GERM Reservoir Database
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GERM Database Search Results        
Reservoir Z Element Value Median SD Low High N Unit Info Reference Source(s)
ALH 77005 Meteorite 49 In 11           ppb Mars elemental abundances as given by ALH77005 meteorite, which is a lherzolitic shergottite, as given in Lodders 1988. McSween, Jr. 2004 Lodders 1998
Angra dos Reis Angrite 49 In 1.43           ppb Elemental abundance of the Angra dos Reis meteorite.  Classified as an Angrite, the sample itself consists of a thin slice of material most likely made with a cutoff wheel.  However, the high abundance of Cu in the sample indicates that the sample was contaminated from the wheel used to make the slice of material. Laul et al. 1972
Bereba Eucrite 49 In 0.94           ppb Elemental abundance of the B¿r¿ba meteorite.  Sample consisted of one or several chips between 500-300 mg, and no cleaning was attempted before irradiation.1 Laul et al. 1972
Bialystok Howardite 49 In 2.73           ppb Elemental abundance of the Bialystok meteorite.  Classified as a Howardite, the sample itself consists of one or several chips between 500-300 mg. No cleaning was attempted before irradiation. Laul et al. 1972
Chassigny Achondrite 49 In 3.9           ppb Trace element abundances of the Chassigny meteorite given by Treiman et al. 1986.  These values along with those of the C1 Chondrites are used mainly for comparison and normalization of values taken from other sources pertaining to Urelites.  Janssens et al. 1987 Treiman et al. 1986
Chassigny Meteorite 49 In 3.9           ppb Mars elemental abundances as given by Chassigny meteorite (chassignite) as given in Lodders 1988. McSween, Jr. 2004 Lodders 1998
CI Chondrites 49 In 0.8   0.04         CI Meteorite derived solar system abundances of various elements. Palme & Jones 2004
CI Chondrites 49 In 80           ppb C1 Chondrite trace element abundances as found by Anders and Ebihara 1982.  All Urelite values given by other sources are normalized to these values simply to put the data on a common scale. Janssens et al. 1987 Anders & Ebihara 1982
CI Chondrites 49 In 0.078   0.0078       ppm Abundance of elements in the solar system based off of Palme & Beer 1993 study of CI meteorites. Palme & Jones 2004 Palme & Beer 1993
CI Chondrites 49 In 0.08           ppm Abundance of elements in the solar system from Anders & Grevesse 1989 study of CI meteorites. Palme & Jones 2004 Anders & Grevesse 1989
CI Chondrites 49 In 80           ppb C1 Carbonaceous chondrite major and minor element compositions as given in Wasson & Kallemeyn 1988. These values are given in an effort to accurately represent the C1 chondrites as based on an array of sources and derive a revised model for the composition of the Earth. McDonough & Sun 1995 Wasson & Kallemeyn 1988
CI Chondrites 49 In 80           ppb Based on measurements on 3 out of 5 carbonaceous chrondrites namely Orgueil, Ivuna and Alais. McDonough & Sun 1995
CI Chondrites 49 In 80   5.1     24 ppb Mean C1 chondrite from atomic abundances based on C = 3.788E-3*H*A where C = concentration; H = atomic abundance and A = atomic weight. Values are not normalised to 100% Anders & Grevesse 1989
CI Chondrites 49 In 78   7.8       ppb Composition of the Primitive Mantle of the Earth as based on CI Chondritic major and trace element compositions from Chapter 1.03 Palme & Jones 2004 Treatise of Geochemistry. Palme & O'Neill 2004 Palme & Jones 2004
CI Chondrites 49 In 80           ppb C1 Carbonaceous chondrite major and minor element compositions as given in Palme 1988. These values are given in an effort to accurately represent the C1 chondrites as based on an array of sources and derive a revised model for the composition of the Earth. McDonough & Sun 1995 Palme 1988
Constantinople Eucrite 49 In 1.82           ppb Elemental abundance of the Constantinople meteorite.  Classified as a eucrite the sample consisted of one or several chips between 500-300 mg, and no cleaning was attempted before irradiation. Laul et al. 1972
Continental Crust 49 In 0.05           µg/g Rudnick & Gao 2004
Continental Crust 49 In 50           ppb UCC; LCC = calculated from rock averages compiled by Linn & Schmitt (1972) and contributed by Voland (1969) in the proportions of Figure 2. Wedepohl 1995
Continental Crust 49 In 50           ppb Taylor & McLennan 1995
Continental Crust 49 In 0.05           µg/g Major and trace element compositional estimates of the Bulk Continental Crust given by Taylor and McLennan 1985 & 1995. Major element oxides are given in wt.% and trace elements in either ng/g or ¿g/g. Rudnick & Gao 2004 Taylor & McLennan 1985
