21Ne Production Rates Research Articles

Mineralogy and noble-gas signatures of the carbonate-rich lithology of the Tagish Lake carbonaceous chondrite: evidence for an accretionary breccia

The carbonate-rich lithology of the Tagish Lake carbonaceous chondrite was characterized by noble-gas mass spectrometry, synchrotron X-ray diffraction analysis, and transmission and scanning electron microscopy. Noble-gas analysis was performed on two samples and the results showed that primordial noble gases are abundant and solar noble gases are absent in the samples of carbonate-rich lithology. The concentrations of Ne-A2 and -E in both samples are at the maximum level observed for CI and CM chondrites, suggesting high abundances of presolar diamonds and SiC/graphite, respectively. The cosmic-ray exposure age cannot be determined precisely, because the shielding depth of our Tagish Lake samples is unknown, but the minimum exposure age was determined to be 5.5±0.7 Myr on the basis of cosmogenic 21Ne concentrations and the highest 21Ne production rate. X-ray and electron-microscopic study showed that the carbonate-rich lithology is dominated by loosely packed porous matrix that consists mainly of fine-grained saponite and ferromagenesian carbonate. The matrix contains very few chondrules, but many fine-grained clasts having angular shape with longest dimensions up to 1 mm. The clasts differ from host matrix in both texture and mineralogy. They are massive, compacted material with porosity much lower than matrix and contain abundant magnetite and a coherent intergrowth of serpentine and saponite that is rare in matrix. The presence of texturally and mineralogically distinct clasts indicates that the carbonate-rich lithology is a breccia, but the absence of solar noble gases and impact-induced deformational features in host matrix distinguish it from an asteroid regolith breccia. Our results instead indicate that it is an accretionary breccia formed by simultaneous accretion of diverse objects in a massive dust cloud. The clasts often enclose chondrules and anhydrous silicate fragments such as low-iron-manganese-enriched olivines. This observation and their highly compacted, angular morphology suggests that the clasts derive from earlier-formed chondritic materials which have experienced compression and fragmentation due to mild impacts and from which they were excavated and incorporated into the final rock. It is thus suggested that, in the course of planetesimal formation, agglomeration and disagglomeration of small parent bodies occurred repeatedly in a dense dust cloud where solar wind from the infant sun was shielded. The fine-grained ferromagnesian carbonates must have precipitated from aqueous solutions after the assembly of the Tagish Lake asteroid from recycled materials from previous bodies, because the carbonates coat the surfaces of pores and fill in veins in the clasts.

Exposure history of the St‐Robert (H5) fall

Abstract— The compositionally typical H5 chondrite St‐Robert has an exposure age, 7.8 Ma, indistinguishable from that of the main cluster of H chondrites. Small values of the cosmogenic 22Ne/21Ne ratio in interior samples imply a pre‐atmospheric radius on the order of 40 cm. Sample depths based on tracks and the production rates of Bhattacharya et al. (1973) range from 6 to ∼40 cm and are generally larger than depths estimated from published 60Co activities, perhaps because the track production rates adopted are too high. Depth profiles of the production rates of 14C, 36Cl, 26Al, 10Be, and 21Ne in stony material show increases with depth and reach levels 5% to 15% higher than expected from modeling calculations. The maximum concentrations in St‐Robert are, however, generally comparable to those measured for the L5 chondrite, Knyahinya, whose pre‐atmospheric radius of ∼45 cm is thought to lead to the maximum possible production rates in chondrites. We infer that the pre‐atmospheric radius of St‐Robert was within 5 cm of the value that supports maximum production rates (i.e., 45 ± 5 cm). This radius corresponds to a pre‐atmospheric mass of (1.3 ± 0.4) × 103 kg.The agreement of exposure ages for St‐Robert obtained in several different ways and the similarity of the depth profiles for 14C, 26Al, 10Be, and 21Ne argue against a lengthy pre‐exposure of St‐Robert on the parent body and against a two‐stage exposure after launch from the parent body. Following Morbidelli and Gladman (1998), we suggest that St‐Robert was chipped from deep in its parent body, spent the next 7–8 Ma without undergoing a major collision, was nudged gradually into an orbital resonance with Jupiter, and then traveled quickly to Earth.

