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1.
新疆阿希低硫型金矿稀有气体同位素地球化学及其成矿意义 总被引：3，自引：4，他引：3
阿希是一个赋存在新疆西天山古生代陆相火山岩中的大型低硫型(冰长石-绢云母型)浅成低温热液金矿床.本文利用高真空惰性气体同位素质谱仪测定了阿希金矿黄铁矿中流体包裹体的稀有气体同位素组成,结果显示其~3He/~4He 比值为0.0218～0.138R_a,平均为0.044R_a;~(40)Ar/~(36)Ar 为317.7～866.0,平均为467.3,略高于大气中~(40)Ar/~(36)Ar 比值(295.5);~(20)Ne/~(22)Ne 和~(21)Ne/~(22)Ne 的比值分别为8.08～13.00和0.028～0.063,~(82)Kr/~(84)kr、~(83)Kr/~(84)kr、~(86)Kr/~(84) Kr 的比值分别为0.159～0.278、0.171～0.238、0.280～0.348,~(129)Xe/~(132)Xe 和~(134)XP/~(132)Xe 分别为0.96～1.017、0.401～0.443。流体包裹体~3He/~4He 显示成矿流体来自壳源,不舍幔源 He;流体中除壳源放射性成因~(40)Ar~*外,有大气 Ar 的参与,放射性成因~(40)Ar~*的含量为7.0%～65.9%,平均为29.0%,大气~(40)Ar 的贡献为43.0～93 0%,平均为71.0%,稀有气体同位素组成反映出阿希金矿成矿流体为循环的大气降水。F~(84)Ke 和 F~(129)Xe 值显示流体在成矿作用过程中曾发生过沸腾作用。 相似文献
2.
通过对宽甸新生代碱性玄武岩、地幔包体及辉石巨晶的稀有气体同位素组成的分析，认为不同岩性稀有气体含量的差异反映了岩浆作用过程中轻、重稀有气体的分馏特性，较轻的稀有气体(He、Ne)比较重的稀有气体(Kr、xe)具有更高的活动性和不相容性；该地区上地幔源区具有典型的MORB型源区特征，以辉石巨晶为代表；地幔包体的^3He／^4He值较低，可能是地幔流体交代作用造成的；大陆碱性玄武岩具有与大洋玄武岩截然不同的He同位素组成，反映了大陆区地幔岩浆上升过程中受到了陆壳物质混染。地幔源区^40Ar／^36Ar值为350左右，二辉橄榄岩和碱性火山岩的^40Ar／^36Ar值比大气略高，可能有大气组分的混合。部分样品中有^21Ne、^22Ne、^129Xe、^134Xe和^136Xe相对于大气的过剩现象，是核成因造成的。 相似文献
3.
辽宁宽甸新生代火山岩和地幔包体He-Ar同位素组成 总被引：8，自引：1，他引：8
宽甸新生代碱性玄武岩、地幔包体及辉石巨晶的稀有气体同位素组成和流体含量分析表明，不同岩性稀有气体含量的差异反映了岩浆作用过程中轻、重稀有气体的分馏特性，较轻的稀有气体(He、Ne)比较重的稀有气体(Kr、Xe)具有更高的活动性和不相容性；该地区上地幔源区具有典型的MORB型源区特征，以辉石巨晶为代表；地幔包体的3^He／^4He值较低，可能与地幔上隆过程中富集地幔流体的交代作用或地幔塑性变形作用丢失了部分原始He有关；大陆碱性玄武岩具有与大洋玄武岩截然不同的He同位素组成，反映了大陆区地幔岩浆上升过程中受到了陆壳物质混染。地幔源区^40Ar／^36Ar值为350左右，二辉橄榄岩和碱性火山岩的^40Ar／^36Ar值比大气略高，可能有大气组分的混入。部分样品中有^21Ne、^22Ne、^129Xe、^134Xe和^136Xe相对于大气的过剩现象。 相似文献
4.
