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1.
D. M. Pechersky D. M. Kuzina G. P. Markov V. A. Tsel’movich 《Izvestiya Physics of the Solid Earth》2017,53(5):658-676
Thermomagnetic and microprobe studies of native iron in the terrestrial upper-mantle hyperbasites (xenoliths in basalts), Siberian traps, and oceanic basalts are carried out. The results are compared to the previous data on native iron in sediments and meteorites. It is established that in terms of the composition and grain size and shape, the particles of native iron in the terrestrial rocks are close to each other and to the extraterrestrial iron particles from sediments and meteorites. This suggests that the sources of the origin of these particles were similar; i.e., the formation conditions in the Earth were close to the conditions in the meteorites’ parent bodies. This similarity is likely to be due to the homogeneity of the gas and dust cloud at the early stage of the solar system. The predominance of pure native iron in the sediments can probably be accounted for by the fact that interstellar dust is mostly contributed by the upper-mantle material of the planets, whereas the lower-mantle and core material falls on the Earth mainly in the form of meteorites. A model describing the structure of the planets in the solar system from the standpoint of the distribution of native iron and FeNi alloys is proposed. 相似文献
2.
The paper summarizes the results of thermomagnetic analysis concerning the distribution of metallic iron in the sediments
ranging in age from Miocene to Early Cretaceous sampled from the following sections: Gams (Austria); Verkhorech’e and Sel’bukhra
(the Crimea); Kvirinaki and Tetritskaro (Georgia); Aimaki, Dzhengutai, Madzhalis, and Gergebil (Ciscaucasia, Russia); Klyuchi
and Teplovka (Volga region, Russia); Koshak (Kazakhstan); and Khalats and Kara-Kala (Turkmenia). Small amounts of native iron
(from 10−5% to 0.05%) are identified in 521 samples of 921 studied; i.e., iron particles are almost pervasive. This fact traces the
origin of these particles to cosmic dust. Some established features point to the heterogeneous character of the cosmic dust:
(a) the samples clearly fall into two groups. One group comprises the rocks that contain iron particles; the rocks of the
other group are iron-free. In the first group, four intervals are distinguished where the sediments are globally enriched with iron with constant nickel content (5–6%); (b) in terms of composition, the iron particles are divided into
three groups. The first group contains pure iron; the particles pertaining to the second group contain iron with a minor amount
of nickel typical for kamacite; and the third group comprises the particles of Fe-Ni alloy with more than 20% nickel. The
first and the second groups are ubiquitous; the particles of the third group are spread locally. They bear no relation to
cosmic dust and are probably associated with the meteoritic impacts. 相似文献
3.
D. M. Pechersky D. K. Nurgaliev V. A. Fomin Z. V. Sharonova D. M. Gil’manova 《Izvestiya Physics of the Solid Earth》2011,47(5):379-401
The composition and distribution of particles of native iron in eight sections of the Cretaceous-Danian sediments in the Caucasus,
Crimea and Kopet Dagh were studied using thermomagnetic analysis up to 800°C. Iron particles are found in 330 of 571 tested
samples, their percentage varies from 10−5 to 0.05%, and their distribution is bimodal. It was established that the Santonian sediments of the Caucasus and Kara-Kala
are enriched with the iron particles; the upper boundary of these sediments is marked by a sharp drop in the iron content
at approximately 84 Ma, which coincides with the upper boundary of the Dzhalal hyperchron. The variations in the Curie point
of iron from 680°C up to 780°C reflect the fluctuations of the nickel admixture. A peak of the elevated iron content with
nearly constant nickel of 5% was found in all studied sections, i.e., this is a global effect. The global pattern of the distribution
and composition of the iron particles clearly indicates that their origin is associated with cosmic dust. At the same time,
the particles of Ni-Fe alloy and pure nickel are very rare, and their concentration does not correlate with the content of
iron particles. Apparently, there are very few Ni-Fe and pure nickel particles in cosmic dust, and, most likely, the particles
of Ni-Fe alloy are mainly due to impact events. 相似文献
4.
