Early diagenesis of phytyl esters in a contemporary temperate intertidal sediment

Analysis of a sediment core for hydrolysed chlorins (acidic chlorins e.g. pheophorbide a) and non-acidic chlorins, and free, bound and esterified alcohols have been performed and the results have been interpreted in terms of input and sedimentary interconversions. There is an association of the acidic chlorin input with an input of unesterified aliphatic n-alkanols (> C₂₀), and subsequent degradation of the chlorins with depth. Input of phytol to the anoxic region of the sediment is not associated with the n-alkanols:phytol in the sediment is derived largely from chlorophyll-a input to the surface layers as intact microalgae. Degradation with depth involves conversion of the chlorophyll-a to non-chlorin, colourless phytyl esters prior to incorporation of the phytol into a bound fraction. At depth this bound phytol is hydrolysed resulting in release of free phytol.     

Effect of Silica Activity on OH- IR Spectra of Olivine: Implications for Low-aSiO2 Mantle Metasomatism

Hydrogen solubility and hydroxyl substitution mechanism in olivineat upper-mantle conditions are not only a function of pressure,temperature, water fugacity and hydrogen fugacity, but are alsoinfluenced by silica activity. Olivine synthesized in equilibriumwith magnesiowüstite displays hydroxyl stretching bandsin the wavenumber range from 3640 to 3430 cm^–1. In contrast,olivine in equilibrium with orthopyroxene shows absorption bandsin a narrower wavenumber range from 3380 to 3285 cm^–1.The two fundamentally different spectra are assigned to hydroxylin tetrahedral and octahedral sublattices, respectively. Olivinein equilibrium with orthopyroxene is also less capable of incorporatinghydroxyl, relative to olivines in equilibrium with magnesiowüstite,by about a factor of ten. A comparison of spectra obtained aspart of this study with hydroxyl spectra of natural mantle olivinesshows that the latter display hydroxyl stretching patterns reminiscentof equilibrium with magnesiowüstite, although undoubtedlyolivine in the Earth’s mantle coexists with orthopyroxene.This may be attributed to a metasomatic overprint by a low-silicafluid and/or melt that was in reaction relationship with orthopyroxene.A likely metasomatic agent is a carbonatitic melt. When carbonatiticmelts decompose to oxides and CO₂, they may temporarily imposea low-aSiO₂ environment inherited by the olivine structure.If this suggestion proves true, Fourier transform IR spectroscopymay be used to fingerprint metasomatic episodes in the lithosphericmantle. KEY WORDS: FTIR spectrometry; olivine; mantle; metasomatism; water     

Evaluation of the seismic hazard of Lebanon

This paper presents the results of a study undertaken todetermine the seismic hazard of Lebanon. The seismic hazard evaluation wasconducted using probabilistic methods of hazard analysis. Potential sourcesof seismic activities that affect Lebanon were identified and the earthquakerecurrence relationships of these sources were developed from instrumentalseismology data, historical records, and earlier studies undertaken toevaluate the seismic hazard of neighboring countries. The sensitivityof the results to different assumptions regarding the seismic sources in theLebanese segment and choice of the attenuation relationship wasevaluated. Maps of peak ground acceleration contours, based on 10percent of probability of exceedance in 50 years and 100 years time spans,were developed.     

The Bear Brook Watershed in Maine: Multi-decadal whole-watershed experimental acidification

The Bear Brook Watershed in Maine (BBWM) is a long-term research site established to study the response of forest ecosystem function to environmental disturbances of chronic acidic deposition and ecosystem nitrogen enrichment. Starting in 1989, the West Bear (treated) watershed received bimonthly applications of ammonium sulfate [(NH₄)₂SO₄] fertilizer from above the canopy, whereas East Bear (reference) received ambient deposition. The treatments were stopped in 2016, marking the beginning of the recovery phase. Research at the site has focused on soils, streams, and vegetation. Here, we describe data collected over three decades at the BBWM—input and stream output nutrient fluxes, quantitative soil pits and soil chemistry, and soil temperature and moisture.     

A field test of tubino's (1991) model of alternate bar formation

This study investigates the fluvial dynamics of straight natural stream channels. In particular, this experimental field study quantitatively assesses a physically based non-linear mathematical theory of alternate bar formation under unsteady natural flow conditions within a straight alluvial stream. The study site is an artificially straightened section of the Embarras River located approximately 16 km south of Champaign, Illinois. Data were collected on channel form, gradient, alternate bar dimensions, bed sediment size and flow stage over a 2 year study period. Both linear and non-linear steady flow hydrodynamic theories suggest that alternate bars are critical to the process of meander development. But these theories do not predict bar development for unsteady flow conditions, which typically occur in natural alluvial channels. Tubino (1991) suggests that bar evolution for a flood hydrograph can be divided into three parts: (1) a period of limited bar growth during the rising stage of the flood; (2) a stage of modest bar decay near the peak of the flood; and (3) a stage of non-linear bar growth during the prolonged falling stage of the flood. Bars developed during the falling limb of a hydrograph, and exhibited sequential development rather than the uniform growth along the reach predicted by Tubino's model. As flow stage decreased, short, low, fine-grained bars were superimposed on long, high and coarser-grained bars that developed under preceding high flow stages. These results suggest that the process of bar formation in artificially straightened natural streams with heterogeneous bed material may occur under different flow conditions and in a different manner than predicted by theoretical models. Further work should focus on attempting to isolate the physical mechanisms responsible for alternate bar formation in straight natural streams with heterogeneous bed material and flashy hydrologic flow regimes.     

