I-Xe and ⁴⁰Ar-³⁹Ar dating of silicate from Weekeroo Station and Netschaëvo IIE iron meteorites     

Sidney Niemeyer 《Geochimica et cosmochimica acta》1980,44(1):33-44

Silicate inclusions from two IIE iron meteorites were dated by the I-Xe and ⁴⁰Ar-³⁹Ar techniques. Weekeroo Station, a ‘normal’ IIE iron, shows no loss of radiogenic ⁴⁰Ar at low temperature, and the well-defined ⁴⁰Ar-³⁹Ar plateau yields an age of 4.54 ± 0.03 Byr. The xenon data define a good I-Xe correlation with an age of +10.9 ± 0.5 Myr relative to Bjurböle [the monitor error (±2.5 Myr) is not included].^Despite its relatively young age, Weekeroo Station's $\text{(}{}^{129}\text{Xe}{}^{132}\text{Xe)}{}_{\mathrm{trappad}}$ ratio (= 0.84 ± 0.05) lies significantly below the solar value. Netschaëvo silicate has a chondritic composition, unlike ‘normal’ IIE silicate which is more differentiated. Nevertheless Netschaëvo gives a ⁴⁰Ar-³⁹Ar plateau-age of only 3.79 ± 0.03 Byr, with the xenon data failing to define an I-Xe isochron.Only irons from the IAB and IIE groups contain silicate inclusions, but these two groups differ in many other respects, mostly suggesting that IAB meteorites are more primitive. The I-Xe chronology supports this suggestion inasmuch as Weekeroo Station formed well after (8–15 Myr) IAB silicates. In terms of Scott and Wasson's (1976) model, ages for Weekeroo Station date the shock event which formed ‘normal’ IIE irons by mixing the low-melting fraction of the parent silicate with shock-liquefied metal. Scott and Wasson's suggestion that Netschaëvo represents IIE parent material, however, is contradicted by Netschaëvo's 3.8 Byr age.The four silicate-bearing IIE irons which have now been dated can be subdivided into distinct pairs: Weekeroo Station and Colomera formed near the beginning of the solar system, while Netschaëvo and Kodaikanal both formed only 3.8 Byr ago. A review of other properties of these meteorites generally support this subdivision.This work underscores the complexity of the history of IIE meteorites; in particular, an adequate model must account for the formation of two IIE irons at 3.8 Byr without disturbing rare gases in Weekeroo Station. All formation models are quite speculative, but the one which seems best to fit the available evidence postulates two parent bodies: the 3.8 Byr old silicate formed on one parent body, all other IIE material resided in a separate body, and subsequent collision(s) mixed the young silicate with IIE metal.  相似文献   

⁴⁰Ar-³⁹Ar dating of inclusions from IAB iron meteorites     

Sidney Niemeyer 《Geochimica et cosmochimica acta》1979,43(11):1829-1840

Silicate and troilite from IAB iron meteorites were dated by the ⁴⁰Ar-³⁹Ar technique. Silicate from four IAB meteorites gave well-defined apparent-age plateaus which accounted for 71–99% of the released ³⁹Ar. At low temperatures, only Copiapo showed appreciable loss of ⁴⁰Ar, while Mundrabilla and Woodbine released excess ⁴⁰Ar. The plateau ages are: 4.50 Byr for Copiapo, 4.57 Byr for Mundrabilla, 4.57 Byr for Woodbine, 4.54 Byr for unetched Pitts, and 4.57 Byr for etched Pitts; the 1σ error in each case is ± 0.03 Byr. A poorly-defined age plateau for Landes gives an age of 4.48 Byr, while the total K-Ar age (4.55 Byr) is significantly higher. The average $\text{(}{}^{40}\text{Ar/}{}^{36}\text{Ar)}$_trapped ratio for all silicate samples is 0.4 ± 0.4.Simple and undisturbed K-Ar systems are rare for meteorites, yet it appears to be a common feature for IAB silicates. In addition, plateau ages of IAB silicates are as old or older than the mean age of unshocked chondrites (4.47 Byr).Troilite samples yielded complex patterns which were evaluated via ⁴⁰Ar/³⁶Ar vs ³⁹Ar/³⁶Ar plots. Data for Pitts troilite are consistent with silicate and troilite retaining Ar at about the same time initially, but then 4.25 Byr ago nearly all the Ar in troilite was redistributed. The 700–1000°C points for Mundrabilla troilite define a line which gives an age of 6.2 Byr and $\text{(}{}^{40}\text{Ar/}{}^{36}\text{Ar)}{}_{\mathrm{trapped}}\text{= 42}$. This line may be an artifact, perhaps produced by homogenization of Ar and K.Approximate estimates of cosmic-ray exposure ages are 240 Myr for Landes, 130 Myr for Copiapo, 190 Myr for Woodbine, 170 Myr for Mundrabilla troilite, and 60 Myr for Pitts troilite.The I-Xe study of these same samples revealed a good correlation between well-defined I-Xe ages of silicates and Ni contents of metal (Niemeyer, 1979). The poorer resolution of the ⁴⁰Ar-³⁹Ar technique hampers a similar evaluation; nevertheless, plateau ages of the silicates suggest a systematic trend with Ni contents.  相似文献   

