bound corresponds to the difference in mass energy between the ²⁶Al and ²⁶Mg ground states. This includes energy carried away by neutrinos, which does not contribute to heating planetary material. The lower bound does not account for the heating caused by the absorption of the γ rays from the excited ²⁶Mg, or for the annihilation energy deposited in the material if the decay occurs inside even small planetesimals. Based on the calculations described by Schramm et al. [Schramm, D., Tera, F., Wasserburg, G.J., 1970. The isotopic abundance of ²⁶Mg and limits on ²⁶Al in the early Solar System. Earth Planet. Sci. Lett. 10, 44-59] updated with the most recent nuclear constants, we recommend using a heat production value of 3.12 MeV per decay, which is the total energy of disintegration minus the energy carried off by the neutrinos. This heat production value is higher than the value used in the modeling of Iapetus by Castillo-Rogez et al. [Castillo-Rogez, J., Matson, D.L., Sotin, C., Johnson, T.V., Lunine, J.I., Thomas, P.C., 2007. Iapetus’ geophysics: Rotation rate, shape, and equatorial ridge. Icarus 190, 179-202] by about a factor 2.5. The resulting estimate of the time of formation of Iapetus is shifted by about 1 Myr, to between ∼3.4 and 5.4 Myr after the production of the calcium-aluminum inclusions (CAIs).     

岩石红外辐射温度随岩石应力变化的规律和特征以及与声发射率的关系

在实验室对不同岩性不同结构的岩石试件进行单轴加载至试件破裂试验，得出了如下主要结果：（１）岩石试件的红外辐射温度随应力增加而变化，温度变化的范围在０．２℃－０．８℃。（２）岩石试件临破裂前出现明显的岩石破裂温度前兆。（３）有一部分岩石试件临破裂前出现高温条带、高温区或低温条带、低温区。不久，试件沿高温条带、区或低温条带、区发生主破裂。（４）有一部分岩石试件在临破裂前出现温度脉冲，正脉冲达到２．８℃，负脉冲达到－１．０℃。（５）当应力增加时，岩石试件的辐射温度增加与声发射率增加呈互补关系。     

工程地球物理方法技术研究现状综述

从工程地球物理的方法技术角度,结合相应的地球物理理论,综述了工程地球物理方法在各种工程领域的应用现状和发展,并具体讨论了各领域中存在的问题。     

地球物理学在生态环境及其相关领域中的应用

多年来应用地球物理学以地球的岩石圈为研究对象，为矿产资源的勘查和开发提供了理论、方法和手段。而地球科学的功能应该还包括防止地质灾害、保护生态环境、认识地球等。本文从六个方面（地下水及地表水体污染的测量和监控、评价工业区的生态环境，城市中的地球物理监测，查明废弃弹药隐藏地区的位置，监测核爆炸以及监测地震和其它地质灾害等）论述了地球物理学在生态环境及其它领域中的应用。     

On convection in ice I shells of outer Solar System bodies, with detailed application to Callisto

It has been argued that the dominant non-Newtonian creep mechanisms of water ice make the ice shell above Callisto's ocean, and by inference all radiogenically heated ice I shells in the outer Solar System, stable against solid-state convective overturn. Conductive heat transport and internal melting (oceans) are therefore predicted to be, or have been, widespread among midsize and larger icy satellites and Kuiper Belt objects. Alternatively, at low stresses (where non-Newtonian viscosities can be arbitrarily large), convective instabilities may arise in the diffusional creep regime for arbitrarily small temperature perturbations. For Callisto, ice viscosities are low enough that convection is expected over most of geologic time above the internal liquid layer for plausible ice grain sizes (?a few mm); the alternative for early Callisto, a conducting shell over a very deep ocean (>450 km), is not compatible with Callisto's present partially differentiated state. Moreover, if convection is occurring today, the stagnant lid would be quite thick (∼100 km) and compatible with the lack of active geology. Nevertheless, Callisto's steady-state heat flow may have fallen below the convective minimum for its ice I shell late in Solar System history. In this case convection ends, the ice shell melts back at its base, and the internal ocean widens considerably. The presence of such an ocean, of order 200 km thick, is compatible with Callisto's moment-of-inertia, but its formation would have caused an ∼0.25% radial expansion. The tectonic effects of such a late, slow expansion are not observed, so convection likely persists in Callisto, possibly subcritically. Ganymede, due to its greater size, rock fraction and full differentiation, has a substantially higher heat flow than Callisto and has not reached this tectonic end state. Titan, if differentiated, and Triton should be more similar to Ganymede in this regard. Pluto, like Callisto, may be near the tipping point for convective shutdown, but uncertainties in its size and rock fraction prevent a more definitive assessment.     