Cosmic‐ray prdocution rates of helium, neon and argon isotopes in H chondrites based on chlorine‐36/argon‐36 ages

Abstract— We present the concentrations and isotopic compositions of He, Ne, and Ar for nonmagnetic fractions and bulk samples of 17 H chondrites which were recently investigated for their 36Cl‐36Ar cosmic‐ray exposure ages (Graf et al., 2001). All selected meteorites are observed falls with cosmic‐ray exposure ages close to the 7 Ma peak. The rare gas data are consistent with 10Be and 36C1 production rates in the metal phase. Remarkably, only 1 out of the 17 H chondrites, Bath, shows clear indications for a complex exposure history. Based on rare gas concentrations and 36Cl‐36Ar exposure ages, 21Ne production rates as a function of 22Ne/21 Ne and a mean 38Ar production rate are determined. The results confirm model calculations which predict that the relationship between 21Ne production rates and 22Ne/21Ne is ambiguous for high shielding. Besides the mean 38Ar production rate we also give production rate ratios P(38Ar from Ca)/P(38Ar from Fe). They vary between 10 and 77, showing no significant correlation with 38Ar concentrations or 22Ne/21Ne. By investigating the metal separates, Graf et al. (2001) found significant 3He deficits for 6 out of the 17 meteorites. For the nonmagnetic fractions and bulk samples investigated here, the data points in a 3He/21Ne vs. 22Ne/21Ne diagram plot in the area defined by most of the H chondrites. This means that 3He deficits in the metal phase are much more pronounced than in silicate minerals and we will argue that 3H diffusive losses in meteorites should be the rule rather than the exception. The 21Ne exposure ages, calculated on the basis of modeled 21Ne production rates, confirm the assumption by Graf et al. (2001) that the H5 chondrites with low 3He/38Ar in the metal formed in a separate event than those with normal 3He/38Ar ratios. The data can best be interpreted by assuming that the prominent 7 Ma exposure age peak of the H chondrites is due to at least two events about 7.0 and 7.6 Ma ago.

The 21Ne production rate in quartz revisited

I have revised our earlier production rate determination of 21Ne in terrestrial quartz [S. Niedermann, Th. Graf, J.S. Kim, C.P. Kohl, K. Marti and K. Nishiizumi (1994) Earth Planet. Sci. Lett. 125, 341–355], taking account of improved knowledge about the exposure age of samples used in that work and applying distinct procedures for scaling to sea level and high latitudes. The corrected value of 19.0±3.7 atoms g −1 a −1 is in excellent agreement with expectations based on nuclear properties [J. Masarik and R.C. Reedy (1995) Earth Planet. Sci. Lett. 136, 381–395] and closely corresponds to the present-day production rate. In the case of substantial variations of the geomagnetic field in the past, as proposed by several studies, the revised value can consistently be used with suitable correction methods.

Light noble gases and cosmogenic radionuclides in Estherville, Budulan, and other mesosiderites: Implications for exposure histories and production rates