I-Xe dating of silicate and troilite from IAB iron meteorites     

Sidney Nemeyer 《Geochimica et cosmochimica acta》1979,43(6):843-860

The IAB iron meteorites may be related to the chondrites: siderophile elements in the metal matrix have chondritic abundances, and the abundant silicate inclusions are chondritic both in mineralogy and in chemical composition. Silicate and troilite (FeS) from IAB irons were analyzed by the I-Xe technique. Four IAB silicate samples gave well-defined I-Xe ages [in millions of years relative to Bjurböle; the monitor error (± 2.5 Myr) is not included]: ?3.7 ± 0.3 for Woodbine, ?0.7 ± 0. 6 for Mundrabilla, +1.4 ± 0.7 for Copiapo, and +2.6 ± 0.6 for Landes. The (¹²⁹Xe/¹³²Xe)_trapped ratios are consistent with previous values for chondrites, with the exception of Landes which has an extraordinary trapped ratio of 3.5 ± 0.2. Both analyses of silicate from Pitts gave anomalous I-Xe patterns.Troilite samples were also analyzed: Pitts troilite gave a complex I-Xe pattern, which suggests an age of +17 Myr; Mundrabilla troilite defined a good I-Xe correlation, which after correction for neutron capture on ¹²⁸Te gave an age of ?10.8 ± 0.7 Myr. Thus, surprisingly, low-melting troilite substantially predates high-melting silicate in Mundrabilla.Abundances of Ga, Ge, and Ni in metal from these meteorites are correlated with I-Xe ages of the silicate; meteorites with older silicates have greater Ni contents. No model easily accounts for this result as well as other properties of IAB irons; nevertheless, these results, taken at face value, overall favor a nebular formation model (e.g. Wasson, 1970, Icarus 12, 407–423). The great age of troilite from Mundrabilla suggests that this troilite formed in a different nebular region from the silicate and metal, and was later mechanically mixed with these other phases.The correlation between the trace elements in the metal and the I-Xe ages of the silicate provides one of the first known instances in which another well-defined meteoritic property correlates with I-Xe ages. In addition, almost all the ¹²⁹Xe in Mundrabilla silicate (etched in acid) was correlated with ¹²⁸Xe. These two results further support the validity of the I-Xe dating method.  相似文献   

Ar-Ar and I-Xe ages and thermal histories of three unusual metal-rich meteorites     

Donald D. Bogard  Daniel H. Garrison 《Geochimica et cosmochimica acta》2009,73(22):6965-6983

Portales Valley, Sombrerete, and Northwest Africa (NWA) 176 are three unrelated meteorites, which consist of silicate mixed with substantial amounts of metal and which likely formed at elevated temperatures as a consequence of early impacts on their parent bodies. Measured ³⁹Ar-⁴⁰Ar ages of these meteorites are 4477 ± 11 Ma and 4458 ± 16 Ma (two samples of Portales Valley), 4541 ± 12 Ma, and 4524 ± 13 Ma, respectively (Ma = million years; all one-sigma errors). The Ar-Ar data for Portales Valley show no evidence of later open system behavior suggested by some other chronometers. Measured ¹²⁹I-¹²⁹Xe ages of these three meteorites are 4559.9 ± 0.5 Ma, 4561.9 ± 1.0 Ma, and ∼4544 Ma, respectively (relative to Shallowater = 4562.3 ± 0.4 Ma). From stepwise temperature release data, we determined the diffusion characteristics for Ar and Xe in our samples and calculated approximate closure temperatures for the K-Ar and I-Xe chronometers. Adopting results and interpretations about these meteorites from some previous workers, we evaluated all these data against various thermal cooling models. We conclude that Portales Valley formed 4560 Ma ago, cooled quickly to below the I-Xe closure temperature, then cooled deep within the parent body at a rate of ∼4 °C/Ma through K-Ar closure. We conclude that Sombrerete formed 4562 Ma ago and cooled relatively quickly. NWA 176 likely formed and cooled quickly ∼4544 Ma ago, or later than formation times of most meteorite parent bodies. For all three meteorites, the Ar-Ar ages are in better agreement with I-Xe ages and preferred thermal models if we increase these Ar-Ar ages by ∼20 Ma. Such age corrections would be consistent with probable errors in ⁴⁰K decay parameters in current use, as suggested by others. The role of impact heating and possible disruption and partial reassembly of meteorite parent bodies to form some meteorites likely was an important process in the early solar system.  相似文献   

