Variation and pattern in the responses of mammal faunas to Late Pleistocene climatic change in southeastern South Australia     

Amy C. Macken  Gavin J. Prideaux  Elizabeth H. Reed 《第四纪科学杂志》2012,27(4):415-424

We examined mammal occurrence and variability through the Late Pleistocene vertebrate fossil deposit of Grant Hall in Victoria Fossil Cave, Naracoorte, South Australia. To determine long‐term patterns of change, we compared the composition and relative abundance trends of the assemblage with a nearby Middle Pleistocene deposit in Cathedral Cave. Total species richness did not change through the Grant Hall sequence, dated from 93 ± 8 to 70 ± 5 ka. However, species relative abundances varied between ecologically divergent species, and in some cases between species that demonstrate similar environmental preferences. For some species this variation is comparable to that recorded in Cathedral Cave. Of those showing similar trends between the two deposits, the forest inhabitant, Pseudomys fumeus, recorded an 8.6% decline through Grant Hall, coincident with a 9.7% increase in the dry heath/mallee dweller Pseudomys apodemoides. These patterns indicate that climatic transition from relatively warm, moist to cooler, drier conditions impacted some species in similar ways through climatic cycles of the past. However, the majority of the fauna demonstrated complex responses that are individual and variable through time. Statistical tests of species trends from the Grant Hall assemblage caution that large fossil samples are required to validate patterns observed. Copyright © 2012 John Wiley & Sons, Ltd.  相似文献   

构造叠加晕结合五方位测井在甘肃省贾公台金矿寻找深部矿体中的应用          下载免费PDF全文

杨怀玉  蒙轸  刘杰  赵瑛  梁悦  贾新勇 《甘肃地质》2023,(1):20-28

贾公台金矿为甘肃党河南山地区规模最大的金矿床。为探索深部矿化、寻找盲矿体,在贾公台矿段开展原生晕研究,建立原生叠加晕轴向分带,发现贾公台金矿具反向分带特征。说明该矿体深部存在多期次成矿作用。结合地井五方位测井,预测深部3 200 m标高以下存在盲矿体。深部钻探发现了厚度大、品位高的多层金矿体,新增金资源量12吨,取得了显著找矿成果。构造叠加晕结合地井五方位测井成功圈定贾公台金矿深部矿体的实践,对同类矿床的深部找矿具有重要指导意义。  相似文献   

Rapid screening of Zr-containing particles from Chang’e-5 lunar soil samples for isotope geochronology: Technical roadmap for future study     

《地学前缘(英文版)》2022,13(3):101367

New samples returned by China Chang’e-5 (CE-5) mission offer an opportunity for studying the lunar geologic longevity, space weathering, and regolith evolution. The age determination of the CE-5 samples was among the first scientific questions to be answered. However, the precious samples, most in the micrometer size range, challenge many traditional analyses on large single crystals of zircon developed for massive bulk samples. Here, we developed a non-destructive rapid screening of individual zirconium-containing particle for isotope geochronology based on a Micro X-ray fluorescence analysis (µXRF). The selected particles were verified via scanning electron microscopy (SEM), 3D X-ray microscopy (XRM), and focused ion beam scanning electron microscopy (FIB-SEM) techniques, which showed that zirconium-bearing minerals with several microns were precisely positioned and readily suitable for site-specific isotopic dating by second ion mass spectrometry (SIMS). Such protocol could be also applicable in non-destructively screening other types of particles for different scientific purposes. We therefore proposed a correlative workflow for comprehensively studying the CE-5 lunar samples from single particles on nanometer to atomic scales. Linking various microscopic and spectromicroscopic instruments together, this workflow consists of six steps: (1) single-particle selection with non-destructive µXRF technique, (2) 2D/3D morphological and structural characterization with a correlative submicron 3D XRM and nanoscale resolution FIB-SEM imaging methods, (3) SEM analysis of the surface morphology and chemistry of the selected particle, (4) a series of microscopic and microbeam analyses (e.g., SEM, electron probe microanalysis, and SIMS) on the cross-section of the selected particle to obtain structural, mineralogical, chemical, and isotopic features from the micron to nanometer scale, (5) advanced 2D/3D characterization and site-specific sample preparation of thin foil/tip specimens on a microregion of interest in the selected particle with FIB-SEM technique, and (6) comprehensive analyses on the FIB-milled specimens at nanometer to atomic scale with synchrotron-based scanning transmission X-ray microscopy, analytic transmission electron microscopy, and atom probe tomography. Following this technical roadmap, one can integrate multiple modalities into a uniform frame of multimodal and multiscale correlated datasets to acquire high-throughput information on the limited or precious terrestrial and extraterrestrial samples.  相似文献   

