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A review of the scenarios for the Cretaceous/Tertiary (K/T) boundary event is presented and a coherent hypothesis for the
origin of the event is formulated. Many scientists now accept that the event was caused by a meteorite impact at Chicxulub
in the Yucatan Peninsula, Mexico. Our investigations show that the oceans were already stressed by the end of the Late Cretaceous
as a result of the long-term drop in atmospheric CO2, the long-term drop in sea level and the frequent development of oceanic anoxia. Extinction of some marine species was already
occurring several million years prior to the K/T boundary. The biota were therefore susceptible to change. The eruption of
the Deccan Traps, which began at 66.2 Ma, coincides with the K/T boundary events. It erupted huge quantities of H2SO4, HCl, CO2, dust and soot into the atmosphere and led to a significant drop in sea level and marked changes in ocean temperature. The
result was a major reduction in oceanic productivity and the creation of an almost dead ocean. The volcanism lasted almost
0.7 m.y.. Extinction of biological species was graded and appeared to correlate with the main eruptive events. Elements such
as Ir were incorporated into the volcanic ash, possibly on soot particles. This horizon accumulated under anoxic conditions
in local depressions and became the marker horizon for the K/T boundary. An oxidation front penetrated this horizon leading
to the redistribution of elements. The eruption of the Deccan Traps is the largest volcanic event since the Permian-Triassic
event at 245 Ma. It followed a period of 36 m.y. in which the earth’s magnetic field failed to reverse. Instabilities in the
mantle are thought to be responsible for this eruption and therefore for the K/T event. We therefore believe that the K/T
event can be explained in terms of the effects of the Deccan volcanism on an already stressed biosphere. The meteorite impact
at Chicxulub took place after the onset of Deccan volcanism. It probably played a regional, rather than a global, role in
the K/T extinctions. 相似文献
3.
SONG Tianrui ZHENG Ning LIU Yongqing KUANG Hongwei PENG Nan LI Chao TANG Jigang YAN Qinggao GAO Linzhi ZHU Zhicai XIA Xiaoxu WANG Yuchong 《《地质学报》英文版》2020,94(1):38-56
This study covers cosmic spherules derived from the Mesoproterozoic Dahongyu Formation in the Ming Tombs area, Beijing. The cosmic spherules include iron oxide cosmic spherules, carbonaceous chondrites, and atomic iron “steely bead”-shaped cosmic spherules. The mineral assemblage of silicon carbide, forsterite, zircon, and glass spherules and fragments were picked from melt-silicified carbonate of the Mesoproterozoic Dahongyu Formation (ca. 1625 Ma). Cosmic spherule assemblages are solely discovered from sedimentary rocks in China. Platinum group elements (PGE) were determined for the first time in cosmic spherules and associated minerals. PGE comparative observation between meteorite and cosmic spherules is presented in this study. It is recognized that an extraterrestrial meteorite impact event might have occurred in the Dahongyu Stage. The main evidence is a large number of iron cosmic spherules in silicified oncolitic limestone, and associated cosmic silicon carbide, glass spherules, and fragments, as well as the presence of forsterite. The impact-volcanic crater is characteristic of a big black shale block dropped into the bended silicified limestone. 相似文献
4.