Mineralogy, geochemistry, and Ar-Ar geochronology of lunar granulitic breccia Northwest Africa 3163 and paired stones: Comparisons with Apollo samples     

Jillian A. Hudgins  Randy L. Korotev 《Geochimica et cosmochimica acta》2011,75(10):2865-2881

The lunar meteorites Northwest Africa (NWA) 3163, 4881, and 4483 are paired stones classified as granulitic breccias. At 2.4 kg, these three stones constitute one of the largest known lunar meteorite masses. Here we describe the petrography, mineralogy, and chemistry of NWA 3163, 4881, and 4483, and present ⁴⁰Ar-³⁹Ar data for two of the meteorites. Two-pyroxene thermometry indicates that the rocks equilibrated at 1050 ± 50 °C, which represents the high-temperature, low-pressure event that generated their characteristic recrystallization textures and reset their Ar systematics. Stepped-heating, in situ infrared laser microprobe ⁴⁰Ar-³⁹Ar geochronology yields a mean age of 3327 ± 29 Ma for NWA 3163, and a more disturbed release spectrum for NWA 4881. NWA 4881 shows an upward-trending pattern, suggesting that it may have had a ⁴⁰Ar-³⁹Ar age of >3.0 Ga, but that it was partially reset at ∼2.6 Ga. NWA 3163 et al. exhibit shock effects, including maskelynitized plagioclase, shock veins, and melt pockets, which are absent in the Apollo granulitic breccias. Although the Apollo and meteorite samples are texturally similar and have comparable bulk compositions and equilibration temperatures, their trace and siderophile element contents point to distinct parental lithologies derived from different regions of the Moon. Based on mineralogical and geochemical differences between the Apollo and meteorite samples, we conclude that the parent rock(s) of the paired NWA meteorites came from an area outside the Imbrium region and that they underwent high-temperature (granulite event) metamorphism long after the Late Heavy Bombardment.  相似文献   

⁴⁰Ar-³⁹Ar ages and trace element contents of Apollo 14 breccias; an interlaboratory cross-calibration of ⁴⁰Ar-³⁹Ar standards     

E.Calvin Alexander  Paul K. Davis 《Geochimica et cosmochimica acta》1974,38(6):911-928

Rare gas data are presented from step-wise heatings of lunar breccias 14066 and 14318 and from an interlaboratory cross-calibration of five standards used in ⁴⁰Ar-³⁹Ar dating. Four samples of 14066 all show depressed ⁴⁰¹Ar/³⁹¹Ar ratios at high temperatures, thus making age interpretation uncertain. While different in detail, the Ar release patterns in the four samples yield indistinguishable plateau ages of $\text{3.93 ± 0.03}$ b.y. and > 400°C total ages of $\text{3.87 ± 0.06}$ b.y. Concentrations of K, Ca, Ba, Br, U and I are given for 14318 and 14066. We also present an updating of all of the ⁴⁰Ar-³⁹Ar ages and trace element concentrations previously published by this laboratory.⁴⁰Ar-³⁹Ar dating standards from Menlo Park, Pasadena, Stony Brook, Toronto and Berkeley are calibrated against each other and the internal homogeneity of their ⁴⁰¹Ar/K ratios is tested. The Berkeley standard (from the St. Severin meteorite) has an age of $\text{4.504 ± 0.020}$ b.y. from this intercalibration.⁸⁰Kr from capture of lunar neutrons is detected in 14318. A comparison of the release pattern of the ⁸⁰Kr produced by lunar neutrons with the ^80,82Kr produced by pile neutrons in 14318, indicates that 14318 has lost approximately 35 per cent of the ⁸⁰Kr produced by lunar neutrons.  相似文献   