CCSD中HP-UHP岩石稀有气体同位素地球化学及其对板块折返过程的示踪意义 总被引：1，自引：0，他引：1
利用高真空气相质谱系统测定了CCSD中HP-UHP变质岩中主要造岩矿物流体包裹体的稀有气体同位素组成,得出其3He/4He为(0.004~0.775)×10-6,相应R/Ra为0.003~0.553,40Ar/36Ar变化较大,为316.2~11358.8,高于大气40Ar/36Ar(295.5);20Ne/22Ne和21Ne/22Ne分别为9.47~12.4和0.026~0.051,而134Xe/132Xe和136Xe/132Xe分别为0.376~0.484和0.324~0.416,均高于其相应大气值。CCSD中HP-UHP岩石主要造岩矿物的He-Ar、Xe和Ne等同位素组成清楚显示其中流体包裹体主要由地壳变质流体和少量大气饱和水组成,而深源地幔流体组分很低,其中He主要来自地壳,Ar主要由壳源放射性成因40Ar*和少量(平均32.6%)大气Ar混合组成,少量Ne和Xe可能来自地幔。CCSD中HP-UHP岩石具有F40Ar相似文献
5.
测试并分析了柴北缘各油气田的14个天然气样品的氦、氩稀有气体同位素比值,并进行了气源对比。研究发现,柴北缘天然气40Ar/36Ar值分布在951～1712,平均1098,多数样品40Ar/36Ar较通常认为源于侏罗系的天然气40Ar/36Ar明显偏高,研究认为本区不存在幔源高40Ar/36Ar流体的介入,储层年代效应也不可能造成天然气40Ar/36Ar明显偏高,因此柴北缘天然气40Ar/36Ar明显偏高,主要是由于源岩年代积累效应引起的。据估算,气源岩年龄分布范围为164.7～460.8Ma,平均为345.1Ma,可能多数来源于石炭系。这一认识得到了柴北缘广泛分布有石炭系源岩和已发现源于石炭系原油的支持。柴北缘石炭系天然气的发现预示了柴北缘石炭系是一个新的油气勘探层系,从而拓展了柴北缘天然气勘探领域。 相似文献
6.
麦哲伦海山富钴结壳的稀有气体丰度及He、Ar同位素组成 总被引：3，自引：0，他引：3
使用MM5400质谱计对麦哲伦海山富钴结壳和结壳基岩进行稀有气体同位素分析,以此示踪结壳形成期间的海洋环境。富钴结壳的He、Ne、Ar、Kr、Xe稀有气体同位素丰度模式与ASW(air-saturated water,饱和空气的海水)的变化趋势一致,说明结壳是在与海水交换平衡的流体环境中形成的。结壳的分馏因子F_3比饱和空气的海水的F_3高2～3个数量级,表明其相对于海水而言是富集~3He的。其相对于空气亏损~3He、富集Kr和Xe的模式与高度富集~3He、亏损Kr和Xe的星际尘粒的模式完全不同,暗示地球外物质并不是支配富钴结壳稀有气体同位素丰度模式的主要因素。结壳中高的R值甚至超过上地幔代表MORB(大洋中脊玄武岩)的典型值8R_a(R_a为地球大气中~3He/~4He比值,R为样品中~3He/~4He比值),揭示了热点型地幔热液对西太平洋海洋环境的局部贡献。圈层结壳的各结壳层之间的R值差异明显,各结壳层之间的尺值的变化趋势是"较高→最高→较高",结壳中层具有高达15.60R_a的R值,明显有深部地幔流体的加入,这进一步表明滋养结壳生长的热液环境本质上是源于地幔柱型的热点热液。玄武质基岩具有较低的R值,说明该类基岩在形成时严重混染有地壳物质,也说明结壳的物源并非来自玄武质基岩。结壳的~(40)Ar/~(36)Ar比值接近于饱和空气的海水值,也表明结壳的成矿流体与周围海水发生了充分的交换。 相似文献
7.