M.B. Blanchard D.E. Brownlee T.E. Bunch P.W. Hodge F.T. Kyte 《Earth and Planetary Science Letters》1980,46(2):178-190
We present analyses of spheres magnetically extracted from mid-Pacific abyssal clays 0–500,000 years old. The concentration of spheres >200 μm is a few times 10 ppb. The spheres were divided into three groups using their dominant mineralogy, and are named iron, glassy, and silicate. Most spheres were formed from particles that completely melted as they separated from their parent meteoroids during the ablation process. However, some of the silicate spheres contain relict grains of the parent meteoroids that did not experience any melting. Typically, these relict grains are olivine crystals whose cores are Mg-rich (Fo89–99). Commonly the outer rims of these grains were altered during heating. Other relict mineral grains include enstatite, ferrous spinel, chromite, and pentlandite.The three groups of spheres may possibly indicate some genetic significance. It seems reasonable to expect iron-rich spheres to be produced during ablation of iron and metal-rich silicate meteoroids. Metal spheres are probably not produced by ablation of predominantly silicate meteoroids because studies of fusion crusts and laboratory ablated silicate materials have never yielded separate metal spheres, but rather have produced spheres with intergrown iron oxide and silicate phases. The iron spheres possess identical mineralogy with the fusion crusts of Boguslavka, Norfork, and N'Kandhla iron meteorites as well as with the ablation debris created in the laboratory using iron and nickel-iron samples.The glassy spheres are considerably more Fe-rich than the silicate spheres. They consist of magnetite and a Fe-rich glass which is relatively low in Si. Some of these spheres may have experienced pronounced volatile depletion during the ablation process and could have been derived from silicate or metal-rich silicate meteoroids.The silicate spheres are undoubtedly derived from ablation of stony meteoroids. Two of the mineral assemblages occurring in these spheres (olivine-magnetite-glass and sulfide) are identical to those described in the natural fusion crusts of Allende, Orgueil, and Murchison meteorites, laboratory-made ablation debris, and melted interplanetary dust collected from the stratosphere. Bulk compositions and relict grains are useful for determining the parent meteoroid types for the silicate spheres. Bulk analyses of spheres have non-volatile elemental abundances similar to chondritic abundances. Analyses of relict grains identified high-temperature minerals which often occur as larger crystals in a fine-grained matrix that is characterized by voids. These voids were caused by escaping volatiles as minerals decomposed during ablation. Because larger crystals of higher-temperature minerals are associated with fine-grained, low-temperature, volatile-rich matrix, the obvious candidates for parent meteoroids of the silicate spheres containing relict grains are carbonaceous chondrites. 相似文献
5.
Our rock magnetic analysis of core Ph05 from the West Philippine Sea demonstrates that the core preserves a strong, stable
remanent magnetization and meets the magnetic mineral criteria for relative paleointensity (RPI) analyses. The magnetic minerals
in the sequence are dominated by pseudosingle-domain magnetite, and the concentration of magnetic minerals is at the same
scale. Both the conventional normalizing method and the pseudo-Thellier method were used in conjunction with the examination
of the rock magnetic properties and natural remanent magnetization. Susceptibility (χ), anhysteretic remnant magnetization (ARM) and saturation isothermal remnant magnetization (SIRM) were used as the natural
remanent magnetization normalizer. However, coherence analysis indicated that only ARM is more suitable for paleointensity
reconstruction. The age model of core is established based on oxygen isotope data and AMS14C data, which is consistent with the age model estimated from RPI records. The relative paleointensity data provide a continuous
record of the intensity variation during the last 200 ka, which correlates well with the global references RPI stacks. Several
prominent low paleointensity values are identified and are correlated to the main RPI minima in the SINT-200 record, suggesting
that the sediments have recorded the real changes of geomagnetic field.
Supported by National Natural Science Foundation of China (Grant No. 90411014) and Pilot Project of the Knowledge Innovation
Program of Chinese Academy of Sciences (No. KZCX2-YW-211) 相似文献
6.
A. F. Grachev D. M. Pechersky S. E. Borisovskii V. A. Tselmovich 《Izvestiya Physics of the Solid Earth》2008,44(10):789-803
The paper presents results of detailed magnetomineralogical and microprobe studies of sediments at the Cretaceous/Paleogene (K/T) boundary in two epicontinental sections in the Eastern Alps (Austria), where deposits, including the K/T boundary, outcrop along the Gams River and its tributaries. K/T boundary layers in these sections are similar in the set of such magnetic minerals as iron hydroxides, ferrospinels, hemoilmenite, titanomagnetite, magnetite, hematite, and metallic iron. However, the boundary layer in the Gams-1 section is distinguished by the presence of metallic nickel and its alloy with iron and by the absence of iron sulfides, whereas nickel has not been discovered in the Gams-2 section, which, however, contains iron sulfides of the pyrite type. Therefore, these minerals occur locally. It is suggested that enrichment in iron hydroxides of a common origin can be regarded as a global phenomenon inherent in the K/T boundary and unrelated to an impact event. 相似文献
7.
