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1.
冰封期达里诺尔湖同位素与营养盐分布特征及关系的定量分析 总被引：1，自引：0，他引：1
以内蒙古高原的达里诺尔湖为研究对象,对其在冰封期湖水不同相态下总氮(TN)、总磷(TP)浓度以及氢、氧同位素比值的分布特征和定量关系进行初步研究.结果表明:1)在冰封期,达里诺尔湖水体中营养盐的平均浓度相对较高,已远超过国家Ⅴ类水质标准.水体中TN、TP浓度均大于其在对应冰体中的浓度,均值分别是对应冰体中的9.91、3.11倍,说明低温冷冻过程对达里诺尔湖水体中的氮、磷具有浓缩效应.而通过与非冰封期的对比发现,湖冰的排氮效应强于磷.2)冰封期由于结冰过程中同位素热力学分馏明显,加之贡格尔河的入流补给,使得达里诺尔湖冰体中的氢、氧同位素比值远高于水体中的比值,同时,随冰层的加深,同位素逐渐偏重.3)冰封期达里诺尔湖水体及冰体中,同位素比值与营养盐浓度均呈显著负相关,水体的相关性较冰体要好,在冰层中,随着冰层的加深相关性越明显.利用SPSS统计软件分析发现同位素比值与营养盐浓度的相关关系显著,水体中最大相关系数达到0.991,冰体中达到0.988;氢同位素(D)与TN、TP浓度的关系式分别为:TN=-0.2825δD-6.0083和TP=-0.0805δD-1.2395,这为研究湖泊营养盐的时空变化规律提供新的手段和理论. 相似文献
2.
本文分别基于数值结果和地质学模型,在假定地球的上地幔存在稳定Rayleigh-Bénard对流的基础上,模拟了直径为10 km（陨石坑直径约180 km,以Chicxulub为例）和直径为100 km（陨石坑直径约1000 km）的小行星撞击对地球的上地幔对流格局的影响.本文将直径10 km小行星的撞击效果等效为热异常,将直径100 km小行星的撞击效果等效为热异常和速度异常（主要指陨石坑底部的回弹）的叠加.计算结果表明,当小行星的直径在10 km左右时,撞击对上地幔对流的影响十分微弱,热扰动时间仅2—3 Ma;而当小行星的直径达到100 km时,撞击就会对上地幔对流产生强烈影响.这时,对流从扰动到新的稳态有一定模式可循（依次为：调整、多个对流环、调整、稳定）,扰动的持续时间受黏度和撞击点位置影响,同时稳定后地幔热柱会向着撞击点的方向产生一定的位移. 相似文献
3.
文中对含两种不相混流体的饱和孔隙介质模型进行了波场模拟,该模型基于封闭型系统假设,考虑了流相与固相的相对运动和孔隙率、饱和度(毛细管压力)的松弛机制,可以较好的模拟波场的数值衰减。与目前常用的等效流体方法和基于开敞系统假设的非饱和孔隙介质模型相比,更符合勘探阶段的实际情况。前人对该介质模型平面波的速度和衰减做了一定的研究,但对整个波场的计算研究还未见报道。本文推导了该模型包含毛细管压力和孔隙度松弛机制的波动方程,并利用有限元的方法进行了波场模拟,并对波场特征进行了分析。数值模拟结果表明,在地震频段,非湿相位移波场中慢波p3较为清晰;毛细管压力(饱和度)和孔隙度的松弛效应对非湿相流体位移有较大影响,随松弛系数的增大,位移减小。 相似文献
4.