G. Keller 《Australian Journal of Earth Sciences》2013,60(4-5):725-757
Large impacts are credited with the most devastating mass extinctions in Earth's history and the Cretaceous?–?Tertiary (K/T) boundary impact is the strongest and sole direct support for this view. A review of the five largest Phanerozoic mass extinctions provides no support that impacts with craters up to 180 km in diameter caused significant species extinctions. This includes the 170 km-diameter Chicxulub impact crater regarded as 0.3 million years older than the K/T mass extinction. A second, larger impact event may have been the ultimate cause of this mass extinction, as suggested by a global iridium anomaly at the K/T boundary, but no crater has been found to date. The current crater database suggests that multiple impacts, for example comet showers, were the norm, rather than the exception, during the Late Eocene, K/T transition, latest Triassic and the Devonian?–?Carboniferous transition, but did not cause significant species extinctions. Whether multiple impacts substantially contributed to greenhouse warming and associated environmental stresses is yet to be demonstrated. From the current database, it must be concluded that no known Phanerozoic impacts, including the Chicxulub impact (but excluding the K/T impact) caused mass extinctions or even significant species extinctions. The K/T mass extinction may have been caused by the coincidence of a very large impact (>?250 km) upon a highly stressed biotic environment as a result of volcanism. The consistent association of large magmatic provinces (large igneous provinces and continental flood-basalt provinces) with all but one (end-Ordovician) of the five major Phanerozoic mass extinctions suggests that volcanism played a major role. Faunal and geochemical evidence from the end-Permian, end-Devonian, end-Cretaceous and Triassic/Jurassic transition suggests that the biotic stress was due to a lethal combination of tectonically induced hydrothermal and volcanic processes, leading to eutrophication in the oceans, global warming, sea-level transgression and ocean anoxia. It must be concluded that major magmatic events and their long-term environmental consequences are major contributors, though not the sole causes of mass extinctions. Sudden mass extinctions, such as at the K/T boundary, may require the coincidence of major volcanism and a very large Impact. 相似文献
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《Chemie der Erde / Geochemistry》2017,77(1):207-224
On April 23rd 2013 at 2:07 a.m., a 1.3 kg meteorite fell in the Braunschweig suburb Melverode (52° 13′ 32.19″ N. 10° 31′ 11.60″ E). Its estimated velocity was 250 km/h and it formed an impact pit in the concrete fall site with a diameter of 7 cm and a depth of 3 cm. Radial dust striae are present around the impact pit. As a result of the impact, the meteorite disintegrated into several hundred fragments with masses up to 214 g. The meteorite is a typical L6 chondrite, moderately shocked (S4) – but with a remarkably high porosity (up to 20 vol%). The meteorite was ejected from its parent body as an object with a radius of about 10–15 cm (15–50 kg). The U,Th-He gas retention age of ∼550 Ma overlaps with the main impact event on the L-chondrite parent body ∼470 Ma ago that is recorded by many shocked L chondrites. The preferred cosmic-ray exposure age derived from production of radionuclides and noble gas isotopes is (6.0 ± 1.3) Ma. 相似文献
6.
Two sections subsequently sawed from meteorite fragment Kaidun #d(4–5)C were examined under an optical and scanning electron
microscope. The major minerals of the fragment are pigeonite and anorthite; the accessory minerals are spinels and occasional
grains of ilmenite, Ca phosphate, and Fe sulfide. The compositions of the minerals broadly vary. The texture of the fragment,
its mineralogy, and mineral chemistries definitely indicate that the fragment originated from a crystalline rock affected
by partial melting during an impact event. The chemical compositions of both minerals (the concentration of the anorthite
end member of plagioclase An99 and the Fe/Mn atomic ratio of 44 in the pyroxenes) differ from those in other known meteorite samples and suggest that fragment
d(4–5)C of the Kaidun meteorite represents a new differentiated parent body that has never been sampled before. 相似文献
7.
P. W. Haines 《Australian Journal of Earth Sciences》2013,60(4-5):481-507
The Australian continent has one of the best-preserved impact-cratering records on Earth, closely rivalling that of North America and parts of northern Europe, and the rate of new discoveries remains high. In this review 26 impact sites are described, including five small meteorite craters or crater fields associated with actual meteorite fragments (Boxhole, Dalgaranga, Henbury, Veevers, Wolfe Creek) and 21 variably eroded or buried impact structures (Acraman, Amelia Creek, Connolly Basin, Foelsche, Glikson, Goat Paddock, Gosses Bluff, Goyder, Kelly West, Lawn Hill, Liverpool, Matt Wilson, Mt Toondina, Piccaninny, Shoemaker, Spider, Strangways, Tookoonooka, Woodleigh, Yallalie, Yarrabubba). In addition a number of possible impact structures have been proposed and a short list of 22 is detailed herein. The Australian cratering record is anomalously biased towards old structures, and includes the Earth's best record of Proterozoic impact sites. This is likely to be a direct result of aspects of the continent's unique geological evolution. The Australian impact record also includes distal ejecta in the form of two tektite strewn fields (Australasian strewn field, ‘high-soda’ tektites), a single report of 12.1?–?4.6 Ma microtektites, ejecta from the ca 580 Ma Acraman impact structure, and a number of Archaean to Early Palaeoproterozoic impact spherule layers. Possible impact related layers near the Eocene?–?Oligocene and the Permian?–?Triassic boundaries have been described in the literature, but remain unconfirmed. The global K?–?T boundary impact horizon has not been recognised onshore in Australia but is present in nearby deep-sea cores. 相似文献
8.