D. M. Pechersky 《Izvestiya Physics of the Solid Earth》2008,44(3):232-238
Results of petromagnetic studies of epicontinental sediments at the Mesozoic-Cenozoic (K/T) boundary are generalized. Their analysis shows that an abrupt rise in the concentration of iron hydroxides is confined to this boundary. Their concentration is highest at the base of the boundary layer and drops by more than two times at it top. As distinct from iron hydroxides, other magnetic minerals were variously accumulated, depending on their origin and local deposition conditions of terrigenous material (for example, accumulation of particles of metallic iron and nickel, aerial transport of titanomagnetite grains of volcanic origin, and deposition of terrigenous particles of magnetite and ilmenite). 相似文献
8.
Etch rates and etchable lengths of cosmic ray tracks in meteoritic crystals have been used by several workers to derive the charge spectrum of ancient cosmic rays. This is done by comparing the fossil cosmic ray track record with fresh accelerator-produced calibration tracks. These calibration tracks are generally produced at room temperature, while meteorites spend a high proportion of their lifetimes orbiting at large distances from the Sun ( 3–5 AU) and are, consequently, at much lower temperatures (typically 100–150 K) during most of their cosmic ray exposure ages. We have irradiated crystals of apatite, olivine, enstatite and diopside held at 77, 293, 473 and 573 K, with 2 MeV/nucleon81Br ions, and then etched them. We find that their track etching properties are dependent upon the temperature of the mineral during registration. The track etch velocity generally increases with registration temperature up to 300 or 500 K (the upper limit depending upon the type of crystal). Our results also indicate that the annealing sensitivity of fission tracks in fluorapatite may be influenced by the registration temperature. This temperature dependence has important implications not only for cosmic ray particle identification but also for fission track dating of meteorites in view of the fact that the meteorite parent bodies were at elevated temperatures at the beginning af their life when244Pu fission tracks were being generated abundantly. 相似文献
9.
Cooling rates of eight group IVA iron meteorites were determined using a modification of the Wood method where cooling rate curves are calculated as a function of central taenite Ni content and taenite half-width. The major modification of the Wood method was to include the effect of P on the Ni solubility limits and Ni diffusion coefficients in the kamacite phase for each meteorite studied. The Borg and Lai binary kamacite Ni diffusivities were judged to be the best quality data available for the calculations. The calculated cooling rates range between 3 and 65°C/Myr. A correlation between decreasing cooling rate and increasing Ni content within the group IVA irons is observed. This cooling rate variation agrees closely with the 6–70°C/Myr range calculated by the independent bulk Ni-kamacite bandwidth method. Such a large variation in cooling rate within the group IVA argues against formation within the core of a single parent body.Willis and Wasson in the preceding paper found only a factor of 2 variation in cooling rate for the six IVA irons studied. The differences between the results of Willis and Wasson and this study are due mainly to the choice of the Ni diffusion coefficients in α and to the choice of the expressions for the effect of P on both the diffusion coefficients and the Ni solubility in kamacite. The Hirano et al. diffusivities used by Willis and Wasson were judged to be incorrect particularly because they are significantly higher than diffusivities in kamacite and taenite measured by other investigators. The assumption of Willis and Wasson that the same P content (0.03 wt.%) can be used for the low-Ni IVA's and that the same P content (0.16 wt.%) can be used for the high-Ni IVA's was judged to be a serious oversimplification. 相似文献
10.
西安市道路表面灰尘样品的环境磁学研究显示磁化率(χ)、非磁滞磁化率（χARM）以及饱和等温剩磁（SIRM）均比较高,表明样品中磁性矿物含量较高.其中磁化率（χ）主要受人类活动强度影响,而非磁滞磁化率（χARM）及饱和等温剩磁（SIRM）则由人为活动强度和磁性矿物种类共同决定.κ-T曲线以及等温剩磁（IRM）获得曲线显示样品中磁铁矿和磁赤铁矿等亚铁磁性矿物占主导,并可能含有少量的单质铁,其相对含量与人类活动种类有关：与单纯的交通排放及冶金活动相比,密集的人群流动可带来更多的单质铁矿物.磁畴图谱显示磁性矿物粒径变化不大,以准单畴及多畴颗粒等粗颗粒为主,明显大于成土作用形成的磁性颗粒.综合磁性矿物含量种类以及粒径可辨别污染及污染来源,提供污染监测的磁学手段,并初步进行污染来源划分. 相似文献
11.