Abstract— We report measurements of 26AI, 10Be, 41Ca, and 36Cl in the silicate and metal phases of 11 mesosiderites, including several specimens each of Budulan and Estherville, of the brecciated meteorite Bencubbin, and of the iron meteorite Udei Station. Average production rate ratios (atom/atom) for metal phase samples from Estherville and Budulan are 26Al/10Be = 0.77 ± 0.02; 36Cl/10Be = 5.3 ± 0.2. For a larger set of meteorites that includes iron meteorites and other mesosiderites, we find 26Al/10Be = 0.72 ± 0.01 and 36Cl/10Be = 4.5 ± 0.2. The average 41Ca/36Cl production rate ratio is 1.10 ± 0.04 for metal separates from Estherville and four small iron falls. The 41Ca activities in dpm/(kg Ca) of various silicate separates from Budulan and Estherville span nearly a factor of 4, from <400 to >1600, indicating preatmospheric radii of >30 cm. After allowance for composition, the activities of 26Al and 10Be (dpm/kg silicate) are similar to values measured in most ordinary chondrites and appear to depend only weakly on bulk Fe content. Unless shielding effects are larger than suggested by the 36Cl and 41Ca activities of the metal phases, matrix effects are unimportant for 10Be and minor for 26Al.Noble gas concentrations and isotopic abundances are reported for samples of Barea, Emery, Mincy, Morristown, and Marjalahti. New estimates of 36Cl/36Ar exposure ages for the metal phases agree well with published values. Neon‐21 production rates for mesosiderite silicates calculated from these ages and from measured 21Ne contents are consistently higher than predicted for L chondrites despite the fact that the mesosiderite silicates have lower Mg contents than L chondrites. We suggest that the elevation of the 21Ne production rate in mesosiderite silicates reflects a “matrix effect,” that is, the influence of the higher Fe content of mesosiderites, which acts to enhance the flux of low‐energy secondary particles and hence the 21Ne production from Mg. As 10Be production is relatively insensitive to this matrix effect, 10Be/21Ne ages give erroneously low production rates and high exposure ages. By coincidence, standard 22Ne/21Ne based “shielding” corrections give fairly reliable 21Ne production rates in the mesosiderite silicates.

Evidence for common breakup events of the acapulcoites‐lodranites and chondrites

Abstract— Acapulcoites and lodranites are believed to originate on a common parent body and to represent some of the earliest events in the differentiation of the chondritic asteroids. We have conducted isotopic studies of the noble gases He, Ne, Ar, Kr, and Xe, and determinations of the concentrations of the major elements and of the radionuclides 10Be, 26Al, and 36Cl in an attempt to constrain the cosmic‐ray exposure history of two members of the acapulcoite‐lodranite clan recovered in Antarctica: Frontier Mountain (FRO) 95029 and Graves Nunataks (GRA) 95209. From cosmic‐ray‐produced 3He, 21Ne, and 38Ar and appropriate production rates, we derive parent‐body breakup times of 4.59 ± 0.60 and 6.82 ± 0.60 Ma for FOR 95029 and GRA 95209, respectively. These times are consistent with those obtained from the pairs 10Be‐21Ne and 26Al‐21Ne; whereas the times inferred from the pair 36Cl‐36Ar are slightly longer, perhaps because the 36Cl activities decreased as a result of decay on Earth. Terrestrial ages up to ∼50 ka for the two meteorites are consistent with the measured 36Cl activities of the metal phases. All acapulcoites and lodranites dated until now show cosmic‐ray exposure ages in the range of 4–10 Ma. This is the same range as that found for the major exposure age cluster of the H chondrites. As a common parent body is improbable on the basis of the O‐isotopic systematics, a common set of impactors might have affected the asteroid belt 4–10 Ma ago.

Cosmogenic noble gas studies in the oldest landscape on earth: surface exposure ages of the Dry Valleys, Antarctica

Extraordinarily high surface exposure ages have been determined for Sirius Group tillites of Mt. Fleming and Mt. Feather as well as at localities in the Inner Dry Valleys using cosmogenic helium and neon. Ages of 10 Ma at Mt. Fleming, 5.3 Ma at Mt. Feather and 6.5 Ma at Insel Mountain are among the highest nominal exposure ages published so far. These values are minimal ages as they are based on the assumption of zero erosion and uplift. The Mt. Feather sample independently confirms the pre-Pliocene age of the Sirius Group sediments in the Dry Valleys as previously determined at Mt. Fleming. The Insel Mountain samples provide evidence for a landscape formation of the Inner Dry Valleys not later than Late Miocene time. Assuming conservatively low values of 2.5 cm Ma −1 for erosion rate and 50 m Ma −1 for uplift rate we infer that the Sirius Group tillites at Mt. Fleming were deposited earlier than 20 Ma ago. This indicates that the overriding of the Dry Valleys block of the Transantarctic Mountains by the East Antarctic Ice Sheet occurred not later than the Early Miocene. Maximum long-term erosion rates in the Inner Dry Valleys must be <15 cm Ma −1 down to altitudes <1000 m. Since such low erosion rates require permanently cold and hyperarid conditions, the response of Antarctica to the Pliocene warm climatic episode must have been small. Cosmogenic nuclide data from both the Inner Dry Valleys and the Sirius Group sediment localities support the hypothesis of a stable East Antarctic Ice Sheet since at least Late Miocene time, implying that the climate of Antarctica was decoupled from that of lower southern latitudes. We present also new elemental 21Ne production rates of P 21(Mg) = 196 atoms g −1 yr −1 and P 21(Al) = 55 atoms g −1 yr −1 at sea level and high geomagnetic latitude. These figures are consistent with a 3He production rate of P 3 = 110 atoms g −1 yr −1, similar to previously published values. This consistency provides evidence that pyroxene is retentive for both helium and neon over at least 10 Ma. Cosmogenic Ne in quartz and pyroxene has a ( 22Ne/ 21Ne) cos ratio of 1.266 ± 0.040 and 1.159 ± 0.040, respectively.