滇西富碱斑岩型多金属矿区黄铁矿和石英脉流体包裹体中R/Ra值主要为0.160 8~3.470 0,远高于地壳特征值,而整体略低于地幔特征值;20 Ne/22 Ne和21 Ne/22 Ne平均值分别为11.271 0和0.032 2,接近地幔同位素组成;40 Ar/36 Ar和38 Ar/36 Ar平均值分别为395.510 0和0.197 6,均高于大气比值,而低于MORB比值;与大气相比,128 Xe/130 Xe、129 Xe/130 Xe、131 Xe/130 Xe、132 Xe/130 Xe、134 Xe/130 Xe、136 Xe/130 Xe值均表现出过剩的特征;富硅成矿流体的δ30Si值为-2.4‰~-0.1‰,表现出几乎未经动力分馏的原始地幔流体性质,而富碱岩浆的δ30Si值为0.0‰~0.4‰,表现出历经强烈动力分馏的交代富集地幔流体性质。综合研究表明:滇西地区硅同位素组成与包裹体稀有气体同位素组成在显示含矿流体的幔源特征的同时,又表现出强烈的地壳特征;成矿物质主要来自地幔交代作用形成的富集地幔分异产物,即富碱岩浆和与之伴随的富硅成矿流体,二者携带成矿物质沿断裂进入地壳,伴随富硅成矿流体在富碱岩浆的成岩过程中对富碱斑岩与地层岩石的交代蚀变,从而引发壳幔物质叠加混染。正是这种流体作用构成了滇西新生代富碱斑岩多金属成矿的内在统一制约因素。 相似文献
8.
云南大坪金矿白钨矿惰性气体同位素组成及其成矿意义 总被引：11，自引：6，他引：11
利用高真空气相质谱系统测定了云南大坪金矿白钨矿流体包裹体的惰性气体同位素组成,得出其~3He/~4He为(0．988～1．424)×10~(-6),平均1．205×10~(-6),相应R/R_a为0．706～1．018,平均0．898,~(40)Ar/~(36)Ar为1801．8～2663．8,远高于大气~(40)Ar/~(36)Ar;~(20)Ne/~(22)Ne和~(21)Ne/~(22)Ne分别为9．600～11．56和0．028～0．0467,而~(134)Xe/~(132)Xe和~(136)Xe/~(132)Xe分别为0．394～0．692和0．301～0．462,均高于其相应大气值;He-Ar、Ne和Xe同位素组成显示大坪金矿成矿流体主要由深源地幔流体和地壳流体组成,其中基本不含大气饱和水。大坪金矿的形成与该区壳幔相互作用有关:该区喜山早期地壳拉张引起的地幔岩浆上涌和去气形成深源地幔流体,下地壳在上涌地幔烘烤下形成富含CO_2、~(40)Ar、~(134)Xe、~(136)Xe和~4He的地壳流体,它们混合以后沿韧性剪切带上升,水-岩反应和沸腾作用导致矿质沉淀。因此,大坪金矿属于剪切带控制的深源热液型金矿。 相似文献
9.
10.
胜利油田天然气氩同位素特征 总被引：1，自引：0，他引：1
对胜利油田21个天然气样进行氩同位素组成分析,结合甲烷碳同位素组成特征和地质背景,阐明了天然气中40Ar/36Ar比值分布规律及其与源岩?储层的关系,进而讨论了天然气中空气氩和放射成因氩的分布规律,指出胜利油田存在着生物-热催化过渡带气?油田伴生气?煤型气和富CO2气?它们具有各自的氩?碳同位素组成和演化特征?第三系和中生界自生自储天然气的40Ar/36Ar比值分别为335和564?通过数学分析,首次确定古生界和前震旦系新生古储天然气的储层时代效应系数分别为1.25和1.47?并认为前震旦系储层中天然气来自第三系,而储于古生界的天然气是约70%的第三系油型气和约30%的中生界煤型气混合的结果?与岩浆作用有关的无机CO2和第三系有机成因烃类气混合形成平方王富CO2气藏? 相似文献
11.