K–Ar ages of meteorites: Clues to parent-body thermal histories     

Donald D. Bogard 《Chemie der Erde / Geochemistry》2011,71(3):207-226

Whereas most radiometric chronometers give formation ages of individual meteorites >4.5 Ga ago, the K–Ar chronometer rarely gives times of meteorite formation. Instead, K–Ar ages obtained by the ³⁹Ar–⁴⁰Ar technique span the entire age of the solar system and typically measure the diverse thermal histories of meteorites or their parent objects, as produced by internal parent body metamorphism or impact heating. This paper briefly explains the Ar–Ar dating technique. It then reviews Ar–Ar ages of several different types of meteorites, representing at least 16 different parent bodies, and discusses the likely thermal histories these ages represent. Ar–Ar ages of ordinary (H, L, and LL) chondrites, R chondrites, and enstatite meteorites yield cooling times following internal parent body metamorphism extending over ∼200 Ma after parent body formation, consistent with parent bodies of ∼100 km diameter. For a suite of H-chondrites, Ar–Ar and U–Pb ages anti-correlate with the degree of metamorphism, consistent with increasing metamorphic temperatures and longer cooling times at greater depths within the parent body. In contrast, acapulcoites–lodranites, although metamorphosed to higher temperatures than chondrites, give Ar–Ar ages which cluster tightly at ∼4.51 Ga. Ar–Ar ages of silicate from IAB iron meteorites give a continual distribution across ∼4.53–4.32 Ga, whereas silicate from IIE iron meteorites give Ar–Ar ages of either ∼4.5 Ga or ∼3.7 Ga. Both of these parent bodies suffered early, intense collisional heating and mixing. Comparison of Ar–Ar and I–Xe ages for silicate from three other iron meteorites also suggests very early collisional heating and mixing. Most mesosiderites show Ar–Ar ages of ∼3.9 Ga, and their significantly sloped age spectra and Ar diffusion properties, as well as Ni diffusion profiles in metal, indicate very deep burial after collisional mixing and cooling at a very slow rate of ∼0.2 °C/Ma. Ar–Ar ages of a large number of brecciated eucrites range over ∼3.4–4.1 Ga, similar to ages of many lunar highland rocks. These ages on both bodies were reset by large impact heating events, possibly initiated by movements of the giant planets. Many impact-heated chondrites show impact-reset Ar–Ar ages of either >3.5 Ga or <1.0 Ga, and generally only chondrites show these younger ages. The younger ages may represent orbital evolution times in the asteroid belt prior to ejection into Earth-crossing orbits. Among martian meteorites, Ar–Ar ages of nakhlites are similar to ages obtained from other radiometric chronometers, but apparent Ar–Ar ages of younger shergottites are almost always older than igneous crystallization ages, because of the presence of excess (parentless) ⁴⁰Ar. This excess ⁴⁰Ar derives from shock-implanted martian atmosphere or from radiogenic ⁴⁰Ar inherited from the melt. Differences between meteorite ages obtained from other chronometers (e.g., I–Xe and U–Pb) and the oldest measured Ar–Ar ages are consistent with previous suggestions that the ⁴⁰K decay parameters in common use are incorrect and that the K–Ar age of a 4500 Ma meteorite should be possibly increased, but by no more than ∼20 Ma.  相似文献   

Noble gas retention chronologies for the St Séverin meteorite     

C.M Hohenberg  B Hudson  B.M Kennedy  F.A Podosek 《Geochimica et cosmochimica acta》1981,45(4):535-546

⁴⁰Ar-³⁹Ar and ¹²⁹Xe-¹²⁸Xe analyses were performed on two lithologies (light and dark) of the St Séverin (LL6) chondrite. For the light and dark fractions, respectively, we obtained ⁴⁰Ar retention ages of 4.38 and 4.42 AE and ¹²⁹Xe retention ages of 8.4 and 15.2 myr after Bjurböle. The two methods give age differences of opposite sense, and by both methods the differences are significant. Both the ⁴⁰Ar and the ¹²⁹Xe ages are interpreted as dating relaxation of metamorphic conditions. These two chronometers are decoupled, however, and do not date the same events. ⁴⁰Ar-³⁹Ar reflect chondritic metamorphisrn on a 10⁸ yr time scale. The ¹²⁹Xe-¹²⁸Xe ages reflect isotopic closure at higher temperatures and earlier times.  相似文献   

The Chassigny meteorite: a cumulate dunite with hydrous amphibole-bearing melt inclusions     

R.J. Floran  Martin Prinz  P.F. Hlava  Klaus Keil  C.E. Nehru  J.R. Hinthorne 《Geochimica et cosmochimica acta》1978,42(8):1213-1229