Taylor & McLennan 1995
Continental Crust 49 In 0.1           µg/g Major and trace element compositional estimates of the Bulk Continental Crust given by Taylor 1964. Major element oxides are given in wt.% and trace elements in either ng/g or ¿g/g. Rudnick & Gao 2004 Taylor 1964
Continental Crust 49 In 0.05           µg/g Major and trace element compositional estimates of the Bulk Continental Crust given by Wedepohl 1995. Major element oxides are given in wt.% and trace elements in either ng/g or ¿g/g. Rudnick & Gao 2004 Wedepohl 1995
Continental Crust 49 In 0.052           µg/g Recommended composition of the Bulk Continental Crust where the total-crust composition is calculated according to the upper, middle and lower-crust compositions obtained in this study and corresponding weighing factors of 0.317, 0.296 and 0.388. The weighing factors are based on the layer thickness of the global continental crust, recalculated from crustal structure and areal proportion of various tectonic units given by Rudnick and Fountain 1995. Rudnick & Gao 2004 Rudnick & Fountain 1995
Continental Crust 49 In 50           ppb Enrichment of elements in the bulk continental crust given by Rudnick & Gao from Chapter 3.1 of the Treatise on Geochemistry 2004. Palme & O'Neill 2004 Rudnick & Gao 2004
Core 49 In 0           µg/g Compostioinal models for the bulk Earth, core and silicate Earth are modified after McDonough & Sun (1995). McDonough 1998
Depleted Mantle 49 In 12.2   3.05       ppb Estimate for the concentrations in the Depleted Mantle of most of the elements of the Periodic Table.  In/Y is the element ratio/constraint used to make this estimate. Salters & Stracke 2004
Dyalpur Ureilite 49 In 0.4           ppb Trace element values for the Dyalpur meteorite as given in Higuchi et al. 1976.  Mainly used in this study as comparisons to the Kenna and Havero meteorites.  Janssens et al. 1987 Higuchi et al. 1976
Frankfort Howardite 49 In 2.35           ppb Elemental abundance of the Frankfort meteorite.  Classified as a Howardite, the sample itself consists of one or several chips between 500-300 mg. No cleaning was attempted before irradiation. Laul et al. 1972
Goalpara Ureilite 49 In 1.01           ppb Trace element abundances of the Goalpara meteorite first reported by Higuchi et al. 1976.  These trace element values are given in an effort to resolve a disagreement about Ir and W values being associated with veins or bulk rock. These values are compared to other vein and bulk rock values obtained via other meteorites analyzed in this study. Janssens et al. 1987 Higuchi et al. 1976
Havero Ureilite 49 In 0.72           ppb Trace element abundances of the Havero (bulk) meteorite first reported by Higuchi et al. 1976.  These trace element values are given in an effort to resolve a disagreement about Ir and W values being associated with veins or bulk rock. These values are compared to other vein and bulk rock values obtained via other meteorites analyzed in this study. Janssens et al. 1987 Higuchi et al. 1976
Havero Ureilite Vein Metal 49 In 11.5           ppb Trace element abundances of the Havero Vein sample B18-2 analyzed here by Janssens et al. 1987.  According to analysis of the siderophile elements of Havero, this sample is highly enriched in vein material as indicated by noble gas and this trace element data.  .. Janssens et al. 1987
Jonzac Eucrite 49 In 1.23           ppb Elemental abundance of the Jonzac meteorite.  Classified as a eucrite the sample consisted of one or several chips between 500-300 mg, and no cleaning was attempted before irradiation. Laul et al. 1972
Juvinas Eucrite 49 In 1.61           ppb Elemental abundance of the Juvinas meteorite.  Classified as a eucrite the sample consisted of one or several chips between 500-300 mg, and no cleaning was attempted before irradiation. Laul et al. 1972
Kapoeta Howardite 49 In 3.13           ppb Elemental abundance of the Kapoeta meteorite.  Classified as a Howardite, the sample itself consists of dark material from the gas-rich, brecciated meteorite were obtained by Dr. Brian Mason (U.S. National Museum). Laul et al. 1972
Kapoeta Howardite 49 In 1.67           ppb Elemental abundance of the Kapoeta meteorite.  Classified as a Howardite, the sample itself consists of light material from the gas-rich, brecciated meteorite were obtained by Dr. Brian Mason (U.S. National Museum). Laul et al. 1972