西南印度洋中脊为典型的超慢速扩张洋中脊,其岩浆补给具有不均匀分布的特征.洋壳厚度是洋中脊和热点岩浆补给的综合反映,因此反演洋壳厚度是研究大尺度洋中脊和洋盆岩浆补给过程的一种有效方法.本文通过对全球公开的自由空气重力异常、水深、沉积物厚度和洋壳年龄数据处理得到剩余地幔布格重力异常,并反演西南印度洋地区洋壳厚度,定量地分析了西南印度洋的洋壳厚度分布及其岩浆补给特征.研究发现,西南印度洋洋壳平均厚度7.5 km,但变化较大,标准差可达3.5 km,洋壳厚度的频率分布具有双峰式的混合偏态分布特征.通过分离双峰统计的结果,将西南印度洋洋壳厚度分为0~4.8 km的薄洋壳、4.8~9.8 km的正常洋壳和9.8~24 km的厚洋壳三种类型,洋中脊地区按洋壳厚度变化特征可划分为7个洋脊段.西南印度洋地区薄洋壳受转换断层控制明显,转换断层位移量越大,引起的洋壳减薄厚度越大,减薄范围与转换断层位移量不存在明显相关性.厚洋壳主要受控于该区众多的热点活动,其中布维热点、马里昂热点和克洛泽热点的影响范围分别约340 km,550 km和900 km.Andrew Bain转换断层北部外角形成厚的洋壳,具有与快速扩张洋中脊相似的转换断层厚洋壳特征. 相似文献
5.
陨石坑或撞击坑(impact crater)是小行星、彗星和流星体等小天体超高速撞击行星及其卫星表明形成的凹坑或环状地质构造。由于大气层的保护,和其他星球相比,地球遭受到陨石撞击的可能性要低得多。可即便如此,据估计,在地球形成演化的过程中,出现过直径大于10 km的陨石撞击构造不少于1500个,而直径更小的陨石坑数量就更多了! 相似文献
6.
本文对布设在华北克拉通三个陆块的199个宽频带台站记录的远震数据进行了接收函数计算.利用H-κ迭代方法获得了该区域基岩地区的地壳结构,平滑处理后作为背景结构模型中的基岩地区地壳结构;利用相邻算法对沉积层地区的接收函数进行了波形拟合计算,获得了沉积层结构,平滑后作为背景结构模型中的沉积层结构;结合前人的研究成果,完善了研究区域的背景结构模型.以此模型为基础,对接收函数进行了CCP（Common Conversion Point,共转换点）叠加成像,获得了Moho面成像结果,对比沉积层的成像结果发现：西部陆块中鄂尔多斯块体东部地区地壳厚度较大,约为42 km,泊松比较低,小于0.24,为长英质含量较多的地壳层;位于中部陆块的山西地堑地壳厚度小于鄂尔多斯块体,且变化较大,西侧地壳厚度约为40 km,东侧重力梯度带附近地壳厚度迅速减薄至36 km左右,张家口-怀来-大同一带出现了地壳的局部抬升,地壳厚度等值线基本以北北东方向为主,与构造带方向基本一致,地堑内泊松比约为0.26~0.28,前人对此区域的层析成像研究结果表明太行山隆起和阴山隆起存在壳内低速层,推测为地壳部分熔融以及上地幔物质上涌造成的;东部陆块中渤海湾盆地的地壳厚度较薄,约为32 km,部分地区小于30 km,其中冀中坳陷带地壳厚度最薄,约为28 km,沉积层基底分布与Moho面分布呈镜像对称趋势,沉积层较厚地区的地壳较薄,推测东部陆块在太平洋板块俯冲作用下,存在北西-南东向的拉张作用,使其内发育了大量断陷盆地. 相似文献
7.
基于有限元方法对岫岩罗圈里陨石坑地形对地震反应的影响进行了探索。结合文献资料、岩土勘察工作建立了岫岩罗圈里陨石坑二维有限元分析模型。选用粘弹性人工边界和等效节点力输入方法解决了有限元模拟半空间无限域时的边界问题和地震动输入问题。为了突出地形因素的影响,采用弹性材料介质进行数值模拟分析,并与水平场地模型的分析结果进行了对比。数值模拟结果和对比表明:罗圈里陨石坑地形对于陨石坑中部的地震动有显著的放大作用,远高于水平场地模型。此外,盆地中部短周期部分的反应谱也明显高于盆地边缘和水平一维场地模型,这是导致海城地震中盆地中部自振周期较短的单层房屋破坏明显严重的主要原因。 相似文献
8.