The Chassigny meteorite is a moderately shocked olivine achondrite or chassignite with features indicative of a cumulate origin with some subsolidus annealing. Chassigny is an iron-rich dunite (Fo₆₈) with minor amounts of Ca-rich and Ca-poor pyroxene, alkalic feldspar, chromite, and melt inclusions in olivine. Accessory phases include chlorapatite, troilite, marcasite, kaersutite amphibole, pentlandite, ilmenite, rutile and baddeleyite. The meteorite experienced shock pressures of ~150–200 kbar as evidenced by planar and irregular fractures in olivine, local recrystallization in pyroxene and reduced birefringence and rare deformation lamallae in feldspar. Kaersutitic amphibole (K_0.05 Na_0.45)_0.50 (Ca_1.71 Na_0.29)_2.00 (Mg_2.73 ‘Fe’_1.19 Ti_0.73 A1_0.23 Cr_0.08 Mn_0.03)_4.99 (Si_6.05Al_1.95)_8.00 O₂₂ (OH, F)₂ containing hydrogen and lesser amounts of fluorine represents the first extraterrestrial occurrence of hydrous amphibole and the first meteoritic amphibole type other than fluorichterite. Kaersutite is found only in melt inclusions.Melt inclusion bulk compositional data suggest crystallization from a low-Ca melt that may have been similar in major element abundances to the silicate portion of LL group chondrites. However, Chassigny has a fractionated pattern for REE and the lack of metallic iron, possible presence of minor Ni in the olivine and Fe³⁺ in the chromites indicates that Chassigny formed under relatively more oxidizing conditions than most other achondrites. Therefore its parental melt could not have been directly derived from a chondritic composition in a simple single-stage process. The iron-rich bulk composition, cumulate texture and abundance as well as alkalic nature of the interstitial feldspar indicate that Chassigny could not have generated eucritic magmas. This places further constraints on its relationship to other meteorites and the parent body from which it is derived. The Brachina meteorite is similar to Chassigny except that it is finer grained, more feldspathic and is unshocked. It extends the fractionation range of this group which now represents two unusual meteorites.  相似文献   

应用⁴⁰Ar—³⁹Ar定年技术研究某些火山岩及陨石样品的受热历史   总被引：4，自引：0，他引：4       下载免费PDF全文

王松山 《地质科学》1982,(2):226-234

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   

Noble gases,nitrogen and cosmic ray exposure age of the Sulagiri chondrite     

Ramakant R. Mahajan 《地学前缘(英文版)》2017,8(1):205-210

The Sulagiri meteorite fell in India on 12 September 2008,LL6 chondrite class is the largest among all the Indian meteorites.Isotopic compositions of noble gases(He,Ne,Ar,Kr and Xe) and nitrogen in the Sulagiri meteorite and cosmic ray exposure history are discussed.Low cosmogenic(~(22)Ne/~(21)Ne)_c ratio is consistent with irradiation in a large body.Cosmogenic noble gases indicate that Sulagiri has a 4πcosmic-ray exposure(CRE) age of 27.9 ± 3.4 Ma and is a member of the peak of CRE age distribution of IX chondrites.Radiogenic ~4He and ~(40)Ar concentrations in Sulagiri yields the radiogenic ages as 2.29 and4.56 Ca,indicating the loss of He from the meteorite.Xenon and krypton are mixture of Q and spallogenic components.  相似文献   

Ar/Ar thermochronology of the fossil LL6-chondrite from the Morokweng crater, South Africa     

F. Jourdan  M.A.G. Andreoli  I. McDonald 《Geochimica et cosmochimica acta》2010,74(5):1734-1747

Studies of meteorites are based mostly on samples that fell to Earth in the recent past (i.e., a few million years at most). The Morokweng LL-chondrite meteorite is a particularly interesting specimen as its fall is much older (ca. 145 Ma) than most other meteorites and because it is the only macro-meteorite clast (width intersected in drill core: 25 cm) found in a melt sheet of a large impact structure. When applied to the Morokweng meteorite, ⁴⁰Ar/³⁹Ar thermochronology provides an opportunity to study (1) effects associated with pre-impact and post-impact processes and (2) collision events within a potentially distinct and as yet unsampled asteroid population.A single multi-grain aliquot yielded an inverse isochron age of 625 ± 163 Ma. This suggests a major in-space collisional event at this time. We have modeled the diffusion of ⁴⁰Ar^∗ within the meteorite and plagioclase during and after the ∼145 Ma impact on Earth to tentatively explain why pre-terrestrial impact ⁴⁰Ar^∗ has been preserved within the plagioclase grains. The ∼145 Ma terrestrial impact age is recorded in the low-retentivity sites of the meteorite plagioclase grains that yielded a composite inverse isochron age at 141 ± 15 Ma and thus, confirms that age information about major (terrestrial or extraterrestrial) impacts can be recorded in the K-rich mineral phases of a meteorite and measured by the ⁴⁰Ar/³⁹Ar technique. More studies on fossil meteorites need to be carried out to understand if the rough 0.6 Ga age proposed here corresponds to major LL-chondrite asteroid population destructions or, rather, to an isolated collision event.  相似文献   

The compositional classification of chondrites: IV. Ungrouped chondritic meteorites and clasts     

Gregory W. Kallemeyn  John T. Wasson 《Geochimica et cosmochimica acta》1985,49(1):261-270