Magnetic properties of a freshly fallen LL ordinary chondrite: the Bensour meteorite 总被引：1，自引：0，他引：1
Jrme Gattacceca Pierre Rochette Michle Bourot-Denise 《Physics of the Earth and Planetary Interiors》2003,140(4):343-358
A comprehensive rock magnetic, magnetic anisotropy and paleomagnetic study has been undertaken in the brecciated LL6 Bensour ordinary chondrite, a few months only after its fall on Earth. Microscopic observations and electronic microprobe analyses indicate the presence of Ni-rich taenite, tetrataenite and rare Co-rich kamacite. Tetrataenite is the main carrier of remanence. Magnetization and anisotropy measurements were performed on mutually oriented 125 mm3 sub-samples. A very strong coherent susceptibility and remanence anisotropy is evidenced and interpreted as due to the large impact responsible for the post-metamorphic compaction of this brecciated material and disruption of the parent body. We show that the acquisition of remanent magnetization postdates metamorphism on the parent body and predates the entering of the meteorite in Earth’s atmosphere. Three components of magnetization could be isolated. A soft coherent component is closely related to the anisotropy of the meteorite and is interpreted as a shock remanent magnetization acquired during the same large impact on the parent body. Two harder components show random directions at a few mm scale. This randomness is attributed either to the formation mechanism of tetrataenite or to post-metamorphic brecciation. All components are likely acquired in very low (≈μT) to null ambient magnetic field, as demonstrated by comparison with demagnetization behavior of isothermal remanent magnetization. Two other LL6 meteorites, Kilabo and St-Mesmin, have also been studied for comparison with Bensour. 相似文献
12.
《Earth and Planetary Science Letters》2006,241(3-4):530-542
New, high-precision W isotope data on iron meteorites are presented that provide important constraints on the timing of silicate–metal segregation in planetesimals. Magmatic iron meteorites all have ε182W within error or less radiogenic than initial ε182W estimated by studies of chondritic meteorites. At face value this implies that iron meteorites are as old and older than refractory calcium–aluminium rich inclusions (CAI), which are widely thought to be the oldest solar system objects. Moreover, different meteorites from the same magmatic groups, believed to be derived from the same planetissimal core, display a range of ε182W. We suggest that the paradoxical ε182W values more negative than initial Solar System Initial (SSI) are most readily explained as a result of secondary, spallation reactions with cosmic rays during transit between parent body and the earth. This is supported by the most negative ε182W being found in meteorites with the oldest exposure ages and the magnitude of the effect is shown to be consistent with known nuclear reactions. On the other hand, it is also striking that none of the magmatic iron group meteorites have ε182W analyses, outside error, more radiogenic than the estimated solar system initial ratio. This suggests that core formation in parent bodies of magmatic iron meteorites occurred ≤ 1.5 Myr after the formation age of CAI [Y. Amelin, A.N. Krot, I.D. Hutcheon, and A.A. Ulyanov, Lead isotopic ages of chondrules and calcium-aluminum inclusions, Science 297, 1678–1683, 2002]. This extremely early metal–silicate differentiation is coeval with the first chondrules [M. Bizzarro, J.A. Baker, and H. Haack, Mg isotope evidence for contemporaneous formation of chondrules and refractory inclusions, Nature 431, 275–278, 2004, A.N. Krot, Y. Amelin, P. Cassen, and A. Meibom, Young chondrules in CB chondrites from a giant impact in the early Solar System, Nature 436, 989–992, 2005]. Formation of later chondrules, and hence the parent bodies of some chondritic meteorites, must therefore have occurred in the presence of planetesimals large enough to possess iron cores. We conclude that early planetary accretion and differentiation was sufficiently fast for 26Al-decay to be an important heat source. Non-magmatic iron meteorites, however, display more radiogenic and varied W isotope signatures. This is in keeping with them being generated later, by impact melting during which the metal (partially) re-equilibrated with the then more radiogenic silicate fraction. 相似文献
13.