未来气候情景下气候变化响应过程研究综述   总被引：7，自引：0，他引：7  

成爱芳  冯起  张健恺  李宗省  王岗 《地理科学》2015,(1)

气候变化将会对生态系统、自然资源、极端气候和人类社会产生一定的影响,科学评估未来气候变化响应是应对气候变化的前提。通过对当前研究成果的回顾,建立未来气候情景下气候变化响应研究的系统思路,并总结了研究所涉及的方法。系统论述了应用第5阶段耦合模式比较计划(CMIP5)气候模式前进行适用性评价的必要性;分析了当前降尺度方法尤其是统计降尺度的主要方法及进展;归纳了偏差校正过程中普遍使用的方法,最后,综合分析了整个研究过程中的不确定性。研究将为气候变化响应分析提供方法和思路指导。  相似文献   

CMIP5模式对辽宁省气温模拟能力及未来2℃升温阈值出现时间评估     

王涛  王乙舒  沈玉敏  王艳  赵连伟  王小桃  沈历都 《气象与环境学报》2020,36(2):49-61

利用全球气候模式、多模式集合和辽宁省气象观测数据,评估了不同典型浓度路径下19个全球气候模式和多模式集合对辽宁省气温变化模拟能力和可信度。结果表明:最优模式模拟结果优于多模式集合,具有较高的可信度。随着全球二氧化碳排放浓度增加,气温变化率和可信度呈增加趋势,首次达到2℃年份呈提前趋势,大部分站点出现在2011年之前,且出现年份越晚,升幅往往越高,反之亦然。大部分站点首次稳定到达2℃阈值开始年份在2022年之前,结束年份出现在2019—2026年,持续时间在13 a以下,开始年份均呈西早—东晚分布形势,结束时间和持续时间分布较均匀,且随着全球二氧化碳排放浓度增加,升温幅度呈上升趋势。不同典型浓度路径下各区域最高温、最低温和平均气温出现年份和变化特征均比较一致。  相似文献   

两步保形平流方案在高分辨率球面经纬网格下的跳点差分试验   总被引：1，自引：0，他引：1  

张祎  宇如聪  李建  陈昊明 《气象学报》2013,71(6):1089-1102

尝试用一个基于有限差分的两步保形平流方案（TSPAS）替代美国国家大气研究中心第5版公用大气模式（NCAR-CAM5）欧拉-谱动力框架中的半拉格朗日传输（SLT）平流方案,并针对不同分辨率版本,计算水汽等物质的传输过程。通过设计保证守恒性的跳点差分法,解决了基于经纬网格的模式在高分辨率下由于极区纬向格距过小而造成的差分方案积分时间步长过短的问题,使得TSPAS在高分辨率下仍然可以使用较大的时间步长。理想试验表明：（1）跳点TSPAS在守恒性、数值精度（量级上）、保形性等方面均较好地保持了原TSPAS的特点,而积分步长可增大到与CAM5-SLT相同,比原TSPAS提高超过一个数量级;（2）较半拉格朗日传输方案,尽管TSPAS的耗散更大,但是在相同时间步长下更省时,且改进了半拉格朗日传输求解平流方程造成的不守恒问题。CAM5的比较试验表明：（1）采用跳点TSPAS的模式结果与非跳点计算结果相当,在高纬度跳点区域也并未出现模拟异常;（2）在高分辨率下,采用跳点TSPAS方案的CAM5模拟结果与原模式结果相近,并初步显示对东亚青藏高原南侧的虚假降水有所抑制。该工作确保了基于欧拉通量差分型的TSPAS在高分辨率模式下的大时间步长稳定积分,为解决有限差分方法在高分辨率模式发展中的相关计算问题提供了启示,为后续针对东亚地区的模式性能改进奠定了基础。  相似文献   