Six specimens of unusual chondritic materials were analyzed by neutron activation for 30 elements in order to assess their degree of chondritic compositional pristinity and to search for evidence of genetic links to other chondrites. Five have highly recrystallized textures; the other, the Cumberland Falls chondrite, has suffered minor metamorphic recrystallization. Acapulco and Allan Hills A77081, are closely related and have subpristine compositions; they are more distantly related to Enon which has an altered composition. Udei Station appears to be a IAB meteorite even though its $\text{FeO}\text{(FeO + MgO)}$ ratio is slightly above the IAB field. The highly weathered meteorite Tierra Bianca is closely related to IAB but has a δ¹⁸O value 5 standard deviations higher than the IAB mean and is designated ungrouped. Udei Station and Tierra Bianca have altered compositions; rare earth element patterns indicate loss of a phosphate phase. The elemental composition of the Cumberland Falls chondrite is virtually identical to that of LL chondrites and its O-isotope composition is closely similar to those of some unequilibrated ordinary chondrites including LL Semarkona. The $\text{FeO}\text{(FeO + MgO)}$ ratios in its olivine are generally much lower than those in pyroxene, a relationship we show to be indicative of in situ reduction resulting from exchange with the aubritic host. The names winonaites and forsterite chondrites have no taxonomic utility.  相似文献   

The I-Xe chronometer     

C. M. Hohenberg  R. H. Brazzle  O. V. Pravdivtseva  A. P. Meshik 《Journal of Earth System Science》1998,107(4):413-423

¹²⁹Xe, from the decay of the now-extinct 16.7 Ma¹²⁹I, accumulates in iodine-bearing sites and since most iodine host phases are secondary, the I-Xe system is typically a chronometer for post-formational processes. The validity of the I-Xe chronometer is confirmed by comparison with Pb-Pb ages on phosphate and feldspar separates from twelve meteorites. Phosphate separates are found to be concordant with Pb-Pb for all six samples in which useful I-Xe data were obtained. Feldspar is a better iodine host than apatite in H chondrites, typically providing good I-Xe isochrons. These too are concordant with the Pb-Pb ages of the corresponding phosphates for five out of six feldspar separates. The exception is Allegan whose feldspar yields one of the oldest I-Xe ages observed, similar to those for CI and CM magnetites. We attribute this to a more primary mineralization, predating the secondary phosphate from which the comparison Pb-Pb age was obtained. Absolute I-Xe ages, found using the reported Pb-Pb age of Acapulco phosphate provide an absolute I-Xe age of 4.566 ± 0.002 Ga for both Shallowater and Bjurböle irradiation standards. This allows relative I-Xe ages to be interpreted in the context of absolute ages.  相似文献   

Chronology and petrogenesis of young achondrites,Shergotty, Zagami,and ALHA77005: late magmatism on a geologically active planet     

C.-Y. Shih  L.E. Nyquist  D.D. Bogard  G.A. McKay  J.L. Wooden  B.M. Bansal  H. Wiesmann 《Geochimica et cosmochimica acta》1982,46(11):2323-2344

A study was undertaken to determine the chronology, petrogenesis and relationships among the shergottites, Shergotty and Zagami and the unique achondrite ALHA77005. These meteorites are the product of a variety of complex processes.Petrogenesis: Chondrite-normalized abundance patterns of Shergotty and Zagami are very similar and show pronounced depletions of both the light REE (La-Nd) and heavy REE (Dy-Lu) relative to Sm-Gd. These characteristic depletions are even more pronounced for ALHA77005. The light REE depletion is qualitatively consistent with the presence of cumulus pyroxene and/or olivine in these meteorites, but trace element models show that the parental magmas of all three meteorites were probably also light REE depleted. Both trace element model calculations and combined Rb-Sr and Sm-Nd isotopic systematics show that the meteorites could not have been co-magmatic nor can ALHA77005 be representative of the source material of the shergottites. Light REE depletion of the parental magmas also implies light REE depletion of the source material. The Sm-Nd systematics of the shergottites require a time-averaged sub-chondritic (light REE enriched) Sm-Nd ratio since 4.6 AE ago. The Sm-Nd systematics of ALHA77005 permit a time-averaged super-chondritic (light REE depleted) Sm/Nd ratio if its crystallization age is less than T_ICE = 0.72 AE.Chronology. Rb-Sr internal isochrons for all three meteorites and a Sm-Nd internal isochron for Zagami are concordant at ~ 180 Myr. ³⁹Ar-⁴⁰Ar plateau ages of Shergotty and Zagami maskelynite are ~250–260 Myr. These ages apparently reflect resetting of these isotopic systems by shock metamorphism which converted the feldspar to maskelynite. The concordance of these ages suggests a single shock event during which the meteorites were in close physical proximity. The time of this event is most precisely given by the Rb-Sr age of 180 ± 4 Myr for Zagami.The crystallization ages of the meteorites were not precisely determined. Extreme upper limits are determined by Sm-Nd model ages relative to an eucrite initial ${}^{143}\text{Nd}{}^{144}\text{Nd = 0.505835}$ at 4.6 AE ago. These model ages for Shergotty, Zagami and ALHA77005 are 3600, 3500 and 2850 Myr, respectively. The Sm-Nd whole rock age of 1340 ± 60 Myr for the three meteorites gives the crystallization age if the Sm/Nd ratios of the precursor materials were always the same. We consider this 1340 Myr age as a “best estimate” upper limit. “Best estimate” lower limits for Shergotty and Zagami are taken from the average ³⁹Ar-⁴⁰Ar ages of 1200 and 900 Myr of pyroxene separates. The average ³⁹Ar-⁴⁰Ar age of a whole rock sample of ALHA77005 was 1600 Myr and can be partitioned between a low temperature (feldspar) phase and a high temperature (olivine + pyroxene + inclusions) “phase”. The average apparent ³⁹Ar-⁴⁰Ar age of the low temperature phase is ~1050 Myr, which is chosen as the “best estimate” lower limit to the age. The crystallization ages of Shergotty, Zagami and ALHA77005 probably lie within the ranges of 1200–1300, 900–1300 and 1000–1300 Myr, respectively. The Rb-Sr whole rock age of 4400 ± 400 Myr and single-stage BABI model ages of ~4800–5100 Myr are interpreted as reflecting differentiation of the parent body at ~4600 Myr ago.The complex geochemical and isotopic evolution recorded by these meteorites suggests a geologically active parent body capable of sustaining melting at two or more epochs in its history.  相似文献   