Kenna Ureilite 49 In 2.1         1 ppb Abundances of the trace elements found in the Kenna Meteorite taken from sample H159.23 from the American Meteorite Laboratory.  This bulk urelite sample is the richest in siderophile elements. Janssens et al. 1987
Kenna Ureilite Vein Metal 49 In 1.9           ppb Trace element abundances of the Kenna Vein material which in fact was a hand picked separate of only 33mg.  According to this analysis of the siderophile elements it is only slightly enriched in vein material.  Janssens et al. 1987
Lafayette Nakhlite 49 In 20.3           ppb Elemental abundance of the Lafayette meteorite.  Classified as a Nakhlite, the sample itself consists of material from one or several chips between 500 and 300 mg. No cleaning was attempted prior to irradiation. Laul et al. 1972
Lower Continental Crust 49 In 50           ppb Taylor & McLennan 1995
Lower Continental Crust 49 In 0.05           µg/g Recommended composition of the Lower Continental crust as given by various sources. Major element oxides are given in wt.% and trace element concentrations are given in either ng/g or ¿g/g. Rudnick & Gao 2004 Wedepohl 1995
Lower Continental Crust 49 In 0.052           ppm LCC = calculated from rock averages of Heinrichs et al. (1980) in the proportions of Figure 2. Wedepohl 1995
Lower Continental Crust 49 In 0.05           µg/g Major and trace element compositional estimates of the lower continental crust as given by Taylor and McLennan 1985, 1995 using average lower crustal abundances. Major element oxides are given in wt.% and trace elements in either ng/g or ¿g/g. Rudnick & Gao 2004 Taylor & McLennan 1985
Taylor & McLennan 1995
Lower Continental Crust 49 In 0.052           µg/g Major and trace element compositional estimates of the lower continental crust as given by Wedepohl 1995 using lower crust in Western Europe derived from siesmic data and granulite xenolith composition. Major element oxides are given in wt.% and trace elements in either ng/g or ¿g/g. Rudnick & Gao 2004 Wedepohl 1995
Manganese Nodules 49 In 0.25           ppm Average concentrations of various elements found in deep sea Manganese nodules.  Sea salt components are subtracted assuming all chloride is of seawater origin. Li 1991 Baturin 1988
Marine Pelagic Clay 49 In 0.08           ppm Average concentrations for various elements enriched in Oceanic Pelagic Clays.  Compared to the element values of Shales, the Pelagic Clays are relatively similar with few exceptions.   All sea salt components are subtracted from the sample analysis assuming all chloride is of seawater origin. Li 1991 Turekian & Wedepohl 1961
Marine Pelagic Clay 49 In 0.08           ppm Average concentrations of elements in oceanic pelagic clays.  The elemental values found in the Pelagic clays give good indications on river input of elements to the oceans.  From river sources to mid oceanic ridge sinks this is also a good indicator of atmospheric conditions for varying periods of world history.   Li 1982
Marine Shales 49 In 0.1           ppm Average concentrations of various elements in shales, note that the values are within a factor of two or better as compared to Oceanic Pelagic Clays with a few exceptions.  The exceptions, as far as this reference is concerned, are not critical and any conclusions drawn are applicable to both Oceanic Pelagic Clays and Shales.  Li 1991 Turekian & Wedepohl 1961
Molteno Howardite 49 In 7.63           ppb Elemental abundance of the Molteno meteorite.  Classified as a Howardite, the sample itself consists of light material from one or several chips between 500 and 300 mg. No cleaning was attempted prior to irradiation. Laul et al. 1972
Nakhla Meteorite 49 In 20   7       ppb Mars elemental abundances as given by Nakhla meteorite (nakhlite) as given in Lodders 1988. McSween, Jr. 2004 Lodders 1998
Nakhla Nakhlite 49 In 24.4           ppb Elemental abundance of the Nakhla meteorite.  Classified as a Nakhlite, the sample itself consists of material from one or several chips between 500 and 300 mg. No cleaning was attempted prior to irradiation. Laul et al. 1972
Novo-Urei Ureilite 49 In 1           ppb Trace element abundances of the Novo Urei meteorite originally given by Higuchi et al. 1976. Novo Urei happens to be the second in line as far as richest in siderophile element abundances, second only to Kenna Meteorite.  Janssens et al. 1987 Higuchi et al. 1976
Oceans Deep water 49 In 0.1           ng/kg Deep ocean water is ~1,000 m depth. Where possible data is from the Pacific ocean that shows the greates variations; otherwhise data is from the Atlantic ocean. Depth = 1000 m. Quinby-Hunt & Turekian 1983 Matthews & Riley 1970