利用WRF-Chem模拟研究京津冀地区夏季大气污染物的分布和演变   总被引：9，自引：4，他引：5  

庞杨  韩志伟  朱彬  李嘉伟 《南京气象学院学报》2013,(6):674-682

应用WRF—Chem（Weather Research and Forecasting Model with Chemistry）模式模拟研究了2007年8月京津冀地区近地面O3、NO2、PM2.5浓度的时空变化特征,将模拟结果与观测数据进行详细对比,结果表明,模式可以较好地模拟O3、PM2.5,浓度的空间分布和时间变化特征,成功再现了8月33和PM2.5的几次积累增加过程,其中O,的模拟值与观测值的相关系数为0．69～0．86,PM2.5的相关系数为0．44～0．49,但模式对NO2的模拟相对较差,相关系数为0．27～0．43。北京、天津地区为O3月均低值区,月均体积浓度约30×10^-9,渤海及京津冀以西地区O3月平均体积浓度可达60×10^-9;PM2,呈现南高北低的分布特征,变化范围为120～240μg／m3。14时月平均03体积浓度在北京、天津地区低于周边地区,约为60×10^-9;而PM2.5质量浓度在环渤海地区和河北南部较高,为100～120μg/m^3。8月17日北京出现一次典型的高浓度O,污染事件,14时北京地区温度达到33℃,O3体积浓度为80×10^-9～110×10^-9。在局地排放、化学反应和外来输送的共同作用下,渤海西岸和北岸PM2.5的质量浓度超过120μg／m3,其中二次气溶胶质量浓度为50～100μg／m3,一次排放人为气溶胶质量浓度为10～20μg／m3,海盐质量浓度为1～7μg／m3,二次气溶胶是该地区PM2.5的主要贡献者。  相似文献   

Poleward expansion of the hadley circulation in CMIP5 simulations   总被引：1，自引：0，他引：1  

胡永云  陶利军  刘骥平 《大气科学进展》2013,30(3):790-795

Observational analyses have demonstrated that the Hadley circulation has expanded poleward in recent decades. Important issues are what caused the widening of the Hadley circulation and whether the observed widening is related to anthropogenic forcing. In the present study, we use currently available simulations of the Coupled Model Intercomparison Project Phase-5 (CMIP5) to analyze changes in the width of the Hadley circulation. It is found that CMIP5 historical simulations with greenhouse gas (GHG) forcing generate a total widening of ～0.15o0.06o in latitude (10 yr)-1 for the period 1979--2005, and the widening in CMIP5 historical simulations with all forcings is ～0.17o0.06o per decade. Similar to that in CMIP3, the simulated poleward expansion in CMIP5 is much weaker than the observational reanalyses. In CMIP5 projection simulations for the 21st century, magnitudes of widening of the Hadley circulation increase with radiative forcing. For the extreme projected radiative forcing of RCP8.5, the total annual-mean widening of the Hadley circulation is ～0.27o0.04o(10 yr)-1 in the 21st century. Although CMIP5 underestimates observed poleward expansion of the Hadley circulation, the results of this study suggest that the observed trends in the width of the Hadley circulation are caused by anthropogenic forcing and that increasing GHGs play an important role in the observed poleward expansion of the Hadley circulation, in addition to other forcings emphasized in previous studies.  相似文献   