Tidal heating and the long-term stability of a subsurface ocean on Enceladus

Tidal dissipation has been suggested as the heat source for the south polar thermal anomaly on Enceladus. We find that under present-day conditions and assuming Maxwellian behavior, tidal dissipation is negligible in the silicate core. Dissipation may be significant in the ice shell if the shell is decoupled from the silicate core by a subsurface ocean. We have run a series of self-consistent convection and conduction models in 2D axisymmetric and 3D spherical geometry in which we include the spatially-variable tidal heat production. We find that in all cases, the shell removes more heat from the interior than can be produced in the core by radioactive decay, resulting in cooling of the interior and the freezing of any ocean. Under likely conditions, a 40-km thick ocean made of pure water would freeze solid on a ∼30 Ma timescale. An ocean containing other chemical components will have a lower freezing point, but even a water-ammonia eutectic composition will only prolong the freezing, not prevent it. If the eccentricity of Enceladus were higher (e?0.015) in the past, the increased dissipation in the ice shell may have been sufficient to maintain a liquid layer. We cannot therefore rule out the presence of a transient ocean, as a relic of an earlier era of greater heating. If the eccentricity is periodically pumped up, the ocean may have thickened and thinned on a similar timescale as the orbital evolution, provided the ocean never froze completely. We conclude that the current heat flux of Enceladus and any possible subsurface ocean is not in steady-state, and is the remnant of an epoch of higher eccentricity and tidal dissipation.     

On the tectonics of the Neocomian Rio do Peixe Rift Basin, NE Brazil: Lessons from gravity, magnetics, and radiometric data

A geophysical perspective based on well-acquired gravity, magnetic, and radiometric data provides good insights into the basin architectural elements and tectonic evolution of the Rio do Peixe Basin (RPB), an Early Cretaceous intracontinental basin in the northeast Brazilian rift system, which developed during the opening of the South Atlantic. NW–SE-trending extensional forces acting over an intensively deformed Precambrian basement yielded a composite basin architecture strongly controlled by preexisting, mechanically weak fault zones in the upper crust. Reactivated NE–SW and E–W ductile shear zones of Brasiliano age (0.6 Ga) divided the RPB into three asymmetrical half-grabens (Brejo das Freiras, Sousa, and Pombal subbasins), separated by basement highs of granite bodies that seem to anchor and distinguish the mechanical subsidence of the subbasins. Radiometric and geopotential field data highlight the relationship between the tectonic stress field and the role of a preexisting structural framework inserted in the final rift geometry. The up-to-2000 m thick half-grabens are sequentially located at the inflexion of sigmoidal-shaped shear zones and acquire a typical NE–SW-oriented elliptic shape. The Sousa Subbasin is the single exception. Because of its uncommon E–W elongated form, three-dimensional gravity modeling reveals an E–W axis of depocenters within the Sousa Subbasin framework, in which the eastern shoulders are controlled by NE–SW-trending faults. These faults belong to the Precambrian structural fabric, as is well illustrated by the gamma ray and magnetic signatures of the basement grain. Release faults were identified nearly perpendicular or oblique to master faults, forming marginal strike ramps and horst structures in all subbasins. The emplacement mechanism of Brasiliano granites around the RPB was partially oriented by the same structural framework, as is indicated by the gravity signature of the granitic bodies after removal of the gravity effect of the basin-filling deposits. The RPB major-fault occurrence along the releasing bend of a strong discontinuity – the so-called Portalegre Shear Zone – in addition to the configuration of a gentle crustal thinning, according to gravity field studies, suggests that a crustal discontinuity governs the nucleation of the RPB, followed probably by small displacement in deep crustal levels accommodating low-rate stretching during basin subsidence.     

Une carte gravimétrique haute résolution du massif du Mont-Blanc : implications structuralesA high-resolution gravity map of the Mont-Blanc massif: structural consequences

We performed a gravity survey in the Mont-Blanc and Aiguilles Rouges ranges in order to improve the gravity data coverage of the Alpine crystalline external ranges, and to constrain the deep geometry of a crustal scale thrust. Preliminary results allow us to propose a geometry for the deep structure of the ranges, taking into account a major reverse fault that bounds the Mont-Blanc range: the Mont-Blanc shear zone. To cite this article: F. Masson et al., C. R. Geoscience 334 (2002) 1011–1019.     

岩石物性与岩体结构物性研究进展

利用地球物理属性定量化研究岩体结构的成果在国内外较少见。由于风化和构造等原因,浅层岩石与一定范围内岩体的地球物理性质有很大的差别。本文从Archie公式出发介绍岩石物性研究现状,在岩体结构和工程物探研究的基础上,除了介绍岩体结构物性的概念和研究现状外,还分析了以岩心为约束条件下电阻率与波速联合的研究现状,初步探索后认为在工程上能用各种地球物理参数帮助精确描述岩体结构,因此岩体结构物性是一个新的研究方向。