《Physics of the Earth and Planetary Interiors》2006,154(3-4):290-298
Thermally acquired remanent magnetization is important for the estimation of the past magnetic field present at the time of cooling. Rocks that cool slowly commonly contain magnetic grains of millimeter scale. This study investigated 1-mm-sized magnetic minerals of iron, iron–nickel, magnetite, and hematite and concluded that the thermoremanent magnetization (TRM) acquired by these grains did not accurately record the ambient magnetic fields less than 1 μT. Instead, the TRM of these grains fluctuated around a constant value. Consequently, the magnetic grain ability to record the ambient field accurately is reduced. Above the critical field, TRM acquisition is governed by an empirical law and is proportional to saturation magnetization (Ms). The efficiency of TRM is inversely proportional to the mineral's saturation magnetization Ms and is related to the number of domains in the magnetic grains. The absolute field for which we have an onset of TRM sensitivity is inversely proportional to the size of the magnetic grain. These results have implications for previous reports of random directions in meteorites during alternating field demagnetization, or thermal demagnetization of TRM. Extraterrestrial magnetic fields in our solar system are weaker than the geomagnetic field by several orders of magnitude. Extraterrestrial rocks commonly contain large iron-based magnetic minerals as a common part of their composition, and therefore ignoring this behavior of multidomain grains can result in erroneous paleofield estimates. 相似文献
14.
The possibility that the parent body of the SNC meteorites is Mars implies that the magnetic properties of these meteorites may provide evidence concerning ancient Martian magnetic fields. EETA 79001 possesses a weak, very stable primary magnetization, the properties of which are consistent with its acquisition in an ambient magnetic field either during the meteorite's formation or during the severe shock event later in its history. The samples of ALHA 77005 studied possessed no measurable primary magnetization: the observed remanence appears to be a viscous magnetization acquired in local laboratory fields. The magnetic carriers in the meteorites are fine-grained magnetite and a lower Curie point mineral, probably titanomagnetite or pyrrhotite, present to the extent of less than 0.1% by weight. Estimates of the strength of the magnetizing field for EETA 79001 are in the range 1–10 μT. 相似文献
15.
对贵州省麦岗水库沉积物环境磁性特征的研究表明,亚铁磁性矿物主导了沉积物矿物磁性特征,但同时也存在反铁磁性矿物等其他矿物,超顺磁颗粒在沉积物中广泛存在.在所选矿物磁性参数中,χlf、χfd、SOFT与粒度不相关;χARM、SIRM、F300与粒度相关,但相关系数不高;χARM/χlf、χARM/SIRM和粒度显著相关,可以作为粒度的代用指标.研究结果显示,磁性参数确实可以作为粒度的代用指标.但对比研究表明,在不同沉积环境,甚至相似沉积环境的沉积物中,矿物磁性参数和粒度的关系可能不同,在特定沉积环境中,利用磁性参数作为粒度的代用指标应该在充分研究的基础上进行,使研究结果更为可靠. 相似文献
16.
A. V. Belov E. A. Eroshenko V. G. Yanke V. A. Oleneva M. A. Abunina A. A. Abunin 《Geomagnetism and Aeronomy》2018,58(3):356-372
One of the variants of the global survey method developed and used for many years at the Institute of Terrestrial Magnetism, Ionosphere, and Radio Wave Propagation of the Russian Academy of Sciences is described. Data from the world network of neutron monitors for every hour from July 1957 to the present has been processed by this method. A consistent continuous series of hourly characteristics of variation of the density and vector anisotropy of cosmic rays with a rigidity of 10 GV is obtained. A database of Forbush decreases in galactic cosmic rays caused by large-scale disturbances of the interplanetary medium for more than half a century has been created based on this series. The capabilities of the database make it possible to perform a correlation analysis of various parameters of the space environment (characteristics of the Sun, solar wind, and interplanetary magnetic field) with the parameters of cosmic rays and to study their interrelationships in the solar–terrestrial space. The features of reception coefficients for different stations are considered, which allows the transition from variations according to ground measurements to variations of primary cosmic rays. The advantages and disadvantages of this variant of the global survey method and the opportunities for its development and improvement are assessed. The developed method makes it possible to minimize the problems of the network of neutron monitors and to make significant use of its advantages. 相似文献
17.
铁镍合金是陨石中重要的磁性物质,其中铁纹石、镍纹石和四方镍纹石是球粒陨石中的主要铁镍合金.然而,迄今针对陨石中铁镍合金的磁学性质研究仍非常缺乏.本文研究了吉林陨石中的铁纹石、四方镍纹石、以及陨硫铁的磁学特征.实验表明,镍含量为6%~7%的铁纹石是该陨石中最主要的铁镍合金物质,它具有低矫顽力和高的热稳定性,居里温度~750 ℃.镍含量为~48%的四方镍纹石具有高矫顽力和高的热稳定性,居里温度~565 ℃,它是剩磁的主要载体.陨硫铁在室温为反铁磁性,不具有载剩磁能力,在60 K左右存在一个低温转换,在氩气中加热较稳定而在空气中加热被氧化转化为磁铁矿.这些研究结果为鉴定球粒陨石中的磁性物质提供了依据. 相似文献
18.