Cosmic‐ray exposure ages of diogenites and the recent collisional history of the howardite, eucrite and diogenite parent body/bodies

Abstract— We determined the cosmic‐ray exposure age of 20 diogenites from measured cosmogenic noble gas isotopes and calculated production rates of 3He, 21Ne and 38Ar. The production rates were calculated on the basis of the measured chemical composition and the cosmogenic 22Ne/21Ne ratio of each sample. The shielding conditions of each sample were also checked on the basis of the measured 10Be and 26AI concentrations. The exposure ages range from 6 to 50 Ma but do not form a continuous distribution: ten ages cluster at 21–25 Ma and four at 35–42 Ma. The two diogenite clusters coincide with the 22 Ma and 38 Ma peaks in the exposure age distribution of eucrites and howardites. After the selection from literature data of 32 eucrites and 11 howardites with reliable ages, we find a total of 23 howardite, eucrite and diogenite (HED) group meteorites at 20–25 Ma and 10 at 35–42 Ma. The shape of the two peaks is consistent with single impact events, and random number statistics show that they are statistically significant at the 99% level. Altogether, this provides strong evidence for two major impact events 22 Ma and 39 Ma ago. Although these two events can explain more than half of all HED exposure ages, it takes at least five impact events to explain all ages &lt;50 Ma. An impact frequency of one per 10 Ma corresponds to projectiles of at least 2–4 km in diameter for Vesta and of 60–300 m for the 100× smaller Vesta‐derived “vestoids.” Based on the HED exposure‐age distribution, the size distribution of the main‐belt asteroids and the difference in size between Vesta and the kilometer size vestoids, we favor Vesta as the major source of HED meteorites, although some of the meteorites may have been ejected from the vestoids rather than directly from Vesta.

Complex exposure histories for meteorites with “short” exposure ages

Abstract— We report measurements of 26Al and 10Be activities in nine ordinary chondrites and of the light noble gas concentrations and 36Cl and 41Ca activities in subsets of those meteorites. All but Murray have low 21Ne concentrations (&lt;1.0 × 10−8cm3STP/g) and have previously been used to estimate 21Ne production rates. Ladder Creek, Murchison, Sena, and Timochin have inventories of cosmogenic radionuclides that are compatible with a single stage of irradiation and give 21Ne production rates that are consistent with the standard L‐chondrite value of 0.33 × 10−8cm3STP/g/Ma. In contrast, Cullison, Guenie, Shaw, and Tsarev experienced complex irradiation histories. They and several other meteorites with low nominal exposure ages also have lower 3He/21Ne ratios than expected based on their 22Ne/21Ne ratios. A general association between low 21Ne contents and 3He losses suggests that meteorites with short lifetimes often occupy orbits with small perihelia. However, meteorites with low 21Ne contents, one‐stage exposure histories, and losses of cosmogenic 3He are rare. Possible explanations for the scarcity are (1) statistical, (2) that it is harder for more deeply buried protometeoroids to lose gas in a liberating collision, and (3) that it is harder to insert more deeply buried protometeoroids directly into orbits with small perihelia.