The noble gas isotopic composition and content data of 2 alkali basalts, 3 Iherzolite xenoliths and one clinopyroxene megacryst from the Kuandian region have confirmed the occurrence of a fractionation of noble gases during magmatism. Light noble gases such as He and Ne are high in mobility and appear to be incompatible as compared with heavy ones ( such as Kr and Xe). Therefore, light noble gases are abundant in volcanics, especially in the volcanics with bubbles; lherzolite xenoliths have relatively high heavy noble gases. The clinopyroxene megacryst has the lowest abundance of noble gases, probably due to its high P-T origin. Noble gas isotopic composition of the clinopyroxene megacryst reveals that the mantle source beneath the Kuandian area has an MORB-like reservoir with^3 He/^4He ratio of—10 Ra(Ra: atmospheric^3 He/^4He ratio) and^40 Ar/^36 Ar ratio of 345.6. The Iherzolite xenoliths possess moderate^3 He/^4He ratios of 2.59 -4.53 Ra, reflecting the loss of primary helium during rock deformation or metasomatism caused by enriched mantle fluids during the up-lifting. The alkali volcanics have very low^3 He/^4 He ratios(0.47—0.61 Ra),indicating a contribution of radiogenic^4 He, probably having resulted from crust contamination. Most of the samples have excess^21 Ne and^22 Ne as compared with atmospheric neon, but Kr and Xe isotopic compositions are indistinguishable from atmospheric values within uncertainties with only individual samples having excess^129Xe,^134Xeand^136 Xe. 相似文献
12.
Abundances and isotopic compositions of Ne (in bulk samples only), Ar, Kr, and Xe have been investigated in 6 monomict, 3 polymict, and the diamond-free ureilite ALH78019 and their acid-resistant, C-rich residues. Isotopic ratios of Kr and Xe are very uniform and agree with data for ureilites from the literature. The measured ratio 38Ar/36Ar showed large variations due to an experimental artifact. This is shown to be connected to the pressure dependence of the instrumental mass discrimination, which for ureilites with their low abundance of 40Ar is different from that of the usual air standard. This observation necessitates a reassessment for the recently reported 36Ar excesses due to possible decay of extinct 36Cl in the Efremovka meteorite.Trapped 22Ne in the range of (1.4-2.5) × 10−8 cc STP/g is present in bulk ureilites. A Ne three-isotope plot for polymict ureilites indicates the presence of solar Ne. 21Ne-based cosmic ray exposure ages for the 10 ureilites studied range from 0.1 Ma (for ALH78019) to 46.8 Ma (for EET83309)All ureilites may have started with nearly the same initial elemental ratio (132Xe/36Ar)0, established in the nebula during gas trapping into their carbon carrier phases (diamond, amorphous C) by ion implantation. Whereas diamonds are highly retentive, amorphous C has suffered gas loss due to parent body metamorphism. The correlation of the elemental ratios 132Xe/36Ar and 84Kr/36Ar along the mass fractionation line could be understood as a two-component mixture of the unaffected diamond gases and the fractionated (to varying degrees) gases from amorphous C. In this view, the initial ratio (132Xe/36Ar)0 is a measure of the plasma temperature in the nebula at the formation location of the carbon phases. Its lack of correlation with Δ17O (a signature of the silicate formation location) indicates that carbon phases and silicates formed independently in the nebula, and not from a carbon-rich magmaThe elemental ratios 132Xe/36Ar and 84Kr/36Ar in carbon-rich acid residues show a decreasing trend with depth (inferred from carbon consumption during combustion), which can be interpreted as a consequence of the ion implantation mechanism of gas trapping that leads to greater depth of implantation for lighter mass ionThe similarity between trapped gases in phase Q in primitive chondrites and the C phases in ureilites—for both elemental and isotopic compositions—strongly suggests that phase Q might also have received its noble gases by ion implantation from the nebula. The slight differences in the elemental ratios can be explained by a plasma temperature at the location of phase Q gas loading that was about 2000 K lower than for ureilite C phases. This inference is also consistent with the finding that the trapped ratio 129Xe/132Xe (1.042 ± 0.002) in phase Q is slightly higher, compared to that of ureilite C phases (1.035 ± 0.002), as a consequence of in situ decay of 129I, and becomes observable due to higher value of I/Xe in phase Q as a result of ion implantation at about 2000 K lower plasma temperature. 相似文献
13.
