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长江口地区地面沉降的深部动力学机制分析

地表变形、活动断裂和地球物理的综合分析表明,菲律宾洋壳向欧亚大陆的俯冲导致的地幔对流是控制中国东部沿海地区晚新生代以来构造作用的主导因素,是长江口地区地面沉降的主要深部动力学机制。由于地幔对流和青藏高原挤压共同作用导致的地壳热流值的差异则是长江口地区西部隆升、东部沉降且向东沉降速率增大的直接驱动力。预测未来长江口地区的基岩沉降范围将以>10cm/a的速率向西扩大,沉降速率将呈明显加速趋势,40000a之内上海市可能被海水淹没,但板块构造演化的“渐变”特征决定其对当地未来的人类活动不会造成显著影响。根据“地壳均衡理论”,建议在长江口南西部(浙江省北东部)的丘陵山区加大重力载荷如加快城市化进程或人工造山以减小和控制上海地区的沉降。     

辽南早元古宙变质热液型金矿床成矿机理探讨

辽南早元古宙辽河群变质岩系中的金矿床为变质热液成因金矿床,矿床的形成与吕梁期变质变形作用关系密切。金矿化带的展布与金矿体的产出受韧性剪切带控制。剪切带内岩石具有明显的动态性组构特征,直接赋矿围岩为辽河群盖县组糜棱岩化千枚岩、变砂岩及云母石英糜棱岩等。韧性剪切带为含矿流体的运移提供通道。作者定义这类金矿床为变质热液型含金剪切带金矿床。     

A Note on the Mixing Length Theory and Massive Star Evolution

1 INTRODUCTIONThe mixing length theory (MLT) for stellar convection originally developed by Vitense(1953, 1958) has been the most popularly used local convection theory in the studies of stellarstructure and evolution. The theory was later modified and revised by many investigators,who suggested some different expressions. In fact, MLT is not a real hydrodynamic theory,rather, it is a simple "ballistic" theory which traces the motion of imaginary convective elements. In reality j stell…     

Corrections to Solar Thermal Structure when a Turbulent Magnetic Field is Included

Correction of non-ideal effect due to a magnetic fluctuating tensor is derived from the ideal MHD equations. The inclusion of a magnetic turbulent field leads to modifications of the hydrostatic equilibrium equation and thermodynamical variables such as the temperature T, the adiabatic exponent γ, the adiabatic temperature gradient △↓ad and the temperature gradient △↓. In particular, the modifications in the adiabatic and radiative temperature gradients will result in a change in the Schwarzchild criterion, hence in the location of the base of the convective zone. Incorporating the modifications, we construct a modified thermodynamical equilibrium structure of the Sun.     

Characteristics of convection and overshooting in RGB and AGB stars

Based on the turbulent convection model (TCM) of Li & Yang, we have studied the characteristics of turbulent convection in the envelopes of 2 and 5M⊙ stars at the red giant branch and asymptotic giant branch phases. The TCM has been successfully applied over the entire convective envelopes, including the convective unstable zone and the overshooting regions. We find that the convective motions become progressively stronger when the stellar models are located farther up along the Hayashi line. In the convect...     

Convective-conductive transitions and sensitivity of a convecting ice shell to perturbations in heat flux and tidal-heating rate: Implications for Europa

We investigate the response of conductive and convective ice shells on Europa to variations of heat flux and interior tidal-heating rate. We present numerical simulations of convection in Europa's ice shell with Newtonian, temperature-dependent viscosity and tidal heating. Modest variations in the heat flux supplied to the base of a convective ice shell, ΔF, can cause large variations of the ice-shell thickness Δδ. In contrast, for a conductive ice shell, large ΔF involves relatively small Δδ. We demonstrate that, for a fluid with temperature-dependent viscosity, the heat flux undergoes a finite-amplitude jump at the critical Rayleigh number Racr. This jump implies that, for a range of heat fluxes relevant to Europa, two equilibrium states—corresponding to a thin, conductive shell and a thick, convective shell—exist for a given heat flux. We show that, as a result, modest variations in heat flux near the critical Rayleigh number can force the ice shell to switch between the thin, conductive and thick, convective configurations over a ∼10⁷-year interval, with thickness changes of up to ∼10-30 km. Depending on the orbital and thermal history, such switches might occur repeatedly. However, existing evolution models based on parameterized-convection schemes have to date not allowed these transitions to occur. Rapid thickening of the ice shell would cause radial expansion of Europa, which could produce extensional tectonic features such as fractures or bands. Furthermore, based on interpretations for how features such as chaos and ridges are formed, several authors have suggested that Europa's ice shell has recently undergone changes in thickness. Our model provides a mechanism for such changes to occur.