本文利用30个基准台所记录的238条长周期面波资料,经过适配滤波和分格频散反演,得到中国大陆及邻区147个分格10-105s的纯路径频散,进而反演出青藏高原及邻近地区深至170km的剪切波三维速度结构.研究表明,青藏高原中西部地区和东部地区的地壳平均厚度分别为70±7km和65±7km,地壳平均剪切波速度分别为3.55和3.62km/s,上地幔顶盖平均速度分别为4.63和4.61km/s; 岩石层厚度均为120±10km;东部地区下地壳内30-40km深度处普遍存在低速层;青藏高原及其东侧的上地幔低速层内有横贯东西且明显向上隆起的低速腔.滇西缅北地区的地壳厚45±5km,上地壳及下地壳内都有低速层;上地幔顶盖的速度为4.42km/s,比青藏高原本体及恒河平原都低.恒河平原地壳厚34±2km,速度平均为3.45km/s;上地幔顶盖厚86±10km,速度平均为4.63km/s,顶盖内55-83km深处有一个低速夹层. 相似文献
9.
频率域全波形反演是重要的地震成像方法,而频率域波动方程数值模拟是频率域全波形反演的基础.对于大规模的问题,由于受存储和计算量的限制,基于LU分解的直接方法一般不再适用,而是采用迭代方法.基于多重网格预条件的双共轭梯度稳定化方法是一种重要的迭代方法.本文重点讨论了多重网格预条件求解过程中的松弛因子选择方法,研究结果表明,(1)对于一般选取的松弛因子,随模型复杂性的增加,所能计算的重数逐渐下降,方法的实用性也随之下降;(2)对于复杂模型,采用局部模式分析方法选取松弛因子,提高了所能计算的重数,保证了多重网格方法的收敛性和实用性.这些研究成果对基于多重网格预条件的迭代算法的实际应用具有重要意义. 相似文献
10.
本文基于中国地震观测台网记录到的震中距为10°~23°之间琉球俯冲区一个中深源地震的P波三重震相信息,研究了下扬子克拉通转换带顶部P波速度结构.通过射线追踪和理论地震图与观测地震波形的对比,发现下扬子克拉通下方的410 km间断面为一厚度20 km的梯度带,其上存在一由西南向东北变厚的低速层,厚度变化40~57 km,P波速度减低2.7%~4.5%.该低速层可以被认为是由于地幔橄榄岩部分熔融引起的. 相似文献
11.
Richard J. Pike 《Earth and Planetary Science Letters》1974,23(3):265-271
Amendments to a quantitative scheme developed by T.R. McGetchin et al. (1973) for predicting the distribution of ejecta from lunar basins yield substantially thicker estimates of ejecta, deposited at the basin rim-crest and at varying ranges byond, than does the original model. Estimates of the total volume of material ejected from a basin, illustrated by Imbrium, also are much greater. Because many uncertainties affect any geometric model developed primarily from terrestrial analogs of lunar craters, predictions of ejecta thickness and volume on the Moon may range within at least an order of magnitude. These problems are exemplified by the variability ofT, thickness of ejecta at the rim-crest of terrestrial experimental craters. The proportion ofT to crater rim-height depends critically upon scaled depth-of-burst and whether the explosive is nuclear or chemical. 相似文献
12.
Experimentally produced impact craters in limestone targets displayed millimeter-sized shatter cones within crater spallation zones. The craters have been produced by accelerating spherical metal projectiles by means of a light-gas gun. Variation of the impact velocity showed that at about 3 km/s shatter cone formation starts and is reproducible at any higher impact velocities. In most cases the cone apices were pointing in the direction of the impact center. The occurrence of shatter cones directly at the target surface (spallation zones of craters) does not support a theoretical model on shatter cone formation published by Gash (1971). 相似文献
13.