The expedition for studying the Volga R. was organized by the Institute of Oceanology, Russian Academy of Sciences and the Institute of Inland Water Biology, Russian Academy of Sciences, with the participation of the Institute of Geochemistry and Analytical Chemistry on the r/v Akademik Topchiev (June 2–18, 2016). The main objective of the expedition studies of the Institute of Oceanology, Russian Academy of Sciences, was to examine the sedimentation and biogeochemical processes in the mixing zone of the Volga and its tributaries with the aim to assess the present-day water quality and trends in its changes in the recent years. In this context, the study was focused on the aerosols of near-water layer, surface water, and bottom sediments along the route the Rybinsk Reservoir (Borok Settl.)–Lower Volga (Astrakhan C.). The methodology was based on a multidisciplinary study of dissolved compounds and suspended particles (<1 μm). The main attention was focused on studying the spatial variations of biogenic substances, organic compounds (Corg in suspension and solution), the suspension itself, and hydrcarbons. 相似文献
19.
Magnetic mineral diagenesis in the post-glacial muddy sediments from the southeastern South Yellow Sea: Response to marine environmental changes 总被引：2，自引：1，他引：1
Jeong-Hae Chang 《中国科学D辑(英文版)》2005,48(1):134-144
Core YSDP103 was retrieved in the muddy deposit under the cold eddy of the southeastern South Yellow Sea, and the uppermost 29.79 m core represents the muddy sediments formed in the shelf since about 13 ka BP. The lower part from 29.79 to 13.35 m, called Unit A2, was deposited during the period from the post-glacial transgression to the middle Holocene (at about 6 14C ka BP) when the rising sea level reached its maximum, while the upper part above 13.35 m (called Unit A1) was deposited in a cold eddy associated with the formation of the Yellow Sea Warm Current just after the peak of post-glacial sea level rise. Rock-magnetic properties of the uppermost 29.79 m core were investigated in detail. The experimental results indicate that the magnetic mineralogy of the core is dominated by magnetite, maghemite and hematite and that, except for the uppermost 2.35 m, the magnetic minerals were subject to reductive diagene-sis leading to significant decline of magnetic mineral content and the proportion of low-coe 相似文献
20.
Petromagnetic features of sediments at the Mesozoic-Cenozoic boundary: Results from the Gams section
D. M. Pechersky A. F. Grachev D. K. Nourgaliev V. A. Tselmovich Z. V. Sharonova 《Izvestiya Physics of the Solid Earth》2008,44(5):401-420
The paper continues a cycle of petromagnetic investigations of epicontinental deposits at the Mesozoic-Cenozoic (K/T) boundary and is devoted to the study of the Gams section (Austria). Using thermomagnetic analysis, the following magnetic phases are identified: goethite (T C = 90–150°C), hemoilmenite (T C = 200?300°C), metallic nickel (T C = 350–360°C), magnetite and titanomagnetite (T C = 550–610°C), Fe-Ni alloy (T C = 640–660°C), and metallic iron (T C = 740–770°C). Their concentrations are determined from M(T). In all samples, ensembles of magnetic grains have similar coercivity spectra and are characterized by a high coercivity. An exception is the lower coercivity of the boundary clay layer due to grains of metallic nickel and iron. With rare exceptions, the studied sediments are anisotropic and generally possess a magnetic foliation, which indicates a terrigenous accumulation of magnetic minerals. Many samples of sandy-clayey rocks have an inverse magnetic fabric associated with the presence of acicular goethite. The values of paramagnetic and diamagnetic components in the deposits are calculated. According to the results obtained, the K/T boundary is marked by a sharp increase in the concentration of Fe hydroxides. The distribution of titanomagnetite reflects its dispersal during eruptive activity, which is better expressed in the Maastrichtian and at the base of the layer J. The along-section distribution of metallic iron, most likely of cosmic origin, is rather uniformly chaotic. The presence of nickel, most probably of impact origin, is a particularly local phenomenon as yet. The K/T boundary is not directly related to an impact event. 相似文献