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Agostino Renda Daisuke Kawata Yeshe Fenner Brad K. Gibson 《Monthly notices of the Royal Astronomical Society》2005,356(3):1071-1078
The chemical evolution history of a galaxy hides clues about how it formed and has been changing through time. We have studied the chemical evolution history of the Milky Way (MW) and Andromeda (M31) to find which are common features in the chemical evolution of disc galaxies as well as which are galaxy-dependent. We use a semi-analytic multizone chemical evolution model. Such models have succeeded in explaining the mean trends of the observed chemical properties in these two Local Group spiral galaxies with similar mass and morphology. Our results suggest that while the evolution of the MW and M31 shares general similarities, differences in the formation history are required to explain the observations in detail. In particular, we found that the observed higher metallicity in the M31 halo can be explained by either (i) a higher halo star formation efficiency (SFE), or (ii) a larger reservoir of infalling halo gas with a longer halo formation phase. These two different pictures would lead to (i) a higher [O/Fe] at low metallicities, or (ii) younger stellar populations in the M31 halo, respectively. Both pictures result in a more massive stellar halo in M31, which suggests a possible correlation between the halo metallicity and its stellar mass. 相似文献
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Stable isotope ratios obtained from pronghorn teeth recovered from archaeological sites in southwestern Wyoming may provide information on past climate and hunter behavior. However, the interpretation of archaeological isotope values depends on pronghorn isotopic correlations with the environment and geography. To investigate these correlations, a series of modern Wyoming carbon, oxygen and strontium isoscapes are compared with recent temperature, humidity and geological variation. Results indicate that both pronghorn and sagebrush carbon, and to a lesser degree oxygen, isotope ratios are tied to relative humidity. Temperature is correlated with oxygen isotope ratios in sagebrush, but not pronghorn. Strontium isotope ratios in both sagebrush and pronghorn vary with geography, which in turn reflects variation in geology. 相似文献
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M. C. Kennicutt II W. L. Keeney-Kennicutt B. J. Bresley F. Fenner 《Environmental Geology》1982,4(3-4):239-249
The influence of drilling fluid dispersion on the chemistry of surficial sediments was determined by an integrated study of
organic and inorganic parameters. Pyrolysis characteristics and barium, organic carbon, and carbonate content were determined
for sediments associated with six drilling sites in coastal Gulf of Mexico waters. The areal extent and magnitude of influence
of dispersed fluids were related to water depth, prevailing currents, density of the dispersed material, history of the drill
site and platform-induced biological activity. The potential use of pyrolysis techniques for defining the impact area and
the various types of inputs derived from off-shore drilling operations was demonstrated. 相似文献
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S. D. Ryder Y. Fenner B. K. Gibson 《Monthly notices of the Royal Astronomical Society》2005,358(4):1337-1351
We describe the technique of absorption-line imaging of galaxy discs using the Taurus Tunable Filter on the Anglo-Australian Telescope and demonstrate its sensitivity to the behaviour of spectral features associated with Mg and Fe. Radial profiles of Mg2 and Fe5270 line strengths are presented for a sample of eight face-on spiral galaxies spanning a range of Hubble types. Signatures of phenomena including merger-induced star formation, H ii rings and galactic bars are also reported. This study demonstrates the capacity of tunable filters to measure Mg and Fe line strengths across the face of spiral galaxies, which can ultimately reveal clues about the star formation history and chemical evolution. 相似文献
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F. Lindenmaier R. Miller J. Fenner G. Christelis H. G. Dill T. Himmelsbach S. Kaufhold C. Lohe M. Quinger F. Schildknecht G. Symons A. Walzer B. van Wyk 《Hydrogeology Journal》2014,22(6):1307-1328
An exploration strategy for groundwater was established and followed in the northern Namibian Cuvelai-Etosha Basin (CEB). The data derived from transient electromagnetics, rotary-drilling, coring and sample investigation were used to refine stratigraphy and hydrostratigraphy, and to develop a 3D map of aquifers within the Cubango Megafan. The results have delineated three major aquifers. The newly found, deep-seated Ohangwena II Aquifer (KOH-2) has the potential of providing significant additional water to the water supply of northern Namibia and Angola. While near-surface aquifers carry predominantly brackish water, freshwater in the deep-seated aquifer is further extended and features good hydraulic properties. To date, only a small part of the hydrogeological potential of arid CEB has been explored and an extension of exploration is needed, including southern Angola. The combination of structural, sedimentological and hydrogeological approaches greatly advanced both the geological and hydrogeological understanding. With regard to the deep-seated aquifer, strict measures need to be applied to ensure that the water in the KOH-2 reservoir is exploited sustainably. Water control areas need to be established to ensure long-term preservation of this newly explored aquifer. 相似文献
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Y. Fenner M. T. Murphy B. K. Gibson 《Monthly notices of the Royal Astronomical Society》2005,358(2):468-480
At redshifts z abs ≲ 2 , quasar absorption-line constraints on space–time variations in the fine-structure constant, α, rely on the comparison of Mg ii and Fe ii transition wavelengths. One potentially important uncertainty is the relative abundance of Mg isotopes in the absorbers, which, if different from solar, can cause spurious shifts in the measured wavelengths and, therefore, α. Here we explore chemical evolution models with enhanced populations of intermediate-mass (IM) stars, which, in their asymptotic giant branch phase, are thought to be the dominant factories for heavy Mg isotopes at the low metallicities typical of quasar absorption systems. By design, these models partially explain recent Keck/HIRES evidence for a smaller α in z abs < 2 absorption clouds than on Earth. However, such models also overproduce N, violating observed abundance trends in high- z abs damped Lyman-α (DLA) systems. Our results do not support the recent claim of Ashenfelter et al. that similar models of IM-enhanced initial mass functions (IMFs) may simultaneously explain the HIRES varying-α data and DLA N abundances. We explore the effect of the IM-enhanced model on Si, Al and P abundances, finding it to be much less pronounced than for N. We also show that the 13 C/12 C ratio, as measured in absorption systems, could constitute a future diagnostic of non-standard models of the high-redshift IMF. 相似文献
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