History of lunar meteorites Queen Alexandra Range 93069, Asuka 881757, and Yamato 793169 based on noble gas isotopic abundances, radionuclide concentrations, and chemical composition

Abstract— We investigated the characteristics and history of lunar meteorites Queen Alexandra Range 93069, Yamato 793169 and Asuka 881757 based on the abundances of all stable noble gas isotopes, the concentrations of the radionuclides 10Be, 26Al, 36Cl, and 81Kr, and the abundances of Mg, Al, K, Ca, Fe, Cl, Sr, Y, Zr, Ba, and La. Based on the solar wind and cosmic‐ray irradiations, QUE 93069 is the most mature lunar meteorite studied up to now. The 40Ar/36Ar ratio of the trapped component is 1.87 ± 0.16. This ratio corresponds to a time when the material was exposed to solar and lunar atmospheric volatiles ∼400 Ma ago. On the other hand, Yamato 793169 and Asuka 881757 contain very little or no solar noble gases, which indicates that these materials resided in the top layer of the lunar regolith only briefly or not at all. For all lunar meteorites, we observe a positive correlation of the concentrations of cosmic‐ray produced with trapped solar noble gases. The duration of lunar regolith residence for the lunar meteorites was calculated based on cosmic‐ray produced 21Ne, 38Ar, 78Kr, 83Kr, and 126Xe and appropriate production rates that were derived based on the target element abundances and the shielding indicator 131Xe/126Xe. For QUE 93069, Yamato 793169, and Asuka 881757, we obtained 1000 ± 400 Ma, 50 ± 10 Ma, and &lt;1 Ma, respectively. Both Asuka 881757 and Yamato 793169 show losses of radiogenic 4He from U and Th decay and Yamato 793169 also 40Ar loss from K‐decay. For Asuka 881757, we calculate a K‐Ar gas retention age of 3100 ± 600 Ma and a 244Pu‐136Xe fission age of 4240 ± 170 Ma. This age is one of the oldest formation ages ever observed for a lunar basalt. The exposure history of QUE 93069 after ejection from the Moon was derived from the radionuclide concentrations: ejection 0.16 ± 0.03 Ma ago, duration of Moon‐Earth transit 0.15 ± 0.02 Ma and fall on Earth &lt;0.015 Ma ago. This ejection event is distinguished temporally from those which produced the other lunar meteorites. We conclude that six to eight events are necessary to eject all the known lunar meteorites.

Placental norepinephrine clearance: in vivo measurement and physiological role

The intrauterine clearance rate of catecholamines is higher than in newborn animals or in adults. The separate contributions of the fetus and placenta to this clearance are not known. The placenta is a site of expression of the amine plasma membrane transporters that mediate this process. To determine the physiological role of this placental transporter in vivo, we studied fetal sheep at 123 days with common umbilical vein (UV), fetal arterial (AO), and venous catheters. Tritiated norepinephrine ([3H]NE) was infused to determine the kinetics of placental and fetal NE appearance and clearance rates. Umbilical flow was determined by [3H]NE infusion. Placental and total (fetal-placental) NE clearance rates were determined by measurement of [3H]NE from simultaneously drawn UV and AO samples. Total clearance was 99 +/- 8 ml.kg-1.min-1. Placental fractional [3H]NE extraction was 21% and accounted for 48% of total clearance. Fetal plasma NE production rate was 85 +/- 20 ng.kg-1.min-1. We conclude that placental catecholamine clearance is an important metabolic function of the placenta. This mechanism for clearance of the high fetal production rate of catecholamines is vital for fetal homeostasis. We speculate that derangements in placental catecholamine clearance may explain the exaggerated adverse effects on the fetus of drugs like cocaine, which block catecholamine transport.

