天堂山花岗质岩石条带状构造的成因与演化

天堂山地区花岗质岩石中条带状构造异常发育,据成因可分为分异条带状构造和构造置换———复合条带状构造两种类型。它们的形成与岩石变形变质作用有密切关系,形成和演化过程可分为３个阶段：递进变形变质阶段;重熔活化阶段;构造置换改造阶段。分异条带状构造是岩石在递进变形变质作用过程中具不同熔点的矿物发生分离和分异形成的;构造置换———复合条带状构造是重熔活化阶段形成的长英质脉体和先期分异条带一起又受到强烈的构造置换改造,发生平行化而成。     

胶南造山带变质岩系中角闪石的初步研究

本文对胶南造山带变质岩系中角闪石的基本特征及形成条件进行了初步研究,根据不同地质单元中角闪石的类型、赋存状态、矿物组合等矿物学特点及电子探针分析结果,认为该区角闪石主要属钙质角闪石亚类。其形成的温压范围是：温度５４５～８０６．５℃,压力主要在０．２５～１．２ＧＰａ之间     

松潘—甘孜造山带中丹巴地区变质岩演化及其地质意义

丹巴地区位于松潘—甘孜造山带中部。区域动热变质作用主要发生于印支晚期—喜马拉雅早期,与深层滑脱-逆冲作用有关。根据特征矿物组合．丹巴地区变质岩可划分出六个变质带：绢云母—绿泥石带、黑云母带、石榴子石带、十字石带、蓝晶石带和夕线石带。石榴子石生长环带代表每段时间矿物晶体边部的平衡,可用于推测石榴子石生长时的P－t轨迹。利用石榴子石—黑云母温度计和石榴子石—斜长石—Al2SiO5-石英压力计得到石榴子石的参考温度、压力,根据环带定量计算得到的变质作用p-t轨迹为顺时外形式,与其所处的构造背景为大陆碰撞造山带是一致的。     

涟源煤盆地测水组煤系的X射线衍射特征

通过对湘中涟源煤盆地测水组煤及其顶板泥岩的Ｘ射线衍射分析可知,区域岩浆热变质作用是湘中涟源煤盆地测水组煤系变质的主要原因,对测水组煤系化学结构影响较大,动力变质作用仅起局部和次要作用。     

非洲西北部的In Ouzzal麻粒岩带

非洲西北部的InOuzzal麻粒岩带是太古宙地体,以构造窗形式出现在新元古代的泛非造山带中。基底岩石主要是2．7Ga前的TTG岩套以及后来的侵入体,表壳岩有绿岩带和变质沉积岩,在20Ga的比里姆（Biriman）期发生了极高温的变质作用（P≈12×108Pa,T≈1100℃）,具有顺时针的PTt轨迹。在后来的泛非期,该带两侧叠加了糜棱岩化作用,形成了热液型的世界级金矿床。大部分研究者认为该地体是地壳深处岩石的地表露头,对研究地壳的形成、演化及相应的大陆裂解和碰撞有非常重要的意义。     

Global solutions of adiabatic accretion flows with isothermal shocks in Kerr black hole geometry

This paper presents global solutions of adiabatic accretion flows with isothermal shocks in Kerr black hole geometry. It is known that in the previously studied cases, where the flow including the shock is either entirely adiabatic or entirely isothermal, there can be no more than one stable shock solution, and the solution can only be of α –x type. However, the solution topology in the present case shows remarkable new characteristics: for the same flow parameters there can be two stable shock solutions satisfying physical boundary conditions, and the solution can be of three types, namely α– x , x –α and α–α type. In addition, shocks in the present case occur for a parameter region different from that for Rankine–Hugoniot shocks. These results greatly increase the possibilities of shock formation in astrophysical flows. It is also significant that the effects of frame-dragging of a rapid Kerr black hole on the shock formation are discovered. Finally, a brief comparison is made between shocked inviscid flows and two types of shock-free viscous flows, namely those of Shakura & Sunyaev and Narayan & Yi, and some comments are made about the fact that numerous authors who have studied transonic global solutions of accretion flows have found no shocks.     

A new plasmon solution with centrifugal pressure

The 'plasmon' solution of De Young & Axford describes the interaction between a high-velocity clump and the surrounding medium. Even though this solution is probably too simplistic, it has proven to be most useful in the study of diverse astrophysical flows. In the present paper, we discuss a more detailed solution of the plasmon problem, which includes the centrifugal effects of the environmental material flowing around the plasmon. We derive both numerical and approximate analytic solutions of this problem, and compare them with the analytic solution of De Young & Axford.     

Radiative steady-state colliding stellar wind models: are they correct?

The properties of radiative steady-state colliding stellar winds in binary systems are studied. It is shown that the presence of a singularity at the stagnation point has a major influence on the structure of these flows. This problem is of great importance if their stability properties are considered. None of the existing models treats this mathematical problem properly, and special efforts must be undertaken in the future in order to come to a firm conclusion about the physical nature of possible instabilities. At the moment, neither numerical nor analytical models can be considered to be of acceptable accuracy in the case of highly radiative steady-state colliding stellar winds.     

Smoothed particle hydrodynamic simulations of viscous accretion discs around black holes

Viscous Keplerian discs become sub-Keplerian close to a black hole since they pass through sonic points before entering into it. We study the time evolution of polytropic viscous accretion discs (both in one- and two-dimensional flows) using smoothed particle hydrodynamics. We discover that for a large region of the parameter space spanned by energy, angular momentum and polytropic index, when the flow viscosity parameter is less than a critical value, standing shock waves are formed. If the viscosity is very high then the shock wave disappears. In the intermediate viscosity, the disc oscillates very significantly in the viscous time-scale. Our simulations indicate that these centrifugally supported high density regions close to a black hole play an active role in the flow dynamics, and consequently, the radiation dynamics.