The use of caesium‐137 to estimate agricultural erosion on steep slopes in a tropical watershed

The estimation of erosion and sediment delivery rates in tropical mountain watersheds is difficult and most of the methods widely used for estimating soil erosion over large areas have serious limitations. The ¹³⁷Cs approach has potential for quantifying soil erosion because it can provide retrospective estimates of long‐term (since 1963) net sediment redistribution relatively quickly. Despite its great potential, ¹³⁷Cs has not yet been used in an extensive, reconnaissance level survey of erosion in complex tropical mountain environments. The objective of this study was to examine the applicability of the ¹³⁷Cs method to estimate erosion on steep tropical agricultural lands (23 to 80% slopes) in the Nizao watershed, a humid, tropical mountain area of the Dominican Republic. In this study we (i) examine the variation of ¹³⁷Cs in ten reference sites—eight coffee groves and two forested sites—and (ii) estimate erosion from 14 cultivated fields. The soil pool of ¹³⁷Cs ranged from to 150 to 192 mBq cm⁻² on reference sites with minimal erosion. Variability among reference sites was less than expected for such complex mountain terrain. The variability within coffee and forested reference (average CV=28%) sites was similar to the variability found on grassland and forested reference sites in the temperate zone. The estimated annual soil loss from 14 sampled fields ranged from 6 to 61 t ha⁻¹ year⁻¹ with an overall mean of 26 t ha⁻¹ year⁻¹. Overall, the soil erosion estimates found using the ¹³⁷Cs method were much lower than those often assumed for such steep tropical hillsides. These erosion estimates account for soil loss since 1963 only and it seems likely that soil losses may have been much higher in earlier decades immediately after initial forest clearing earlier in the 20th century. Copyright © 2000 John Wiley & Sons, Ltd.     

Observations of rapid mean flow produced in mercury by a moving heater

Abstract

Experimental and theoretical results are described for the moving flame experiment, where a heat source moves under a horizontal, annular channel filled with liquid mercury. The physical range under discussion consists of the creep flow limit, in which inertial forces are less than viscous forces. A mean surface flow was observed on the mercury. This flow was up to four times greater than the heater speed, and in an opposite direction. The ratio of mean flow to heater speed was theoretically and experimentally found to be proportional to the square of the thermal amplitude, in agreement with a special limit of Davey's earlier results. The basic flow here, as contrasted to those flows analyzed by earlier theories, appears to be generated by surface tension. However, the Reynolds stress mechanism which generates the mean flow is the same. Some experimental flows were so rapid that the range of validity of the present, as well as some earlier theories, was exceeded. The present theory suggests that the higher order nonlinearities may have cancellative effects, which implies that the present and some earlier theories are valid beyond their normal range of validity.     

雅鲁藏布江缝合带的双陆内俯冲构造与部分熔融层特征──INDEPTH项目结果的初步综合

根据中、美两国合作开展的西藏深反射地震结果,提出雅鲁藏布江缝合带（YZS）的"双陆内俯冲"构造模式和缝合带南、北分别存在着不同特征的、规模不一的部分熔融层;提出YZS处断裂向深部延深有限,认为YZS处地壳增厚有4种机制：①地壳规模的大的俯冲增厚;②上部地壳内的俯冲和背冲增厚;③下地壳内的底部垫托增厚和挤压增厚;④深部熔融体的向上挤入而引起的地壳增厚.提出可能存在两条大的伸展性断裂,造成江孜南、北地块间出现了大升降.     

Changed relation between sunspot numbers,solar UV/EUV radiation and TSI during the declining phase of solar cycle 23

We study the mutual relation of sunspot numbers and several proxies of solar UV/EUV radiation, such as the F10.7 radio flux, the HeI 1083 nm equivalent width and the solar MgII core-to-wing ratio. It has been noted earlier that the relation between these solar activity parameters changed in 2001/2002, during a large enhancement of solar activity in the early declining phase of solar cycle 23. This enhancement (the secondary peak after the Gnevyshev gap) forms the maximum of solar UV/EUV parameters during solar cycle 23. We note that the changed mutual relation between sunspot numbers and UV/EUV proxies continues systematically during the whole declining phase of solar cycle 23, with the UV/EUV proxies attaining relatively larger values for the same sunspot number than during the several decennia prior to this time. We have also verified this evolution using the indirect solar UV/EUV proxy given by a globally averaged f₀(F2) frequency of the ionospheric F2 layer. We also note of a simultaneous, systematic change in the relation between the sunspot numbers and the total solar irradiance, which follow an exceptionally steep relation leading to a new minimum. Our results suggest that the reduction of sunspot magnetic fields (probably photospheric fields in general), started quite abruptly in 2001/2002. While these changes do not similarly affect the chromospheric UV/EUV emissions, the TSI suffers an even more dramatic reduction, which cannot be understood in terms of the photospheric field reduction only. However, the changes in TSI are seen to be simultaneous to those in sunspots, so most likely being due to the same ultimate cause.     

The brown dwarf desert as a consequence of orbital migration

We show that the dearth of brown dwarfs in short-period orbits around Solar-mass stars – the brown dwarf desert – can be understood as a consequence of inward migration within an evolving protoplanetary disc. Brown dwarf secondaries forming at the same time as the primary star have masses which are comparable to the initial mass of the protoplanetary disc. Subsequent disc evolution leads to inward migration, and destruction of the brown dwarf, via merger with the star. This is in contrast with massive planets, which avoid this fate by forming at a later epoch when the disc is close to being dispersed. Within this model, a brown dwarf desert arises because the mass at the hydrogen-burning limit is coincidentally comparable to the initial disc mass for a Solar mass star. Brown dwarfs should be found in close binaries around very low mass stars, around other brown dwarfs, and around Solar-type stars during the earliest phases of star formation.