Cosmic-ray-produced 21Ne in terrestrial quartz: the neon inventory of Sierra Nevada quartz separates

The study of cosmic-ray-produced radioactive and stable nuclides on the surface of the Earth can provide relevant geomorphological and glaciological information. At present, the cosmic ray production rates of stable 21Ne are not well known. This study attempts to remedy the situation by determining the production rate ratio of 21Ne and 26Al, P 21 P 26 , in quartz. 26Al concentrations and P 26 rates have previously been investigated for quartz separates of Sierra Nevada rocks which were brought to the surface by glacial scouring during the Tioga period at the end of the last ice age [1]. We used splits of the same samples for our studies and found that Ne in these rocks represents a mixture of several components: trapped Ne, nucleogenic 21Ne and 22Ne produced by (α,n) reactions in oxygen and fluorine, respectively, as well as cosmic-ray-produced Ne, which is the component of interest in this study. The trapped component was substantially lost in one sample (W86-12) by crushing and by a density separation of the grain sizes 38–90 μm and 90–125 μm, permitting the resolution of the in situ produced 21Ne into cosmic-ray spallation and (α,n) produced components and the determination of a lower limit to P 21 P 26 . In a second sample (W86-8) one split contained small enough amounts of nucleogenic 21Ne to permit the determination of a reasonable upper limit to P 21 P 26 . The two ratio determinations are consistent within error limits and the value adopted, 0.65 ± 0.11 (2σ), agrees with ratios observed in extraterrestrial matter. Apparently, P 21 P 26 is thus not very sensitive to the neutron spectrum. However, the observed production rate ratio is substantially larger than theoretical estimates for Si targets, reflecting poorly known neutron excitation functions. The above P 21 P 26 value, coupled to the observed 26Al production rate [1], corresponds to a 21Ne production rate of P 21 = 21 atoms g −1 a −1 in quartz or to P 21 = 45 atoms (g Si) −1 a −1 (at sea level and high latitudes). This rate is based on an adopted exposure age of 11,000 yr for our quartz samples.

On the Bur Gheluai H5 chondrite and other meteorites with complex exposure histories

Abstract— We present the 14C, 26Al, 10Be, 3He, 4He, 20Ne, 21Ne, 22Ne, 36Ar, 38Ar, and 40Ar concentrations and the track densities measured in up to 13 samples of the Bur Gheluai (H5) meteorite fall. Only a multi‐stage exposure history can explain the data in a self‐consistent way. Parameters for a model two‐stage history obtained by simultaneous, least‐squares fitting of the concentrations of 14C, 26Al, 10Be, and 21Ne were: first stage duration ∼10 Ma and radius &gt;2 m; second stage duration ∼0.6 Ma and radius 40–100 cm.Nominal one‐stage 21Ne production rates (P21) inferred from 26Al in Bur Gheluai samples exceed those inferred from 10Be as expected for a meteorite with a complex history. Nonetheless, data for other meteorites indicate that multi‐stage irradiations alone do not account for all the high reported values of P21 based on 26A***l: The equations describing the production of cosmogenic nuclides show that uncorrected shielding effects may also play a role.A compilation of ordinary, solar‐gas‐poor chondrites for which two‐stage histories have been proposed includes many with short second stages but none with unambiguously long first stages (&gt;0.2 Ga).

On the production of cosmogenic nuclides in meteoroids by galactic protons

Abstract— A purely physical model is presented describing the depth‐ and size‐dependence of the production of cosmogenic nuclides in meteoroids with radii up to 85 cm and in planetary surfaces by galactic cosmic ray protons. The model is based on Monte Carlo calculations of the intra‐ and internuclear cascades, by which depth‐ and size‐dependent spectra of primary and secondary protons and of secondary neutrons are derived, and on experimental and theoretical thin‐target cross sections of the underlying nuclear reactions. Model calculations are presented for production rates of 53Mn, 26Al, 22Ne, and 21Ne in H‐ and L‐chondrites and of 53Mn and 26Al in lunar surface material and compared with experimental data. From the analysis of 53Mn and 26Al in the Apollo 15 lunar drill core and in the L‐chondrite Knyahinya GCR p‐spectra and integral particle fluxes at 1 A.U. and in the meteoroid orbits averaged over the last 10 Ma are derived. An analysis of experimental depth profiles in four H‐ and L‐chondrites demonstrates, that the new model is well capable of describing depth‐ and size‐dependences of production rates of cosmogenic nuclides. Moreover, it is possible to determine exposure ages for these meteorites on the basis of the theoretical 21Ne production rates. The model calculations further explain the depth‐ and size‐dependence of 22Ne/21Ne‐ratios and the dependences on these ratios of 21Ne, 26Al and 53Mn production rates. The future requirements for model calculations of cosmogenic nuclide production rates in extraterrestrial matter are outlined.