内蒙古大青山逆冲推覆体系中生代逆冲构造活动的⁴⁰Ar-³⁹Ar定年   总被引：3，自引：2，他引：1  

张进江  戚国伟  郭磊  刘江 《岩石学报》2009,25(3):609-620

内蒙古大青山呼和浩特段北侧发育3条走向北东东、指向北西的逆冲断层,并与被其分割的3个逆冲席体及一个原地系构成大青山逆冲推覆体系。逆冲断层上盘底部发育较深层次的糜棱岩,下盘顶部多发育低温的千糜岩。本研究在构造地质调查基础上,结合宏-微观岩石矿物学分析,采用⁴⁰Ar-³⁹Ar定年对该逆冲体系的活动时间进行约束。逆冲断层带内3个千糜岩绢云母⁴⁰Ar-³⁹Ar年龄范围为120~119Ma,另一样品给出了120Ma的概率统计峰值年龄。千糜岩为低温同变形变质产物,细粒绢云母为同变形新生矿物,其⁴⁰Ar-³⁹Ar年龄可代表变形年龄。侵位在断层内弱变形的花岗闪长岩为同构造晚期侵位,角闪石⁴⁰Ar-³⁹Ar年龄限定其冷却时间下限为121Ma,概率统计峰值年龄为119Ma。逆冲断层上盘底部发育较高温的糜棱岩,而低温千糜岩的形成时间应属于变形后期。因此,120Ma至119Ma期间,大青山逆冲推覆体系的逆冲作用应已是处于变形晚期。  相似文献   

Barium silicates of the Berisal Complex, Switzerland: A study in geochronology and rare-gas release systematics     

C.J. Hetherington  I.M. Villa 《Geochimica et cosmochimica acta》2007,71(13):3336-3347

Barium silicate minerals such as celsian, ganterite, armenite, as well as Ba-bearing and Ba-free white mica from the Berisal Complex, Simplon Nappe, Swiss Alps, were dated by ³⁹Ar-⁴⁰Ar. Ages of Ba-free micas are ca. 17 Ma, while Ba and parentless ⁴⁰Ar are correlated in Ba silicates, suggesting common inheritance from the Paleozoic orthogneissic protolith. The release pattern of reactor-produced ³⁹Ar (or ³⁷Ar) from hydrated and anhydrous minerals is very similar, with apparent activation energies of ca. 180 kJ/mole and a conspicuous kink around 900 °C. White micas release Ar at higher temperature than the literature determination of their dehydroxylation. In addition to Ar, we studied the degassing of monoisotopic ¹³¹Xe produced from Ba during neutron irradiation. Xe is degassed at higher temperature than Ar, and again all analyzed silicates have the same apparent activation energy of ca. 300 kJ/mole. The decoupling of Ar and Xe rules out delamination as the dominant degassing mechanism in mica and implies that recoiled rare gas atoms mostly reside inside the T-O-T layers of the mica structure. The near-identical apparent activation energies in such diverse silicates as tecto-, phyllo- and cyclosilicate requires instead that the in-vacuo gas release kinetics are the same in all three silicates. As the only structural element common to these three silicate families are silica tetrahedra, it is possible that their well-known rotation plays a decisive role for in-vacuo Ar degassing; additional high-temperature in situ structural investigations on feldspars and micas would be needed to help constrain the mechanisms of laboratory Ar release.  相似文献   