Oceans Surface water 49 In 0.3           ng/kg Surface or near-surface concentratio. Where possible data is from the Pacific ocean that shows the greates variations; otherwhise data is from the Atlantic ocean. Depth = 2 m. Quinby-Hunt & Turekian 1983 Matthews & Riley 1970
Orgueil Chondrite 49 In 77.8         16 ppb Orgueil meteorite measurements. Anders & Grevesse 1989
Orgueil Chondrite 49 In 77.8         16 ppb Solar system abundances of major and minor elements as based on studies from the Orgueil Meteorite. Abundances in the Orgueil meteorite are adequately close to the C1 chondrite mean except for REE, in which case other studies will yield more preferable results Anders & Ebihara 1982
Pesyanoe Aubrite 49 In 0.51           ppb Elemental abundance of the Pesyanoe meteorite.  Classified as an Angrite, the sample itself consists of light material from the gas-rich, brecciated meteorite which was obtained by Dr. Brian Mason (U.S. National Museum).  Laul et al. 1972
Pesyanoe Aubrite 49 In 0.53           ppb Elemental abundance of the Pesyanoe meteorite.  Classified as an Angrite, the sample itself consists of dark material from the gas-rich, brecciated meteorite which was obtained by Dr. Brian Mason (U.S. National Museum).  Laul et al. 1972
Primitive Mantle 49 In 11   4.4       ppb Pyrolite model for the silicate Earth composition based on peridotites, komatiites and basalts. Error estimate is subjective. McDonough & Sun 1995
Primitive Mantle 49 In 13           ppb Elemental abundances of the Primitive Mantle of the Earth as given by various sources. This set of values are given as a comparison to those of the Bulk Continental Crust given by Rudnick & Gao of the Treatise on Geochemistry Chapter 3.1. Palme & O'Neill 2004 Yi et al. 2000
Primitive Mantle 49 In 13   5.2       ppb Elemental composition of the Primitive Mantle of the Earth as given from this study and other various sources. These elemental values are compared to those of CI Chondrites given by Palme & Jones 2004 Treatise of Geochemistry. Comments given by the authors in reference to these values: In/Y = 3 ¿ 1E-3, spinel lherzolites Palme & O'Neill 2004 Yi et al. 2000
Seawater 49 In 1             Unknown distribution type. In(OH)3[0+] is the probable main species in oxygenated seawater. Range and average concentrations normalized to 35¿ salinity. Accuracy and concentration range are uncertain. Bruland 1983
Seawater 49 In 1e-06             Broeker & Peng 1982
Seawater 49 In 0.0001           ppb Average concentration of elements in unfiltered seawater.  These values are used in conjuction with concentrations taken from the same elements in filtered river water and then used in equations (given in Li 1982) to determine mean oceanic residence time of particular elements.  Problems arise however with the relative pollution found in average river waters, and a lack of adequate data for filtered seawater to make a better comparison to filtered river water (which in this instance is found to be the most ideal comparison, yet the most difficult to perform). Li 1982
Seawater 49 In 0.1             Elemental average concentrations of the deep Atlantic and deep Pacific waters summarized by Whitfield & Turner 1987.  Li 1991 Whitfield & Turner 1987
Bruland 1983
Seawater 49 In 0.2           ng/kg This mean ocean concentratio has been calculated based on the correlation expressions in Table 1, assuming a salinity of 35¿, a nitrate concentratio of 30 ¿mol/kg, a phosphate concentratio of 2 ¿mol/kg and a silicate concentratio of 110 ¿mol/kg. Where possible data is from the Pacific ocean that shows the greates variations; otherwhise data is from the Atlantic ocean. Quinby-Hunt & Turekian 1983 Matthews & Riley 1970
Sera de Mage Eucrite 49 In 0.73           ppb Elemental abundance of the Serra de Mag¿ meteorite.  Classified as an unbrecciated eucrite, the sample used was a powder which had been reconstituted in the original proportions from magnetically separated pyroxene and feldspar fractions. Laul et al. 1972
Shergotty Meteorite 49 In 26   4       ppb Mars elemental abundances as given by Shergotty meteorite (basalitc shergottite) as given in Lodders 1988. Mars elemental abundances as given by Shergotty meteorite, which is a basalitc shergottite, as given in Lodders 1988. McSween, Jr. 2004 Lodders 1998
