Abundances data sources

Percentage of meteorites seen to fall. Chondrites. Over 90% of meteorites that are observed to fall out of the sky are classified as chondrites, samples that are distinguished from terrestrial rocks in many ways (3). One of the most fundamental is age. Like most meteorites, chondrites have formation ages close to 4.55 Gyr. Elemental composition is also a property that distinguishes chondrites from all other terrestrial and extraterrestrial samples. Chondrites basically have undifferentiated elemental compositions for most nonvolatile elements and match solar abundances except for moderately volatile elements. The most compositionaHy primitive chondrites are members of the type 1 carbonaceous (Cl) class. The analyses of the small number of existing samples of this rare class most closely match estimates of solar compositions (5) and in fact are primary source solar or cosmic abundances data for the elements that cannot be accurately determined by analysis of lines in the solar spectmm (Table 2). Table 2. Solar System Abundances of the Elements ... 

Table 3.1. Data sources and methods for cosmic abundances...

Nevertheless, the mid-peak potentials determined by cyclic voltammetry and other characteristic potentials obtained by different electroanalytical techniques (such as pulse, alternating current, or square wave voltammetries) supply valuable information on the behavior of the redox systems. In fact, for the majority of redox reactions, especially for the novel systems, we have only these values. (The cyclic voltammetry almost entirely replaced the polarography which has been used for six decades from 1920. However, the abundant data, especially the half-wave potentials, 1/2, are still very useful sources for providing information on the redox properties of different systems.)... 

Figure 12.4 Vertical profiles of the Group 3 elements in the North Pacific Ocean, including selected actinides. Data sources Sc (Spencer et al., 1970), Y, La, Pr-Lu (Zhang and Nozaki, 1996), Ce (Piepgras and Jacobsen, 1992), Ac (Nozaki, 19 84), 232Th (Roy-Barman et al., 1996), U (Chen et al., 1986) and 241Am (Livingston et al., 1983). Relative species abundance is shown to the right of each figure in descending order.

Figure 6.5 Correlation plots between 36 Ar abundance and 3He, 20Ne, 84Kr, and 132Xe abundances (cf. Table 6.1 for data source). Note that even though there are good correlations among the heavier noble gases (Ne in OIB Ar, Kr, and Xe in MORB and OIB), correlations between He and the heavier noble gases are totally lacking.

Figure 1. Plot of thermoluminescence sensitivity against petrologic type (5,6), which reflects the degree of metamorphic alteration 3, least metamorphosed 6, most metamorphosed. The feldspar scale is calculated on the assumption that the TL sensitivity is directly proportional to feldspar abundance and type 5,6 chondrites typically contain about 8% of this mineral. The cross-hatched region refers to TL sensitivity levels at which the feldspar is thought to be in the low-temperature ordered form (see Figure 13). The symbols refer to the three data sources (6,8,14). (Reprinted by permission from Ref. 31.

Figure 9 Normative spinel Iherzolite mineral abundances (wt.%) versus rock Mg for a subset of 292 off-craton mantle compositions (shaded circles). Data from a given locality were included if compositions had a correlation between Mg and normative olivine with a correlation coefficient (i ) of 0.6 or better. Data sources for xenoliths are Beccaluva et al. (2001a,h), Reid and Woods (1978), Rivalenti et al. (2000), Stem et al. (1999), Vaselli et al. (1995), Wiechert et al. (1997), Xu et al. (1988), and Zangana et al. (1999). Data sources for orogenic Iherzolites are Bodinier et al. (1988), Frey et al. (1985, 1991), Hartmann and Wedepohl (1993), and Lugovic et al. (1991). Open circles are the reconstmcted abyssal peridotite compositions from Figure 7. Also shown are estimates of primitive mantle from Table 2 white square = 1, circle = 2, triangle = 3, diamond = 5, inverted triangle = 6, ex = 7, and shaded star = 8.

Figure 7 The relative abundances of C, N, and H in the Earth plotted versus the log of the 50% condensation temperature (K) at 10 " atm pressure. The Earth s estimate is based on compositional estimates of these gases in the mantle and the Earth s surface, as well as by comparison with data for carbonaceous chondrites (data sources are as in Eigure 5).