本文综述了全球陨石坑研究的研究历史和最新成果、基本的概念、陨石坑的识别要点、世界著名的陨石坑、陨石撞击地球可能引起的岩浆活动、陨石撞击与生命演化等内容。确定一个陨石坑,要从有一定弧度的地貌开始,鉴别低平圆形地质体是陨石还是其它原因造成的,综合确定岩石的岩石学特征、岩石中是否有撞击变质矿物、残余陨石、重力异常。陨石撞击太阳系的所有行星。由于地球表面遭受严重的风化和侵蚀,地质学家很难发现陨石坑。截至2021年3月31日,全球陨石坑数据库中有190个经确认的陨石坑,但中国只有一个,中国地质学家在发现陨石坑方面应当积极努力。对一个陨石坑认识可能不很成熟,但往往能改变对一个地区的地质成因理论的认识,形成完整的陨石坑证据链可能需要几代科学家的不断努力。 相似文献
9.
本文综述了全球陨石坑研究的研究历史和最新成果、基本的概念、陨石坑的识别要点、世界著名的陨石坑、陨石撞击地球可能引起的岩浆活动、陨石撞击与生命演化等内容。确定一个陨石坑,要从有一定弧度的地貌开始,鉴别低平圆形地质体是陨石还是其他原因造成的,综合确定岩石的岩石学特征、岩石中是否有撞击变质矿物、残余陨石、重力异常。陨石撞击太阳系的所有行星。由于地球表面遭受严重的风化和侵蚀,地质学家很难发现陨石坑。截至2021年3月31日,全球陨石坑数据库中有190个经确认的陨石坑,但中国只有一个,中国地质学家在发现陨石坑方面应当积极努力。对一个陨石坑认识可能不很成熟,但往往能改变对一个地区的地质成因理论的认识,形成完整的陨石坑证据链可能需要几代科学家的不断努力。 相似文献
10.
撞击角砾岩是陨石撞击过程形成的特有岩石种类,是研究撞击成坑过程、陨石坑定年、矿物岩石冲击变质的理想对象。岫岩陨石坑是一个直径1800m的简单陨石坑,坑内有大量松散堆积的撞击角砾岩。本研究通过光学显微镜、费氏台、电子探针、X射线荧光光谱仪、电感耦合等离子质谱仪等分析测试手段,主要研究了岫岩陨石坑撞击角砾岩的岩相学和冲击变质特征,并在此基础上讨论了撞击角砾岩的形成过程和陨石坑的形貌特征。岫岩陨石坑内产出有三种撞击角砾岩,分别是来自上部的玄武质角砾岩和复成分岩屑角砾岩,以及底部的含熔体角砾岩。组成玄武质角砾岩和复成分岩屑角砾岩的碎屑受到的冲击程度较低,仅有少量石英发育面状变形页理,指示不超过20GPa的冲击压力。而组成含熔体角砾岩的碎屑受到了很强的冲击,发育了熔融硅酸盐玻璃、石英面状变形页理、柯石英、二氧化硅玻璃、击变长石玻璃、莱氏石等冲击变质特征,指示的峰值压力超过50GPa。本研究证实了含熔体角砾岩通常产出在简单陨石坑底部,由瞬间坑的坑缘和坑壁垮塌的岩石碎屑与坑底的冲击熔体混合形成。岫岩坑的真实深度是495m,真实深度与直径的比值为0.275,符合简单陨石坑的尺寸特征。陨石坑内的撞击角砾岩中心厚度为188m,与直径之比为0.104,略低于其它简单坑,可能是受丘陵地貌影响导致改造阶段垮塌到坑内的岩石角砾偏少。 相似文献
11.