Investigations of cosmic-ray-produced nuclides in iron meteorites, 6. The Signer-Nier model and the history of the cosmic radiation

About thirty years ago, a simple model was proposed by Martin and by Ebert and Wänke to describe the interaction of cosmic rays with meteoritic iron. The model was later used by Signer and Nier to calculate the spatial distribution of cosmogenic noble gas nuclides in spherical meteoroids. A rigorous mathematical evaluation of the model—known as the Signer-Nier model—is presented. The model is broadly compatible with data on noble gas nuclides and on 41K/ 40K exposure ages: (1)|In the framework of the model, the abundance ratio of any two of the cosmogenic nuclides 3He, 4He, 21Ne, and 38Ar is correlated with the ratio of any other pair of these nuclides. These ratios depend only on the effective irradiation hardness in the sample. Analysis of these nuclides in a single sample does not permit determination of radiation dosage, of size of the meteoroid, and of location of the sample within the meteoroid. The model-derived correlations agree with the corresponding experimental correlations except for samples from relatively large depths. (2)|The model makes it possible to derive a P 21- 4He 21Ne diagram predicting how 21Ne production rate P 21 and 4He/ 21Ne ratio depend on meteoroid size and sample depth. Possible combinations of values for P 21 and 4He/ 21Ne are restricted, they define the “allowed field” of the diagram. Each location in this field is associated with a distinct combination of values for meteoroid size and sample depth. The diagram is a tool to determine model-dependent values for sizes and depths. Values of P 21 and 4He/ 21Ne from previous noble gas analyses and from 41K/ 40K age determinations fall into or close to the allowed field. The model represents, therefore, a reasonable description of the cosmic ray interaction with iron meteoroids. Analysis of age-, size-, and depth-distributions indicates that space erosion was probably effective with a rate of the order of 1 cm per 100 Ma. An investigation of the compatibility of noble gas, potassium, and radionuclide data reveals the following: (1) the traditional age scale of the 41K/ 40K method is correct; (2) the intensity of the cosmic radiation was essentially constant in the course of the last 1–2 Ga; (3) the intensity exceeded its long-term average by 50% during the last few million years.

Helium and neon isotope geochemistry of some ground waters from the Canadian Precambrian Shield

Ground waters in a Precambrian granitic batholith at the Whiteshell Nuclear Research Establishment (WNRE) in Pinawa, Manitoba contain between 5 × 10 −5 and 10 −1 cc STP/g H 2O of radiogenic helium-4 but have relatively uniform 3He/ 4He ratios of between 0.6 × 10 −8 and 2.3 × 10 3. The highest helium samples also contain radiogenic 21,22Ne produced by (α, n) or ( n,α) reactions with other isotopes. As much as 1.8 × 10 −9 cc STP/ g H 2 O of excess 21Ne and 3.8 × 10 −9 cc STP/ gH 2 O of excess 22Ne have been measured. Helium and 21Ne ages of these ground waters, calculated on the basis of known crustal production rates of 4He and 21Ne, are unreasonably high (up to 2 × 10 5 years) and incompatible with the 14C ages and other isotopic and hydrogeologic data. Uranium enrichment in the flow porosity of the granite may dominate 4He and 21,22Ne production in this granite and mask the contributions from more typical U and Th concentrations in the rock matrix. At the Chalk River Nuclear Laboratories in Ontario helium concentrations in ground waters in a Precambrian monzonitic gneiss range from 1.5 × 10 −7 to 8.7 × 10 −4 cc STP/ g H 2 O with the 3He/ 4He ratios ranging from 2.0 × 10 −3 to 1.5 × 10 −7. The highest helium concentrations may be attributable to the presence of a thick uraniferous pegmatite vein and yield helium ages more than two orders of magnitude higher than the 14C ages. Application of He age dating equations to ground waters from Precambrian granitic rocks requires knowledge of the nature of uranium and thorium enrichment in the subsurface in order to select appropriate values for porosity and uranium and thorium concentration in the rock.