Nadia Vogel Veronika S. Heber Donald S. Burnett 《Geochimica et cosmochimica acta》2011,75(11):3057-3071
We present bulk solar wind isotopic and elemental ratios for Ar, Kr, and Xe averaged from up to 14 individual analyses on silicon targets exposed to the solar wind for ∼2.3 years during NASA’s Genesis mission. All averages are given with 1σ standard errors of the means and include the uncertainties of our absolute calibrations. The isotopic ratios 86Kr/84Kr and 129Xe/132Xe are 0.303 ± 0.001 and 1.06 ± 0.01, respectively. The elemental ratios 36Ar/84Kr and 84Kr/132Xe are 2390 ± 120 and 9.9 ± 0.3, respectively. Average fluxes of 84Kr and 132Xe in the bulk solar wind in atoms/(cm2 s) are 0.166 ± 0.009 and 0.017 ± 0.001, respectively. The flux uncertainties also include a 2% uncertainty for the determination of the extracted areas. The bulk solar wind 36Ar/38Ar ratio of 5.50 ± 0.01 and the 36Ar flux of 397 ± 11 atoms/(cm2 s) determined from silicon targets agree well with the 36Ar/38Ar ratio and the 36Ar flux determined earlier on a different type of target by Heber et al. (2009). A comparison of the solar wind noble gas/oxygen abundance ratios with those in the solar photosphere revealed a slight enrichment of Xe and, within uncertainties a roughly uniform depletion of Kr-He in the solar wind, possibly related to the first ionization potentials of the studied elements. Thus, the solar wind elemental abundances He-Kr display within uncertainties roughly photospheric compositions relative to each other. A comparison of the Genesis data with solar wind heavy noble gas data deduced from lunar regolith samples irradiated with solar wind at different times in the past reveals uniform 36Ar/84Kr ratios over the last 1-2 Ga but an increase of the 84Kr/132Xe ratio of about a factor of 2 during the same time span. The reason for this change in the solar wind composition remains unknown. 相似文献
14.
《Geochimica et cosmochimica acta》2001,65(16):2651-2668
The naturally occurring noble gas isotopes (40Ar, 36Ar, 84Kr and 129Xe) and halogens (Cl, Br, I) have been determined simultaneously in irradiated quartz vein samples by noble gas mass spectrometry. Quartz vein samples were collected from the potassic and propylitic alteration zones of six porphyry copper deposits (PCD): Bingham Canyon, Utah; and Silverbell, Ray, Mission, Pinto Valley and Globe-Miami in Arizona. In addition, analyses of 3He/4He have been obtained from sulphide minerals hosted by the quartz veins at Silverbell, Ray, Pinto Valley and Globe-Miami.The majority of PCD fluids studied have Br/Cl and I/Cl ratios that overlap those of fluids included in mantle diamond, suggesting that the salinity had a juvenile origin. The high I/Cl (121 × 10−6 mole, M) in samples from the propylitic zone of Silverbell is attributed to the presence of sedimentary formation water.3He/4He ratios have R/Ra values in the range 0.3 to 1.72, and provide evidence for the involvement of a crustal component in addition to mantle volatiles. 40Ar/36Ar ratios vary from meteoric values of ∼317 in the propylitic zone of Bingham Canyon, and 323 in the skarn alteration of Mission up to 3225 in the potassic zone of Pinto Valley. Fluids in both the potassic and propylitic alteration zones of every deposit are a mixture of a low salinity end-member comprising meteoric water and air, and a high salinity end-member consisting of a mixed mantle and crustal fluid.The 40Ar/Cl ratio of fluid inclusions at Pinto Valley (∼10−4 M) is similar to values obtained previously for mantle fluids. The 40Ar/Cl value is two orders of magnitude lower at Bingham Canyon, where a depleted 36Ar concentration (0.2 × 10−6 cm3/g) below that of air saturated water (ASW), and a range of highly fractionated noble gas compositions (F84Kr = 13 and F129Xe = 160) indicate that boiling and pulsed fluid flow have occurred. 相似文献
15.