Wataru Kanda Yoshikazu Tanaka Mitsuru Utsugi Shinichi Takakura Takeshi Hashimoto Hiroyuki Inoue 《Journal of Volcanology and Geothermal Research》2008
The 1st crater of Naka-dake, Aso volcano, is one of the most active craters in Japan, and known to have a characteristic cycle of activity that consists of the formation of a crater lake, drying-up of the lake water, and finally a Strombolian-type eruption. Recent observations indicate an increase in eruptive activity including a decrease in the level of the lake water, mud eruptions, and red hot glows on the crater wall. Temporal variations in the geomagnetic field observed around the craters of Naka-dake also indicate that thermal demagnetization of the subsurface rocks has been occurring in shallow subsurface areas around the 1st crater. Volcanic explosions act to release the energy transferred from magma or volcanic fluids. Measurement of the subsurface electrical resistivity is a promising method in investigating the shallow structure of the volcanic edifices, where energy from various sources accumulates, and in investigating the behaviors of magma and volcanic fluids. We carried out audio-frequency magnetotelluric surveys around the craters of Naka-dake in 2004 and 2005 to determine the detailed electrical structure down to a depth of around 1 km. The main objective of this study is to identify the specific subsurface structure that acts to store energy as a preparation zone for volcanic eruption. Two-dimensional inversions were applied to four profiles across the craters, revealing a strongly conductive zone at several hundred meters depth beneath the 1st crater and surrounding area. In contrast, we found no such remarkable conductor at shallow depths beneath the 4th crater, which has been inactive for 70 years, finding instead a relatively resistive body. The distribution of the rotational invariant of the magnetotelluric impedance tensor is consistent with the inversion results. This unusual shallow structure probably reflects the existence of a supply path of high-temperature volcanic gases to the crater bottom. We propose that the upper part of the conductor identified beneath the 1st crater is mainly composed of hydrothermally altered zone that acts both as a cap to upwelling fluids supplied from deep-level magma and as a floor to infiltrating fluid from the crater lake. The relatively resistive body found beneath the 4th crater represents consolidated magma. These results suggest that the shallow conductor beneath the active crater is closely related to a component of the mechanism that controls volcanic activity within Naka-dake. 相似文献
14.
Understanding explosive volcanic eruptions, especially phreatomagmatic eruptions, their intensities and energy budgets is of major importance when it comes to risk and hazard studies. With only a few historic occurrences of phreatomagmatic activity, a large amount of our understanding comes from the study of pre-historic volcanic centres, which causes issues when it comes to preservation and vegetation. In this research, we show that using 3D geometrical modelling it is possible to obtain volume estimates for different deposits of a pre-historic, complex, monogenetic centre, the Mt. Gambier Volcanic Complex, south-eastern Australia. Using these volumes, we further explore the energy budgets and the magnitude of this eruption (VEI 4), including dispersal patterns (eruption columns varying between 5 and 10 km, dispersed towards north-east to south), to further our understanding of intraplate, monogenetic eruptions involving phreatomagmatic activity. We also compare which thermodynamic model fits best in the creation of the maar crater of Mt. Gambier: the major-explosion-dominated model or the incremental growth model. In this case, the formation of most of the craters can best be explained by the latter model. 相似文献
15.
Gareth S. Collins Joanna Morgan Penny Barton Gail L. Christeson Sean Gulick Jaime Urrutia Michael Warner Kai Wünnemann 《Earth and Planetary Science Letters》2008,270(3-4):221-230
We investigate the cause of terrace zone asymmetry in the Chicxulub impact crater using dynamic models of crater formation. Marine seismic data acquired across the crater show that the geometry of the crater's terrace zone, a series of sedimentary megablocks that slumped into the crater from the crater rim, varies significantly around the offshore half of the crater. The seismic data also reveal that, at the time of impact, both the water depth and sediment thickness varied with azimuth around the impact site. To test whether the observed heterogeneity in the pre-impact target might have affected terrace zone geometry we constructed two end-member models of upper-target structure at Chicxulub, based on the seismic data at different azimuths. One model, representing the northwest sector, had no water layer and a 3-km thick sediment layer; the other model, representing the northeast sector, had a 2-km water layer above a 4-km sediment layer. Numerical models of vertical impacts into these two targets produced final craters that differ substantially in terrace zone geometry, suggesting that the initial water depth and sediment thickness variations affected the structure of the terrace zone at Chicxulub. Moreover, the differences in terrace zone geometry between the two numerical models are consistent with the observed differences in the geometry of the terrace zone at different azimuths around the Chicxulub crater. We conclude that asymmetry in the pre-impact target rocks at Chicxulub is likely to be the primary cause of asymmetry in the terrace zone. 相似文献
16.