用于风电场功率预测的逐时风速预报   总被引：1，自引：0，他引：1  

白龙  吴息  丁宇宇  丁杰  江燕如 《气象科技》2013,41(4):777-783

为满足风电场精细化风速预报的需要,利用MM5模式的格点输出数值预报产品以及福建沿海地区两座海上测风塔的逐时气象资料,采用逐步回归的统计方法,将MM5数值预报产品与测风塔实测气象资料要素指标值共同引入回归方程,拟合两座测风塔特定高度的逐小时风速预报方程,详细介绍了该方法的实现过程.通过一年的预报效果指标以及15日的独立样本效果检验,结果表明该方法对于逐小时风速的预报有一定的应用价值.  相似文献   

Time‐series high‐resolution spectroscopy and photometry of ε Aurigae from 2006–2013: Another brick in the wall     

K. G. Strassmeier  M. Weber  T. Granzer  L. Schanne  J. Bartus  I. Ilyin 《Astronomische Nachrichten》2014,335(9):904-934

We present continuous and time‐resolved R = 55 000 optical échelle spectroscopy of ε Aurigae from 2006–2013. Data were taken with the STELLA Echelle Spectrograph of the robotic STELLA facility at the Observatorio del Teide in Tenerife. Contemporaneous photometry with the Automatic Photoelectric Telescopes at Fairborn Observatory in Arizona is presented for the years 1996–2013. Spectroscopic observations started three years prior to the photometric eclipse and are still ongoing. A total of 474 high‐resolution échelle spectra are analyzed and made available in this paper. We identify 368 absorption lines of which 161 lines show the characteristic sharp disk lines during eclipse. Another 207 spectral lines appeared nearly unaffected by the eclipse. From spectrum synthesis, we obtained the supergiant atmospheric parameters T_eff = 7395 ± 70 K, log g ≈ 1, and [Fe/H] = +0.02 ± 0.2 with ξ_t = 9 km s^–1, ζ_RT = 13 km s^–1, and v sin i = 28 ± 3 km s^–1. The residual average line broadening expressed in km s^–1 varies with a period of 62.6 ± 0.7 d, in particular at egress and after the eclipse. Two‐dimensional line‐profile periodograms show several periods, the strongest with ≈110 d evident in optically thin lines as well as in the Balmer lines. Center‐of‐intensity weighted radial velocities of individual spectral lines also show the 110‐d period but, again, additional shorter and longer periods are evident and are different in the Balmer lines. The two main spectroscopic Hα periods, ≈ 116 d from the line core and ≈ 150 d from the center‐of‐intensity radial velocities, appear at 102 d and 139 d in the photometry. The Hβ and Johnson V I photometry on the other hand shows two well‐defined and phase‐coherent periods of 77 d and 132 d. We conclude that Hα is contaminated by changes in the circumstellar environment while the Hβ and V I photometry stems predominantly from the non radial pulsations of the F0 supergiant. We isolate the disk‐rotation profile from 61 absorption lines and found that low disk eccentricity generally relates to low disk rotational velocity (but not always) while high disk eccentricity always relates to high velocity. There is also the general trend that the disk‐absorption in spectral lines with higher excitation potential comes from disk regions with higher eccentricity and thus also with higher rotational velocity. The dependency on transition probability is more complex and shows a bi‐modal trend. The outskirts of the disk is distributed asymmetrically around the disk and appears to have been built up mostly in a tail along the orbit behind the secondary. Our data show that this tail continues to eclipse the F0 Iab primary star even two years after the end of the photometric eclipse. High‐resolution spectra were also taken of the other, bona‐fide, visual‐binary components of ε Aur (ADS 3605BCDE). Only the C‐component, a K3‐4‐giant, appears at the same distance than ε Aur but its radial velocity is in disagreement with a bound orbit. The other components are a nearby (≈ 7 pc) cool DA white dwarf, a G8 dwarf, and a B9 supergiant, and not related to ε Aur. The cool white dwarf shows strong DIB lines that suggest the existence of a debris disk around this star. (© 2014 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)  相似文献