Half‐life of 26Al

The half‐life of 26Al has been redetermined because of suggestions of an error in the accepted value based on its use in calculating 21Ne production rates from cosmic rays in meteorites. Two solutions of 26Al were analyzed for the specific radioactivity and mass spectrometric determination of the 26Al concentration. The half‐life obtained for 26Al was 7.05×105 years ±3.4%. This is identical to the accepted value of 7.16×105 years and indicates that problems with the 21Ne production rate is not due to an erroneous half‐life.

The 21Ne production rate in stony meteorites estimated from 10Be and other radionuclides

The 10Be contents of 28 stony meteorites with known 21Ne contents range from 0.97 to 23 dpm/kg and give an average 21Ne production rate ( P 21) of (0.28 ± 0.02) × 10 8 cm 3 STP/g-Myr for shielding conditions corresponding to 22Ne 21Ne = 1.114 in an H-chondrite. Our P 21( 10Be) agrees with others' P 21 based on 22Na, 81Kr and 53Mn but not on 26A1. Temporal variations in the cosmic ray flux do not explain the disagreement satisfactorily; major errors in the radionuclide half-lives are not indicated. The discrepancy seems rooted in the data selection and the difficulties of making accurate corrections for shielding, chemical composition and other sources of variability.

Cosmic-ray constancy and cosmogenic production rates in short-lived chondrites

Five chondrites with short cosmic ray exposure ages (< 3Myr) have been analyzed for 53Mn ( t 1.2 = 3.7Myr), 26Al( t 1.2 = 0.72Myr) and the stable isotopes of He, Ar, and in particular, Ne. In addition, rare gases were determined for five other short-lived chondrites from the same aliquots which had previously been used for 26Al and 53Mn determinations by the Cologne Laboratory. Improved curves of growth were constructed for 26Al and 53Mn to deduce the respective saturation values 26Al 0 and 53Mn 0 and to obtain 21Ne production rates ( 21 P). 26Al and 53Mn saturation values deduced from short-lived chondrites alone agree within 20%, with those deduced from all chondrites. Values of 21 p based on 53Mn and 26Al are 0.30 ± 0.03 and 0.46 ± 0.05, respectively, in H chondrites. Possible causes for the difference include half-life errors, data selection and a recent (≲2.5Myr) increase in the cosmic ray intensity.

Investigations on cosmic-ray-produced nuclides in iron meteorites, 3. Exposure ages, meteoroid sizes and sample depths determined by mass spectrometric analyses of potassium and rare gases

Three physical quantities define the essentials of the cosmic ray exposure history of a sample of an iron meteorite: (1) the cosmic ray exposure age T, (2) the pre-atmospheric “size” S of the irradiated body, and (3) the location, i.e. the “depth” D, of the samples within the body. To establish these quantities for a given sample three independent quantities must be determined experimentally. In the present work T is ascertained by the 41K/ 40K method and the 4He and 21Ne concentrations ( C 4 and C 21) are measured by the isotope dilution method. Signer and Nier's evaluation of the rare gas distribution in the meteorite Grant and the measured exposure age for this meteorite provide the relationships allowing to ascertain for any meteorite the quantities S and D from the 21Ne production rate ( P 21 = C 21/ T) and the 4He/ 21Ne ratio. Earlier measurements have provided data on the isotopic composition of potassium in 74 different iron meteorites. New rare gas measurements are reported for some 40 samples. Results on the age, size and depth are obtained for almost 60 samples. These data suggest that Signer and Nier's model is well suited for describing not only the rare gas distribution in a single selected meteorite (Grant) but also the exposure histories of the great majority of all irons. For a few samples, however, secondary breakups of the meteoroid and a two- or multiple-stage irradiation must be invoked. Further measurements are proposed for testing and, possibly, refining the still somewhat uncertain relationships between the abundances of cosmogenic nuclides and the quantities T, S, and D in very large meteorites. Histograms are presented showing the age distributions for irons of different chemical groups and of different size ranges. The feasibility and the relative merits of other methods for the determination of T, S, and D are discussed.