Jeffrey P. Severinghaus Alexi Grachev Nicolas Caillon 《Geochimica et cosmochimica acta》2003,67(3):325-343
We describe a method for measuring the 40Ar/36Ar ratio and the 84Kr/36Ar ratio in air from bubbles trapped in ice cores. These ratios can provide constraints on the past thickness of the firn layer at the ice core site and on the magnitude of past rapid temperature variations when combined with measured 15N/14N. Both variables contribute to paleoclimatic studies and ultimately to the understanding of the controls on Earth’s climate. The overall precision of the 40Ar/36Ar method (1 standard error of the mean) is 0.012‰ for a sample analyzed in duplicate, corresponding to ±0.6 m in reconstructed firn thickness. We use conventional dynamic isotope ratio mass spectrometry with minor modifications and special gas handling techniques designed to avoid fractionation. About 100 g of ice is used for a duplicate pair of analyses. An example of the technique applied to the GISP2 ice core yields an estimate of 11 ± 3K of abrupt warming at the end of the last glacial period 15,000 years ago. The krypton/argon ratio can provide a diagnostic of argon leakage out of the bubbles, which may happen (naturally) during bubble close-off or (artifactually) if samples are warmed near the freezing point during core retrieval or storage. Argon leakage may fractionate the remaining 40Ar/36Ar ratio by +0.007‰ per ‰ change in 84Kr/36Ar, introducing a possible bias in reconstructed firn thickness of about +2 m if thermal diffusion is not accounted for or +6 m if thermal diffusion effects are quantified with measured 15N/14N. Reproducibility of 84Kr/36Ar measured in air is about ±0.2‰ (1 standard error of the mean) but is about ±1‰ for ice core samples. Ice core samples are systematically enriched in 84Kr/36Ar relative to atmosphere by ∼5‰, probably reflecting preferential size-dependent exclusion of the smaller argon atom during bubble entrapment. Recent results from the Siple Dome ice core reveal two climate events during the last deglaciation, including an 18-m reduction in firn thickness associated with an abrupt warming at sometime between 18 and 22 kyr BP and a partial or total removal of the firn during an ablation event at 15.3 kyr BP. 相似文献
16.
Rare gas abundances in MORB 总被引：1，自引：0，他引：1
David E. Fisher 《Geochimica et cosmochimica acta》1986,50(12):2531-2541
Data are presented for He, Ar and Xe in a number of MORB glasses and crystalline rocks. The rare gases in the latter group are characterized by atmospheric Ar and Xe, coupled with loss of trapped mantle He, Ar and Xe. The glass data also show clear signs of an atmospheric-like component for Ar and Xe. A reasonably constant world-wide average trapped mantle gas value of 40Ar/36Ar ˜15000 ±3000 is suggested. Anomalies are seen in the 129Xe/132Xe ratio, but at least part of this might be due to mass fractionation rather than to 129I decay. Correlating the data with those from oceanic island basalts in Ar-Xe space indicates that the latter samples are probably also greatly influenced by an atmospheric component rather than (or in addition to) trapping gases from an undepleted mantle source. 相似文献
17.