Shergotty Shergottite 49 In 31.3           ppb Elemental abundance of the Shergotty meteorite.  Classified as a Shergottite, the sample itself consists of material from one or several chips between 500 and 300 mg. No cleaning was attempted prior to irradiation. Laul et al. 1972
Silicate Earth 49 In 0.01           µg/g Compostioinal models for the bulk Earth, core and silicate Earth are modified after McDonough & Sun (1995). McDonough 1998
Silicate Earth 49 In 0.01           ppm Composition of the Silicate Earth as given by elemental abundances in ppm (and wt%). McDonough 2004
Silicate Earth 49 In 11   4.4       ppb Pyrolite model for the silicate Earth composition based on peridotites, komatiites and basalts. Error estimate is subjective. McDonough & Sun 1995
Sioux County Eucrite 49 In 0.52           ppb Elemental abundance of the Sioux County meteorite.  Classified as a eucrite the sample consisted of one or several chips between 500-300 mg, and no cleaning was attempted before irradiation. Laul et al. 1972
Solar Photosphere 49 In 1.66   0.15         Abundances in Solar Photosphere; in original table: log N(H) = 12.00. Uncertain data. Anders & Grevesse 1989
Solar Photosphere 49 In 1.66   0.15         Elemental solar photospheric abundances as given by various references. Values are defined as uncertain by Grevesse and Sauval 1998. Palme & Jones 2004 Grevesse & Sauval 1998
Solar System 49 In 0.19             Anders & Ebihara 1982 Cameron 1982
Solar System 49 In 0.184   0.011776     24   Anders & Ebihara 1982
Solar System 49 In 0.184   0.01178     24   Solar atomic abundances based on an average of C1 chondrites. Values are not normalised to 100% but they are relative to 10E6 Silica atoms. Anders & Grevesse 1989
Solid Earth 49 In 0.007           µg/g Compostioinal models for the bulk Earth, core and silicate Earth are modified after McDonough & Sun (1995). McDonough 1998
Solid Earth 49 In 0.007           ppm Bulk elemental composition of the Solid Earth with concentrations given in ppm (and wt% where noted). McDonough 2004
Spinel Peridotites 49 In 12 12 4     19 ppb McDonough 1990
Stannern Trend Eucrites 49 In 1.17           ppb Elemental abundance of the Stannern  meteorite sample 2.  Classified as a eucrite the sample was taken from a region of the meteorite that has a pure white/grey color.  Conversley to sample 1, this sample has lower abundances of trace elements. Laul et al. 1972
Stannern Trend Eucrites 49 In 4.04           ppb Elemental abundance of the Stannern  meteorite sample 1.  Classified as a eucrite the sample was taken from a region of the meteorite that was stained yellow.  This sample turned out to have higher concentrations of 10 trace elements, upwards of two orders of magnitude, than other eucrites. Laul et al. 1972
Upper Continental Crust 49 In 0.061           µg/g Estimates of trace element compositions of the Upper Continental Crust. These values are taken from Wedepohl 1995 and represent a previous estimate. Rudnick & Gao 2004 Wedepohl 1995
Upper Continental Crust 49 In 0.061           ppm UCC = calculated from rock averages of Heinrichs et al. (1980) in the proportions of Figure 2. Wedepohl 1995
Upper Continental Crust 49 In 50           ppb Taylor & McLennan 1995
Upper Continental Crust 49 In 0.056           µg/g Recommended composition of the Upper Continental Crust as given by various sources which are listed in Table 1 and 2 of Rudnick and Gao 2004 as well as in the text. Rudnick & Gao 2004
Upper Continental Crust 49 In 0.056   0.008       µg/g Recommended composition of the Upper Continental Crust as given by various sources which are listed in Table 1 and 2 of Rudnick and Gao 2004 as well as in the text. Rudnick & Gao 2004 see text








Upper Continental Crust 49 In 0.05           µg/g Estimates of trace element compositions of the Upper Continental Crust. These values are taken from Taylor and McLennan 1985 & 1995 and represent estimates derived from sedimentary and loess data. Rudnick & Gao 2004 Taylor & McLennan 1985
Taylor & McLennan 1995
Washougal Howardite 49 In 13.8           ppb Elemental abundance of the Washougal meteorite.  Classified as a Howardite, the sample itself consists of material from one or several chips between 500 and 300 mg. No cleaning was attempted prior to irradiation. Laul et al. 1972
Zagami Shergottite 49 In 22.2           ppb Elemental abundance of the Zagami meteorite.  Classified as a Shergottite, the sample itself consists of material from one or several chips between 500 and 300 mg. No cleaning was attempted prior to irradiation. Laul et al. 1972
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