太原城市化进程对城市热岛的影响

采用城市化的多项要素指标,系统考察了太原1980-2009年期间城市化的发展对其城市热岛效应的影响关系,发现城市化的发展是导致城市热岛效应形成和加剧的主要原因.认为:①近30年,太原市郊区的增温率为0.51℃/10a,市区的增温率为0.90℃/10a,热岛强度的增温率为0.39℃/10a,热岛效应不断增强;②各类城市发展指数与城市热岛效应都有很好的相关关系;③太原城郊温差和总人口对数呈线性相关关系,其长期变化相关系数为0.81;④太原城郊温差和城市房屋建筑面积对数呈线性关系,其长期变化相关系数为0.85.     

东秦岭铅锌银金钼多金属成矿带成矿规律及找矿标志

东秦岭位于华北板块与扬子板块之间的拼合带——秦岭造山带东段。该区是一典型的地球化学急变带与地球物理梯度交叉区，壳幔富含Pb，Zn，Au，Ag，W，Mo元素，为一元古宙一古生代裂陷槽，熊耳群、宽坪群、二郎坪群、耀岭河组火山岩系中的火山喷发Cu，Pb，Zn，Ag，Au矿(化)层；秦岭群、官道口群、栾川群、陶湾群滨海、浅海陆缘碎屑碳酸盐建造中强烈的火山喷(气)发活动形成的硅质条带(团块)硅质岩以及含Ag，Pb，Zn，Au矿化层状矽卡岩带，多期次的构造岩浆活动，使区内Pb，Zn，Ag，Au，W，Mo叠加富集体成矿，从而使东秦岭地区Pb，Zn，Ag，Au，W，Mo多金属矿床在区域分布、成矿空间、时间上呈现出一定的规律性和明显的找矿标志。     

硇洲岛底栖海藻的初步研究

调查了硇洲岛底栖海藻的种类组成、垂直分布特点和区系性质。硇洲岛的海藻计有４３属６７种，其中包括４０种经济海藻。马尾藻属等在潮下带构成环岛的海底林带。其区系性质属亚热带。并对合理开发利用和保护现有的海藻资源，开展经济海藻的人工养殖提出了建议。     

阿尔金造山带东段地质构造演化概论

阿尔金造山带曾是一个早古生代拗拉槽,其两侧地质体具有极为相似的地质构造特征。该区构造演化可以概括为:晚太古代至早元古代处于底侵造壳阶段,经吕梁旋回发生克拉通化,出现中元古代稳定型盖层沉积。加里东旋回中叶,经过短暂的拗拉、裂陷,分裂的塔柴板块又重新聚合。华力西旋回该区以剥蚀夷平作用为主,仅在山间断陷或山前凹陷的局部地段沉积有上泥盆统磨拉石建造。石炭纪发生短暂小规模海侵。侏罗纪全区进入陆相发育阶段。区内岩浆活动频繁,燕山旋回为最高潮。在喜山旋回,随着印度板块与欧亚板块的碰撞,该区也被卷入青藏高原总体的巨大演变之中。早期由边缘断陷转化为大型断陷盆地,至上新世湖水淹没了大部地区;晚期,随着阿尔金迅速崛起,塔里木—柴达木板块再度分裂,南盘抬升,北盘下降。文章最后探讨了阿尔金左行斜滑地震断裂带的控震作用。     

3. Solar System Formation and Early Evolution: the First 100 Million Years

The solar system, as we know it today, is about 4.5 billion years old. It is widely believed that it was essentially completed 100 million years after the formation of the Sun, which itself took less than 1 million years, although the exact chronology remains highly uncertain. For instance: which, of the giant planets or the terrestrial planets, formed first, and how? How did they acquire their mass? What was the early evolution of the “primitive solar nebula” (solar nebula for short)? What is its relation with the circumstellar disks that are ubiquitous around young low-mass stars today? Is it possible to define a “time zero” (t ₀), the epoch of the formation of the solar system? Is the solar system exceptional or common? This astronomical chapter focuses on the early stages, which determine in large part the subsequent evolution of the proto-solar system. This evolution is logarithmic, being very fast initially, then gradually slowing down. The chapter is thus divided in three parts: (1) The first million years: the stellar era. The dominant phase is the formation of the Sun in a stellar cluster, via accretion of material from a circumstellar disk, itself fed by a progressively vanishing circumstellar envelope. (2) The first 10 million years: the disk era. The dominant phase is the evolution and progressive disappearance of circumstellar disks around evolved young stars; planets will start to form at this stage. Important constraints on the solar nebula and on planet formation are drawn from the most primitive objects in the solar system, i.e., meteorites. (3) The first 100 million years: the “telluric” era. This phase is dominated by terrestrial (rocky) planet formation and differentiation, and the appearance of oceans and atmospheres.     