M. A. Nazarov S. I. Demidova M. O. Anosova Yu. A. Kostitsyn Th. Ntaflos F. Brandstaetter 《Petrology》2012,20(6):506-519
The Dhofar 280 lunar highland meteorite is the first one in which native silicon was identified in association with iron silicides. This association is surrounded by silicate material enriched in Si, Na, K, and S and occurs within an impact-melt matrix. Compared to the meteorite matrix, the objects with native Si and the silicate material around them show high Al-normalized concentrations of volatile elements and/or elements with low sensitivity to oxygen but are not any significantly enriched in refractory lithophile elements. Some lithophile elements (V, U, Sm, Eu, and Yb) seem to be contained in reduced forms, and this predetermines REE proportions atypical of lunar rocks and a very low Th/U ratio. The admixture of siderophile elements (Ni, Co, Ge, and Sb) suggests that the Si-bearing objects were contaminated with meteorite material and were produced by the impact reworking of lunar rocks. The high concentrations of volatile elements suggest that the genesis of these objects could be related to the condensation of silicate vapor generated during meteorite impacts. The reduction of silicon and other elements could take place in an impact vapor cloud, with the subsequent condensation of these elements together with volatile components. On the other hand, condensates of silicate vapor could be reduced by impact reworking of impact breccias. Impact-induced vaporization and condensation seem not to play any significant role in forming the composition of the lunar crust, but the contents of the products of such processes can be locally relatively high. The greatest amounts of silicate vapor were generated during significant impact events. For example, more than 70% of the total mass of lunar material evaporated in the course of impact events should have resulted from the collision of the Moon with a cosmic body that produced the Moon??s largest South Pole-Aitken basin. 相似文献
12.
As previously found for a chondritic inclusion of unknown affinity, mineralogic and petrologic properties of 9 inclusions in the Cumberland Falls enstatitc achondrite are primitive members of the forsterite (F) chondrite group, hitherto defined by 4 meteorites of similar redox state. The inclusions define a primitive suite with properties indicating 8 as F3 and one of even lower petrologic type. The abundant minerals include: low-Ca pyroxene, olivine, plagioclase, kamacite, taenite, schreibersite, troilite, ferroan alabandite and daubreelite. Diopside, oldhamite and a Ti-rich sulfide are present in one or two inclusions. Petrologic textures and jadeitic pyroxene, hitherto unidentified in meteorites, indicate substantial degree of shock. The inclusions acquired their chemical characteristics during nebular condensation and accretion over a broad redox range (metal-silicate trends in them verify Prior's Rules): their parent body later impacted the enstatite meteorite parent body. During impact, the inclusions were shocked and incorporated with enstatite achondrite host as a breccia that would become Cumberland Falls. 相似文献
13.
常规的K-Ar法是基于40K通过K-层电子捕获衰变成40Ar*这一机理,应用衰变定律而定年的。它具有测定对象广、测定年龄范围大等优点,是同位素地质定年的主要方法之一。但是,由于40Ar*是气体,当岩石、矿物形成以后受到搅动时(如岩浆的侵入、构造活动、宇宙物质的冲击等),40Ar*容易丢失,使年龄值偏低。1962年由Sigurgeirsson提出的,后经Merrihue、Turner等人逐步完善的40Ar-39Ar快中子活化定年技术,很好地克服了K-Ar法的局限性。40Ar-39Ar定年分为两种:一是全熔融法(total fusion),样品被快中子照射后一次加热熔融,然后计算年龄,此值与常规K-Ar法结果相当;另一种是阶段加热法(step-heating),被照射的样品从低温到高温被逐步加热,分别计算各温度阶段的40Ar/39Ar视年龄,并进而得到一条年龄谱和一个坪年龄(plateau age)。后一种方法对研究地质体是否受过热的挠动、岩石矿物的早期结晶年代、后期热挠动次数、热挠动年代、岩石矿物对氢的保存性、过剩氩的存在状态等具有独特作用,它开辟了同位素地质年代学的一个新领域。本文将着重介绍应用40Ar-39Ar阶段加热技术研究地球物质及陨石受热历史的某些成果。 相似文献
14.
Paul C. Buchanan Takaaki Noguchi Donald D. Bogard Ikuo Katayama 《Geochimica et cosmochimica acta》2005,69(7):1883-1898
The unequilibrated eucrite Yamato 82202 (Y82202) contains a network of relatively thick (up to 1 mm in width) glass veins. The host of the meteorite represents a monomict breccia composed of volcanic rock that crystallized > 4.3 Ga ago as a lava flow on the surface of 4 Vesta. The veins formed 3.90 ± 0.04 Ga ago, probably as a result of frictional melting associated with impact, under conditions of low effective oxygen fugacity and higher sulfur fugacity. The glass contains disordered structural elements characteristic of pyroxene and feldspar, reminiscent of the eucritic target lithology. The unequilibrated pyroxenes of the volcanic host and the pristine character of the glass indicate that this meteoritic material did not experience significant thermal metamorphism after initial crystallization of the lava. Hence, it was not affected by regional metamorphism caused by burial to a significant depth or by long-term contact metamorphism associated with a thick lava flow, large intrusion, or hot layer of impact ejecta. The meteorite resided at a shallow depth (though not at the surface) on 4 Vesta or on one of the vestoids until it was ejected and traveled to Earth, probably with other HED materials that have 36Ar exposure ages of ∼13 Ma. These data suggest that the surface of the asteroid 4 Vesta has significant, though probably small, proportions of glass, as well as unequilibrated volcanic rock. 相似文献
15.