Figure 13 Nd abundance versus (a) salinity and (b) silicate in deep seawater. Nd concentrations do not show the same well-behaved characteristics as Nd-isotope ratios with salinity and silicate in global deep water. Mixing envelopes are shown between North Atlantic and Pacific end-members, and the circum-Antarctic, South Atlantic, and Indian Ocean samples fall outside of it. Plotted data are from >2,500 mb si, except two Drake Passage data from 1,900 m and 2,000 m (Nd data sources Piepgras and Wasserburg, 1980, 1982, 1983, 1987 Spivack and Wasserburg, 1988 Piepgras and Jacobsen, 1988 Bertram and Elderfield, 1993 Jeandel, 1993 Shimizu et al., 1994 Jeandel et ah, 1998). Where salinity or silicate were not available in the publication, they were estimated from Levitus (1994),...

Figure 10. Distribution of zinc content (left panel) and arsenic content (right panel) in coals from the Illinois basin. Data sources are given in the text. The size of the symbol is proportional to the abundance of the element. The breakpoints for the element distributions were chosen using the default natural breaks algorithm in the computer program Arcview . Faults are shown as light lines. Note the concentration of zinc and arsenic associated with the intense faulting in the southern Illinois Basin, and the localization of zinc and arsenic in the northwestern portion of the basin.

Fig. 2. Comparison of volatile abundance data in protosolar nebula (PSN), primitive chondrites, terrestrial mantle and atmosphere (atmosphere sensu stricto, crust, sediments, oceans). Data are normalized to Ne and PSN, so that the PSN pattern is flat. The choice of Ne as a normalizing isotope is based on the observation that recycling of atmospheric neon in the mantle is limited as indicated by its isotopic composition. Data sources Mazor et al. (1970), Marty Jambon (1987), Anders Grevesse (1989), Pepin (1991), Moreira et al. (1998), Ozima et al. (1998), Marty Zimmermann (1999).

There are several reasons to introduce ADDs. First an ADD easily illustrates distributions of sources in age and distance. Then it is possible to plot expectation lines for an abundance of sources of different types and compare them with data (i.e. line which show how many sources of smaller than a given value we can expect to find at distances smaller than a given one). Finally since the observability of sources depends mainly on their ages and distances, it is possible to illustrate observational limits. 

Stellar atmospheres. Stellar spectroscopy, most particularly stellar photospheric spectroscopy, is a major source of the abundance data used to address questions of nucleosynthesis. 

The observational data to be discussed represent a highly selected sample of abundances, gas masses, and stellar photometry from sources too numerous to mention here. (If you recognize your data in the following plots, feel free to take credit.) I will employ abundances derived almost exclusively from H II region spectra, since they contribute the largest set of abundance data for spirals and irregulars in the local universe. 

Fig. 1. The decreasing element concentration ratio of CM- over Cl chondrites indicates volatility related fractionations in CM meteorites and makes them of limited use as an abundance standard. The different symbol shapes indicate the principal mineral host phase for the elements (circle lithophile elements in silicate and oxides box siderophile elements in metal alloy chalcophile sulfides triangle halogen). Data sources for CM chondrites [21] plus updates Cl chondrites [17]...

The selected concentrations for the Orgueil meteorite, considered as most representative for the Cl chondrites, are listed in Table 2 details about the data sources are in LPG09. Concentrations are given as parts per million (ppm) by mass (10,000 ppm = 1 mass%). Corresponding atomic abundances normalized to 106 Si atoms (the cosmochemical abundance scale ) are listed as well. 

It is common for the number of gamma-rays emitted by a nuclide to be referred to as the abundance , sometimes as the yield . Both of these terms lack precision. Historically, confusion was often caused because an author or data source would quote abundances that were effectively beta transition data - the 93.5 % figure quoted above. In fact, the proportion of decays that give rise to 661.7 keV gamma-rays in the example above is 85.1 % when internal conversion is taken into account. In this text, I will use the term gamma emission probability on the basis that it says exactly what it means - the probability that a gamma-ray will be emitted, aU other factors being taken into account. 

In summary, we have determined LA-ICP-MS analysis to be an accurate and precise instrumental technique for chemical characterization of obsidian artifacts and source samples. We have developed two methods for normalization and standardization of obsidian data that while different, permit LA-ICP-MS data to be transformed to abundance data and that data derived by LA-ICP-MS conq>ares favorably to INAA data. The minimal sanq>le preparation time, the ability to select the suite of elements that will be analyzed, and the rapid analytic time make LA-ICP-MS, a minumUy invasive, cost-effective method for characterizing obsidian. 

Remark Manganese ore contains about 40% manganese (Source of production data http //minerals.usgs.gOv/minerals/pubs/commodity/statistical summary/mybl-2006-stati.pdf Source of abundance data Geological handbook, Heibon-sha, Tokyo, Japan)... 

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