高清气象影视虚拟演播室系统设计与调试

以华风集团高清虚拟演播室建设项目为案例,论述了高清虚拟演播室技术在系统建设、系统调试、天气预报节目业务实现环节需要重点解决的几个问题和难点。根据气象电视节目制作要求,在从虚拟演播室系统系统建设到节目制作业务化的整个过程中,重点解决了音频系统延时量计算、绿箱景区施工、绿箱景区灯光布局、绿箱色键抠像调试、摄像机定位与跟踪调试、气象数据调用与转换共6个关键性技术问题。此次业务系统实践的成功是虚拟演播室技术在全国气象影视行业高清节目制作中的应用和推广的很好尝试。     

Solar cycle distribution of strong solar proton events and the related solar-terrestrial phenomena

We investigated the solar cycle distribution of strong solar proton events (SPEs, peak flux ≥1000 pfu) and the solar-terrestrial phenomena associated with the strong SPEs during solar cycles 21–23. The results show that 37 strong SPEs were registered over this period of time, where 20 strong SPEs were originated from the super active regions (SARs) and 28 strong SPEs were accompanied by the X-class flares. Most strong SPEs were not associated with the ground level enhancement (GLE) event. Most strong SPEs occurred in the descending phases of the solar cycles. The weaker the solar cycle, the higher the proportion of strong SPES occurred in the descending phase of the cycle. The number of the strong SPEs that occurred within a solar cycle is poorly associated with the solar cycle size. The intensity of the SPEs is highly dependent of the location of their source regions, with the super SPEs (≥20000 pfu) distributed around solar disk center. A super SPE was always accompanied by a fast shock driven by the associated coronal mass ejection and a great geomagnetic storm. The source location of strongest GLE event is distributed in the well-connected region. The SPEs associated with super GLE events (peak increase rate ≥100%) which have their peak flux much lower than 10000 pfu were not accompanied by an intense geomagnetic storm.     

NanoSIMS analysis of organic carbon from the Tissint Martian meteorite: Evidence for the past existence of subsurface organic‐bearing fluids on Mars

Two petrographic settings of carbonaceous components, mainly filling open fractures and occasionally enclosed in shock‐melt veins, were found in the recently fallen Tissint Martian meteorite. The presence in shock‐melt veins and the deuterium enrichments (δD up to +1183‰) of these components clearly indicate a pristine Martian origin. The carbonaceous components are kerogen‐like, based on micro‐Raman spectra and multielemental ratios, and were probably deposited from fluids in shock‐induced fractures in the parent rock of Tissint. After precipitation of the organic matter, the rock experienced another severe shock event, producing the melt veins that encapsulated a part of the organic matter. The C isotopic compositions of the organic matter (δ¹³C = ?12.8 to ?33.1‰) are significantly lighter than Martian atmospheric CO₂ and carbonate, providing a tantalizing hint for a possible biotic process. Alternatively, the organic matter could be derived from carbonaceous chondrites, as insoluble organic matter from the latter has similar chemical and isotopic compositions. The presence of organic‐rich fluids that infiltrated rocks near the surface of Mars has significant implications for the study of Martian paleoenvironment and perhaps to search for possible ancient biological activities on Mars.     

Non-axisymmetric instabilities in shocked adiabatic accretion flows

We investigate the linear stability of a shocked accretion flow on to a black hole in the adiabatic limit. Our linear analyses and numerical calculations show that, despite the post-shock deceleration, the shock is generally unstable to non-axisymmetric perturbations. The simulation results of Molteni, Tóth & Kuznetsov can be well explained by our linear eigenmodes. The mechanism of this instability is confirmed to be based on the cycle of acoustic waves between the corotation radius and the shock. We obtain an analytical formula to calculate the oscillation period from the physical parameters of the flow. We argue that the quasi-periodic oscillation should be a common phenomenon in accretion flows with angular momentum.     

Modelling of anisotropic damage in brittle rocks under compression dominated stresses

A new model for describing induced anisotropic damage in brittle rocks is proposed. Although phenomenological, the model is based on physical grounds of micromechanical analysis. Induced damage is represented by a second rank tensor, which is related to the density and orientation of microcracks. Damage evolution is related to the propagation condition of microcracks. The onset of microcrack coalescence leading to softening behaviour is also considered. The effective elastic compliance of the damaged material is obtained from a specific form of Gibbs potential. Irreversible damage‐related strains due to residual opening of microcracks after unloading are also captured. All the model's parameters could be determined from conventional triaxial compression tests. The proposed model is applied to a typical brittle rock. Comparison between test data and numerical simulations shows an overall good agreement. The proposed model is able to describe the main features related to induced microcracks in brittle geomaterials. Copyright © 2002 John Wiley & Sons, Ltd.     

辽宁庄河地区构造变形及构造演化初探

辽宁庄河地区构造活动强烈，构造变形样式多种多样，反映了在不同体制下，构造变形由下部构造层次到上部构造层次的系统变化，从早期褶皱变形到后则破裂变形过程中岩石韧性递减的系统演变。笔者利用构造解析方法，初步确定了该区的构造序列并探讨了构造演化过程。     

流体 花岗岩 金矿

流体地质研究是当代地学研究中的重要前沿课题，已成为发展地质科学、建立新的知识体系的一个主要支柱和知识生长点。本文阐述了当今国内外流体的研究现状、发展水平、流体的涵义、性质、研究方法和研究重点及其与板块构造、变质作用、岩浆作用、成矿作用、成矿作用的重要意义。流体地质为地质科学提出了许多新的研究机会和挑战。该文在简要评述当今花岗岩研究现状的基础上，对花岗岩与金矿的关系进行了深入的讨论，指出了不同成因类型的花岗岩与金矿有着完全不同的关系。人们所说的花岗岩与金矿关系多数情况下应考虑是流体作用的结果。最后指出加强流体地质研究对提高河南地质与金矿的研究水平具有十分重要的实际意义和理论意义。     

Beaming Effects in GRBs and Orphan Afterglows

The overall dynamical evolution and radiation mechanism of γ-ray burst (GRB) jets are briefly introduced. Various interesting topics concerning beaming in GRBs are discussed, including jet structures, orphan afterglows and cylindrical jets. The possible connection between GRBs and neutron stars is also addressed.     

A Two—Temperature Supernova Fallback Disk Model for Anomalous X—ray Pulsars

We present a case study of the relevance of the radially pulsational instability of a two-temperature accretion disk around a neutron star to anomalous X-ray pulsars (AXPs). Our estimates are based on the approximation that such a neutron star disk with mass in the range of 10^-6-10^-5M⊙ is formed by supernova fallback. We derive several peculiar properties of the accretion disk instability: a narrow interval of X-ray pulse periods; lower X-ray luminosities; a period derivative and an evolution time scale. All these results are in good agreement with the observations of the AXPs.