Argon and halogen geochemistry of hydrothermal fluids in the Loch Ainort granite,Isle of Skye,Scotland 总被引：1，自引：0，他引：1
Highly turbid alkali feldspars from the Loch Ainort granite (59 Ma), Isle of Skye, have been analysed using the 40Ar-39Ar method to obtain chronological and chemical (K, Cl, Br, I) information concerning their origin and hydrothermal alteration. Three methods of gas extraction have been applied to neutron-irradiated samples: laser probe spot fusion of feldspars, in vacuo crushing of a feldspar/quartz separate, and laser stepped heating of the crushed residue. Apparent ages obtained by laser probe spot fusion are mostly similar to the 59 Ma intrusion age. Analyses of relatively pristine regions give some high apparent ages (>59 Ma) indicating the presence of small amounts of 40ArE (excess 40Ar). Crushing releases significant amounts of 40ArE, but is dominated by an 40ArA (atmospheric 40Ar) component. 84Kr/36Ar values obtained by crushing are higher than air and are consistent with air equilibration with fresh water at low temperature 20°C). Therefore, 40ArA was most probably introduced as palaeoatmospheric argon dissolved in the circulating hydrothermal fluids that interacted with the granite, thus supporting a meteoric origin for the fluids. Stepped heating gives a flat age spectrum and an age of 56±4 Ma. Crushing and stepped heating both released significant amounts of halogens with high Br/Cl and I/Cl ratios; excess Xe is also present as indicated by the high 132Xe/36Ar values. It seems likely that the halogen (and possibly Xe) enrichments resulted from interaction of the meteoric fluids with Jurassic sedimentary country rocks. 相似文献
18.
P. Eberhardt J. Geiss H. Graf N. Grögler U. Krähenbühl H. Schwaller A. Stettler 《Geochimica et cosmochimica acta》1974,38(1):97-120
The noble gases He, Ne, Ar, Kr and Xe and also K and Ba were measured in the Apollo 11 igneous rocks 10017 and 10071, and in an ilmenite and two feldspar concentrates separated from rock 10071. Whole rock K/Ar ages of rocks 10017 and 10071 are (2350 ± 60) × 106 yr and (2880 ± 60) × 106 yr, respectively. The two feldspar concentrates of rock 10071 have distinctly higher ages: (3260 ± 60) × 106 yr and (3350 ± 70) × 106 yr. These ages are still 10 per cent lower than the Rb/Sr age obtained by Papanastassiouet al. (1970) and some Ar40 diffusion loss must have occurred even in the relatively coarse-grained feldspar.The relative abundance patterns of spallation Ne, Ar, Kr and Xe are in agreement with the ratios predicted from meteoritic production rates. However, diffusion loss of spallation He3 is evident in the whole rock samples, and even more in the feldspar concentrates. The ilmenite shows little or no diffusion loss. The isotopic composition of spallation Kr and Xe is similar to the one observed in meteorites. Small, systematic differences in the spallation Kr spectra of rocks 10017 and 10071 are due to variations in the irradiation hardness (shielding). The Kr spallation spectra in the mineral concentrates are different from the whole rock spectra and also show individual variations, reflecting the differences in target element composition. The relative abundance of cosmic ray produced Xe131 differs by nearly 50 per cent in the two rocks. The other Xe isotopes show no variations of similar magnitude. The origin of the Xe131 yield variability is discussed.Kr81 was measured in all the samples investigated. The Kr81/Kr exposure ages of rocks 10017 and 10071 are (480 ± 25) × 106 yr and (350 ± 15) × 106 yr, respectively. Exposure ages derived from spallation Ne21, Ar38, Kr83 and Xe126 are essentially in agreement with the Kr81/Kr ages. The age of rock 10071 might be somewhat low because of a possible recent exposure of our sample to solar flare particles. 相似文献