Relationships between organically bound Cu and Mn in settling particulate matter and biological processes in a subarctic estuary

Plankton studies in Kachemak Bay, Alaska were combined with short-term sediment trap deployments in order to show the relationships of fluxes of Cu and Mn in organic particulate matter with biological processes occurring in the overlying water column. A large spring bloom decrease throughout the summer, due to decreasing nutrient levels and increasing grazing pressure by zooplankton. The concentration of organically bound Cu and Mn in the sediment trap particulate material increased throughout the summer reaching a maximum in August while fecal pellet production exhibited a similar increase. The fluxes of total particulate matter and organic carbon reached a maximum in June and represented a 30% increase over the corresponding fluxes in May. In contrast, the fluxes of organically bound Cu and Mn and fecal pellets in August represented 200%, 360% and 760% increases, respectively, over their respective fluxes in May. These results suggest that the enrichment of Cu and Mn in the organic particulate matter during August was a result of bioaccumulation of these metals into fecal material. The increase in the flux of the organically bound metals indicates a strong coupling between biological processes in the water column and their vertical transport. Thus, the production and subsequent sinking of fecal pellets may govern the transport of trace metals to the underlying water column and may also govern the transfer of a primary source of food and its associated trace metals to benthic communities.     

Vertical transport of steroid alcohols and ketones measured in a sediment trap experiment in the equatorial Atlantic Ocean

The vertical flux and free steroid alcohol (sterol) and ketone composition of particulate material was determined using sediment traps deployed at 389, 988, 3755 and 5068 m at a station in the equatorial North Atlantic, PARFLUX E. Cholest-5-en-3β-ol (cholesterol) was found to be the dominant sterol in all the traps. This compound had a maximum flux at 988 m, accounting for more than 90% of the sterols at this depth. Inputs from mesopelagic Zooplankton populations living in or migrating to depths between the 389 and 988 m traps appear to be responsible for this distribution. The deeper two traps exhibited an increased flux of phytosterols relative to cholesterol, probably due to (a) the incorporation of labile phytoplankton remains in fecal pellets and rapid transport into the deep sea and (b) differential dissolution of heterogeneous large particles. A maximum of 5–22% of the sterols produced in the euphotic zone were present in the 389 m trap. This value drops to less than 1% for the 5068 m trap, 200 m above the sediment surface.In general steroid ketone fluxes gradually decreased with depth. Δ4-Stenones were found in greater abundance than their saturated counterparts. Cholest-4-en-3-one was the major steroid ketone detected in all the traps. A five-fold increase with depth in the cholest-4-en-3-one to cholesterol ratio is most likely due to microbial oxidation of sterols to steroid ketones, or higher Δ4-stenone inputs relative to sterols from organisms.     

Petrography,mineral chemistry and origin of Type I enstatite chondrites

Optical and cathodoluminescence petrography were coupled with electron microprobe analysis to relate the textures and chemical compositions of minerals in the chondrules and matrix of the Indarch, Kota-Kota, Adhi-Kot and Abee Type I enstatite chondrites. Clinoenstatites fall into two distinct chemical groups with characteristic red or blue luminescence; red crystals are higher in Ti, Al, Cr, Mn and Ca, and lower in Na, than blue ones. Rare forsterites in Indarch and Kota-Kota show distinct compositions associated with orange or blue luminescence. The chemical ranges are indistinguishable for each color type in chondrules of all textural types, and the presence of both color types in a single chondrule or a metal fragment requires mechanical aggregation of both crystals and liquids of both color types. Porphyritic chondrules are ascribed mainly to aggregation of existing crystals because both types of pyroxene and olivine occur in the same chondrule. Large crystals of one color type are surrounded by fine-grained crystals of another type in some barred and radiating chondrules. All types of chondrules are surrounded by fine-grained rims rich in sulfide. The matrix contains many broken chondrules and individual silicate grains but is rich in sulfide and metal. Analyses are given of albite (minor elements and luminescence color vary between chondrites), kamacite, schreibersite, oldhamite and niningerite.Although the mineral assemblages do not fit theoretical condensation sequences in detail, the red pyroxene and orange olivine might result ultimately from near-equilibrium crystallization in which early reduced condensates reacted with a gas, while the blue crystals might result from fractional condensation in which early condensates were removed mechanically from a gas. Subsequent episodes involving mixing, melting, crystallization, condensation, fracturing, and mechanical aggregation would be needed to produce the complex textures.     

Low temperature spectral studies of Mn3+-bearing andalusite and epidote type minerals in the range 30000–5000 cm−1

Polarized absorption spectra of natural piemontite (Ca_1.802Mn ²⁺_0.178 Mg_0.025) (Mn ³⁺_0.829 Fe ³⁺_0.346 Al_1.825) [(Si_2.992Al_0.008) O₁₂OH], viridine (Al_1.945Mn ³⁺_0.033 Fe ³⁺_0.063 Mg_0.003) [O|Si_0.970 O₄], and kanonaite (Al_1.291Mn ³⁺_0.682 Fe ³⁺_0.019 ) [O|Si_1.006 O₄] were measured at 295 and ca. 100 K. For piemontite, lowering the temperature resulted in a sharpening of broad bands in the 10 000–25 000 cm⁻¹ region supporting their assignment to single ion Mn³⁺ in M3 non-centrosymmetric sites.