${}^{40}\text{Ar}{}^{39}\text{Ar}$ dating,Ar diffusion properties,and cooling rate determinations of severely shocked chondrites     

D.D. Bogard  W.C. Hirsch 《Geochimica et cosmochimica acta》1980,44(11):1667-1682

Determinations of ${}^{40}\text{Ar}{}^{39}\text{Ar}$ ages are reported for seven severely shock-heated chondrites. Shaw gives a plateau age of 4.29 Gyr. Louisville, Farmington, and Wickenburg give well-defined intercept ages of 0.5–0.6 Gyr. Orvinio, Arapahoe, and Lubbock show complex ${}^{40}\text{Ar}{}^{39}\text{Ar}$ release curves, with age minima of 0.7–1.0 Gyr. Degassing times of 0.5–1.0 Gyr are suggested for these meteorites. Most severely shocked chondrites were apparently not totally degassed of ⁴⁰Ar by the event, but retained from ~ 2 to ~45% of their ⁴⁰Ar. When calculated values of the diffusion parameter, $\text{D}\text{a}{}^2$, for Ar are examined in Arrhenius plots, they show two distinct linear relationships, which apparently correspond to the degassing of different mineral phases with distinct $\text{K}\text{Ca}$ ratios and different average temperatures for Ar release. The experimentally determined values of $\text{D}\text{a}{}^2$ for the high temperature phase of several severely shocked chondrites are ~10^?7 to 10^?5sec^?1 for their determined shock-heating temperatures of ~950°C to ~ 1200°C. The inferred reheating temperatures, $\text{D}\text{a}{}^2$ values, and fraction of ⁴⁰Ar loss during the reheating event for these seven chondrites suggest post-shock cooling rates and burial depth of ~ 10^?2 10^?4°C/sec and ~0.5–2m, respectively. For three chondrites these cooling rates agree with those determined from Ni diffusion in metal grains: for five chondrites the cooling rates derived from ⁴⁰Ar and Ni disagree by a factor of ~10⁵. It is suggested that five of these severely shocked chondrites were part of large ejecta blankets containing hot material and cold clasts with a distribution of sizes and that the cooling rate of this ejecta appreciably decreased as a function of time.  相似文献   

Further ${}^{40}\text{A}\text{r}{}^{39}\text{Ar}$ evidence for the multi-collisional heating of the Kirin chondrite     

T.Mark Harrison  Wang Sungshan 《Geochimica et cosmochimica acta》1981,45(12):2513-2517

Results of an ${}^{40}\text{Ar}{}^{39}\text{Ar}$Ar age spectrum obtained on a sample of the Kirin chondrite (K-5-13) show a similar character to previous published analyses of Kirin samples K-1 and K-2. The K-5-13 age spectrum shows clear evidence of having been substantially outgassed during a presumed collisional event about 0.5 Ga, ago, in good agreement with the estimate obtained from K-2, The differing amounts of ⁴⁰Ar loss registered by K-2 and K-5-13 during the 0.5 Ga event of about 60 and 50%, respectively, allows calculation of their vertical separation in the parent body at about 10cm.  相似文献   

桑干地区高压麻粒岩中石榴石和斜长石的连续激光 探针⁴⁰Ar-³⁹Ar等时年龄及其地质意义     

胡世玲郭敬辉  戴橦谟蒲志平 《岩石学报》1999,15(4):40

Continuous laser probe ⁴⁰Ar-³⁹Ar technique has been taken to carry out in situ analysis onto the metamorphic garnet and plagioclase from high-pressure basic granulites in Sanggan area of the North China craton. Garnet porphyroblasts was formed in the high-pressure granulite facies episode. In the symplectite assemblage arround garnet, plagioclase is one of the garnet breakdown products. Ar analysis of garnet porphyroblasts defines an ⁴⁰Ar-³⁹Ar isochron which gives out an age of 2510Ma, that indicates the high-pressure granulite facies metamorphic age. So, the Archaean high-pressure granulite metamorphism has been confirmed by this age dating. Another ⁴⁰Ar-³⁹Ar isochron age of 1968Ma has been obtained from Ar data of plagioclase. That should represent the age of garnet breakdown reaction. The >500Ma gap between the age of high-pressure metamorphism and garnet breakdown does not support the isothermal decompression P-T path given by petrological view. The symplectite assemblages are more likely to be formed during another medium-pressure metamorphism overprint. This conclusion will give a strong constraint on the crustal evolution of Sanggan area in the North China craton.  相似文献