M. S. Sisodia U. K. Singh G. Lashkari P. N. Shukla A. D. Shukla N. Bhandari 《Journal of Earth System Science》2005,114(2):111-124
We report the presence of a 3–5 cm thick loose fragmental layer in the Siliceous Earth at Matti ka Gol in the Barmer basin
of Rajasthan. Petrographic, chemical and mineralogical study reveals the presence of abundant volcanic debris such as glass
shards, agglutinates, hollow spheroids, kinked biotites, feldspars showing oscillatory zoning, olivines, ilmenite and native
iron. The presence of similar particles in the whole section suggests that the Siliceous Earth is a volcanic ash. Stratigraphic
correlation, palynological and microvertebrate data suggest that the Siliceous Earth may have deposited over a short span
of time during the Upper Cretaceous to Lower Palaeocene. In view of the possibility that this section may contain K/T impact
debris, we looked for grains having impact signatures. Some patches of the Siliceous Earth of Bariyara show the presence of
Ni-rich (> 0.5%) vesicular glasses, sanidine spherules, magnesioferrite crystals, soot, etc., but because of their low abundance,
it is not possible to establish if they are volcanic, micrometeorite ablation products or a part of the K/T impact ejecta. 相似文献
16.
W. Stinnesbeck G. Keller T. Adatte D. Stüben U. Kramar Z. Berner C. Desremeaux E. Molière 《地学学报》1999,11(6):303-310
Examination of new expanded K/T boundary sections near Beloc, Haiti, reveals deposition of a glass spherule-rich deposit (SRD) and two (PGE) anomalies (one Ir-dominated and one Pd-dominated) during the early Danian Parvularugoglobigerina eugubina Zone [Pla(l)]. The presence of the Haiti SRD within the early Danian is interpreted as being due to reworking. Ir is only slightly elevated within the SRD but forms an anomaly at the top of the SRD extending into the overlying pelagic limestones. It is unclear at present whether this Ir anomaly results from mechanical reworking of an impact at the K/T boundary, or an additional impact event in the early Danian. The second PGE anomaly upsection is dominated by Pd and Pt and is more compatible with a magmatic origin. This suggests a multi-event scenario consistent with one (and possibly two) impact(s), followed by a PGE-enriched volcanic event in the Caribbean. 相似文献
17.
Layers with high magnetic susceptibility contain heavy minerals that are the most likely to preserve signatures of impact in metamorphosed Precambrian rocks. The following impact indicators are resistant to alteration and metamorphism and are likely to be found in heavy mineral layers: impact diamond, SiC, shocked zircon, high-pressure TiO2 phases, reidite, and high-pressure chromite. Coesite and stishovite could also be present but are not likely to be preserved in rocks metamorphosed above the greenschist facies. Looking for layers with high magnetic susceptibility will also identify layers that might contain concentrations of zircon for dating. 相似文献
18.
The K?rka borate deposit was deposited in a Miocene lacustrine basin which is closely associated with volcanic activity which lasted from Paleogene to the beginning of Quaternary. Borate mineralization alternates with claystone, mudstone, tuff and fine-layered limestone and mostly shows a lenticular structure. The mineral paragenesis is composed of borax, tincalconite, ulexite, kurnakovite, probertite, tunellite, colemanite, dolomite, smectite group minerals, illite and some firstly reported minerals for the K?rka deposit including hydrochloroborite, brianroulstonite, hilgardite-4M and searlesite minerals. In comparison to average values of earth crust, concentrations of Cs, Sr, Li, As and Se were significantly enriched with respective rates of 21, 15, 14, 3 and 188 folds. Regarding KY, KS1 and KS2 locations, there are differences in both element abundances and their geochemical tendencies which are attributed to variations in discharge regime and physico-chemical conditions of the depositional environment. Independent behaviour of B2O3 might indicate that boron is not associated with clays and carbonates and, therefore, most part of boron must be derived from volcanic activity (hydrothermal solutions, gases). REE data indicate that the K?rka borate deposit was formed in a sedimentary environment where highly alkaline (high pH) hydrothermal solutions also took part in borate precipitation process. 相似文献
19.