Alternatively, in kanonaite, temperature behaviour pointed to a slightly stronger influence of vibronic coupling on strong bands near 16 000 and 22 000 cm⁻¹, which supported an interpretation of Mn³⁺ in nearly centrosymmetric M1 sites. Measurements at ca. 100 K show pronounced fine structure in the viridine spectra which is attributed to Fe³⁺. The ɛ values for Mn³⁺ spin-allowed bands in the three minerals lie in the range 18 to 227 [1·g-atom⁻¹·cm⁻¹].

For the same band and polarisation, ɛ values in Mn³⁺-bearing andalusite-type minerals viridine and kanonaite are the same, which indicates an absence of strong magnetic coupling effects between Mn³⁺ ions in the andalusite type structure down to ca. 100 K.

In silicates, the high ɛ values for Mn³⁺ spin-allowed bands, in comparison to those obtained for Fe²⁺ spin-allowed bands from sites of “similar distortion”, is attributed to a higher degree of covalency in the Mn³⁺-O bonds compared to the Fe²⁺-O bonds, as a result of the higher valence state of manganese.

     

Spectral analysis of earthquake migration in South America

Earthquake migration along linear seismic belts is investigated by analyzing spacetime diagrams using spectral analysis. In order to sample the earthquakes in the space-time domain, they must first be convolved with a (sinx sint)/xt surface to obtain an unbiased and alias free twodimensional Fourier spectrum. Further enhancements are provided by selectively stacking patterns (a pattern is defined as the distribution of earthquakes in space and time before a particular earthquake), thereby reinforcing the similarities within the various patterns. With these techniques, it is possible to quantitatively estimate the migration rates (from theirspatial frequencies) and recurrence intervals (from theirtemporal frequencies) of large earthquakes in South America.Preliminary examination of the spectra for South America indicates that a low frequency peak occurs at approximately 2500 km and 27 years for earthquakes with magnitudes greater than 7.7. The results suggest a migration rate of approximately 95 km/yr from south to north and a recurrence interval of 27 years.     

The fate of stranded pelagic tar on a Bermuda beach

The major process involved in the removal of stranded petroleum residues or ‘tar lumps’ from sandy high energy beaches is the adsorption of sand and shell particles to the residues effecting a density change. This results in transport off the beach, sinking, and sometimes burial of the tar in sublittoral sediments.     

Argon 40-argon 39 chronology of lithic clasts from the Kapoeta howardite

⁴⁰Ar-³⁹Ar age spectra have been measured on plagioclase separates from three basaltic clasts (A, B, C), a pyroxene separate from clast B, and a total sample of a fourth basaltic clast (ρ) from the Kapoeta achondritic meteorite. The Ar data show that three of the four clasts crystallized ≥4.5 AE ago. Xe measurements indicate all four formed within a 0.1 AE period (Huneke, et al., 1977, Lunar Science VIII, pp. 484–486). Three clasts have suffered various degrees of ⁴⁰Ar loss since that time. The times of ⁴⁰Ar degassing do not cluster about a single time analogous to the lunar cataclysm. The survival of ≥4.5 AE ages contrasts with the general absence of ages ≥4.0 AE on the moon.The Ar retention age of clast B of ≥4.57 AE is atypically older than the Rb-Sr age of 3.6 AE (Papanastassiouet al., 1974, Lunar Science V, p. 583). The 3.5 AE Ar age of clast A is distinctly younger than the Rb-Sr age of 3.9 AE (Papanastassiou et al., 1974). The K-Ar and Rb-Sr systems are clearly not equivalent dating techniques in these instances.The combined evidence of Ar, Xe and Rb-Sr studies suggests the period of volcanism on the Kapoeta parent planet was restricted to the first ~0.2 AE of solar system history. The subsequent thermal metamorphic histories recorded in each of the four clasts after formation are distinctly different. The clasts must have existed as independent fragments at least as recently as 3.5 AE ago. The cosmic ray exposure ages of all the four clasts are similar (~ 3 Myr), and are not significantly different from that of the bulk meteorite. The clasts spent essentially all of the time prior to the formation of Kapoeta at depths greater than a few meters.     

The mobility of the rare earth elements: Evidence and implications from selected terrains affected by burial metamorphism

The mobility of the rare earth element (REE) during hydrous burial metamorphism is described from three localities. Comparison of REE abundances in relict domains and metadomains from flood lavas in the Maddina Volcanics, Fortescue Group, Western Australia shows that, relative to the relict domains, REE may be strongly depleted in certain metadomains. Strong variations in La/Yb, La/Sm and Eu may also occur due to postcrystallization secondary processes. Similar comparisons in flood lavas from Mamainse Point in the Canadian Keweenawan Series show that REE are mobile and increase in abundance in metadomains. Spilites from U.S. Virgin Islands also show evidence for REE mobility during low grade burial metamorphism. In this case light REE (LREE) have been preferentially mobilized with heavy REE (HREE) remaining parallel or sub-parallel on chondrite normalized plots.REE analyses from these locations together with an evaluation of published work suggests that the mobility of REE can be described by: 1. gross REE and selective LREE enrichment; 2. REE movement around a primary mean; 3. gross REE depletion; 4. selective REE mobility. Failure to take into account REE mobility may lead to incorrect conclusions concerning petrogenetic models based on altered basic sequences. The coherence of REE with other key trace elements during alteration is also discussed.     

Holocene offset and seismicity along the panamint valley fault zone, western basin-and-range province, California

Holocene right-slip along the central segment of the Panamint Valley totals 20 m and dip-slip is somewhat less. The most recent offset, about 2 m right-slip, probably occurred at least several hundred years ago. If a comparable amount of slip occurred during earlier earthquakes, mean seismic recurrence intervals would have been about 700–2500 years during the Holocene.