The origin of strain patterns resulting from contemporaneous deformation and metamorphism in the Sambagawa metamorphic belt

Abstract The magnitudes of plastic strains of 104 metacherts were determined from the deformed shape of initially spherical radiolarians in the Sambagawa high- P type metamorphic belt of Western Shikoku, Japan. The strain magnitude increases with increasing metamorphic temperature from several per cent to 250%. The a₂/a₃ ratio of strain ellipsoids in the higher metamorphic grades decreases with increasing metamorphic grade while the a₁/a₂ ratio increases rapidly. The long axis of the strain ellipsoid for every grade is nearly parallel to the length of the metamorphic belt, suggesting that the flow direction of the synmetamorphic deformation was uniform along the belt. A map of strain zones within the Sambagawa high- P type metamorphic belt reveals that the metamorphic belt underwent a progressive bulk inhomogeneous shear deformation and that the high-grade zones represent a deep-seated boundary shear zone on the accretionary wedge between a subducting oceanic plate and the immobile rigid continental plate.     

The color of the Kuiper belt Core

Recent dynamical analyses of the Kuiper belt have introduced a rigorous classification scheme, determined the mean orbital plane, and identified “Core” and “Halo” populations as a function of inclination with respect to this plane (Elliot, J.L., Kern, S.D., Clancy, K.B., Gulbis, A.A.S., Millis, R.L., Buie, M.W., Wasserman, L.H., Chiang, E.I., Jordan, A.B., Trilling, D.E., Meech, K.J., 2005. Astron. J. 129, 1117-1162). Here, we use new observations and existing data to investigate the colors of Kuiper belt objects (KBOs) within this framework. With respect to the bulk KBO color distribution (all objects for which we have B-V and V-R colors; median B-R=1.56), we find that the population of objects classified following (Elliot, J.L., Kern, S.D., Clancy, K.B., Gulbis, A.A.S., Millis, R.L., Buie, M.W., Wasserman, L.H., Chiang, E.I., Jordan, A.B., Trilling, D.E., Meech, K.J., 2005. Astron. J. 129, 1117-1162) as Classical tends to be red (B-R>1.56) while the Scattered Near population is mostly neutral (B-R<1.56). Colors of Scattered Extended and Resonant objects are consistent with the bulk distribution. Separating objects into specific resonances demonstrates that the color of the Resonant sample is dominated by KBOs in the 3:2 resonance, which is consistent with previous findings. Unlike the objects in the 3:2 resonance, however, the majority of objects in the 5:2 resonance are neutral and all but one of the objects in the 4:3, 5:3, 7:4, 2:1, and 7:3 resonances are red. In particular, the objects in the 7:4 resonance are remarkably red. We find that the colors of KBOs in the Core (low-inclination) and Halo (high-inclination) are statistically different, with Core objects being primarily red and Halo objects having a slight tendency to be neutral. Notably, virtually all of the non-Resonant Core objects are red. This combination of low inclination, unperturbed orbits and red colors in the Core may be indicative of a relic grouping of objects.     

沂水县龙泉站金矿地质特征及找矿前景

沂水县龙泉站金矿位于沂沭断裂带中段,受沂水汤头断裂控制。金矿体产于沂水汤头断裂主裂面下盘的糜棱岩化碎裂岩和花岗质碎裂岩中,已初步圈出6个金矿体。此外,在牛家小河、石崖官庄、郑家庄地区也发现有较好的矿化显示。通过综合研究,认为该地区金矿化与韧性剪切构造带关系密切,且具有较好的找矿前景。     

The surface composition of Trojan asteroids: constraints set by scattering theory

We present the results of spectral modeling of 17 Trojan asteroids. The surface composition of this group of objects (located just beyond the main belt, trapped in Jupiter's stable Lagrange points) remains uncertain due to an absence of diagnostic absorption features in their spectra. We quantitatively analyze spectra of these objects covering the range 0.3-4.0 μm using the formulation for scattering in a particulate medium developed by Hapke. Since the widest spectral range possible is desired to provide the most robust results, recently measured near-IR spectra are combined with previously published visible and near-IR data. These composite spectra are converted to and modeled in terms of geometric albedo to provide the additional constraint of the absolute brightness of the asteroids. It is important that this modeling is performed for a large number of objects, and results are derived based on trends among best-fit models. Under this rigorous examination, we find that it is unlikely that the red spectral slope is a result of organics on the surfaces, due mainly to the lack of absorptions in the L-band. Instead, anhydrous silicates adequately describe the spectral characteristics of this group of objects. A significant fraction of carbonaceous material is also likely present, but is not responsible for the red spectral slope in these models. Also, using these models, we estimate that these surfaces contain at most a few wt% of H₂O ice and no more than 10-30 wt% of hydrated silicates.