17.
A.W. Gerhard Kunze 《Physics of the Earth and Planetary Interiors》1974,8(4):375-387
The settling trends of 318 lunar mare craters are compared with predictions of numerical finite-element models in order to determine the creep response of the upper lunar mare crust. No settling is evident in craters smaller than 5 km in diameter. Settling rates of larger craters increase as function of crater size in a manner suggesting a non-linear lunar creep response corresponding to the power law where έ is the strain rate and σ is the differential stress. However, the observed nonlinearity is probably an apparent nonlinearity resulting from the temperature induced viscosity decrease with depth due to a lunar crustal temperature gradient of 3° C/km and a creep activation energy of 20 kcal/mole. It is concluded that creep in the lunar medium is essentially Newtonian, and that the effective viscosity of the upper lunar mare crust is (1.6 ± 0.3) · 1025 poise. 相似文献
18.
Most of the known pit craters in Hawaii occur along the East and Southwest Rift Zones of Kilauea volcano. The pit craters typically are either astride a single rift zone fracture or between a pair of rift zone fractures. These fractures are prominent in the pit crater walls. The pit craters are elliptical in plan view, with their major diameters ranging from 8 to 1140 m. They range in depth from 6 m to 186 m. They typically develop with initially steep, locally overhanging walls, but as the walls collapse, the craters fill with talus and become shaped like inverted elliptical cones. None of the craters apparently formed as eruptive vents, although some have been subsequently filled by lava. Devil's Throat is the best-exposed pit crater along the East Rift Zone. It is sited at a `waist' between two east-striking zones of ground cracks; the spacing between the crack zones decreases towards Devil's Throat. East-striking fractures are also prominent in the pit crater walls. Pit craters along the Southwest Rift Zone typically are elongate in plan view along the direction of the rift, have large caves at their bases along the long axes of the craters, and are smaller than those of the East Rift Zone. Some closely spaced pits there have coalesced to form a trough. Based on our observations and mechanical considerations, we infer that pit craters form by stoping over an underlying large-aperture rift zone fracture, and not by piston-like collapse over broad magma bodies or voids. Flow of magma along the underlying fracture may remove stoped blocks and prevent the fracture from being choked with debris. This mechanism is consistent with pit crater location, ground crack patterns, the preferred orientation of fractures in pit crater walls, and pit crater geometry (both in map view and cross-section). The mechanism also fits with observations of stoping into a gaping rift fracture that conducted lava from Kilauea caldera during the 1920s. Additionally, the ratio of pit crater width to depth of 0.5 to 2 is consistent with pit craters forming over a nearly vertical opening mode fracture. 相似文献
19.
Residual meteoritic material has been detected on the surface of crater interiors on lunar samples 60315,29 and 65315,68. Iron-nickel micrometeoroid residues are present in the form of mettallic spherules embedded in or attached to the crater glass-linings; stony-iron meteorite residual material is homogeneously mixed with the glass-linings.Crater simulation experiments show the dependence of crater diameter to depth ratio on projectile density. On the other hand, the projectile velocities exceeding 4 km/s have no measurable influence on the D/T ratios of microcraters. As a result, diameter-to-depth measurements on lunar microcraters yield three groups of micrometeorites in the size range between 1 μm and 1 mm: iron-nickel, stony-iron and low-density particles. The measured D/T values correspond directly to the kind of determined projectile residues: craters showing residues of iron-nickel meteorites have ratios of D/T = 1.3–1.4 and craters with stony-iron residues have ratios ofD/T = 1.9–2.1.Craters with diameters ?30 μm seem to have been formed predominantly by iron-nickel micrometeorites, whereas craters with diameters ?80 μm predominantly by stony meteorites. 相似文献