Biomarkers in flounder (Platichthys flesus): an evaluation of their use in pollution monitoring

Flounder (Platichthys flesus) is among the most common fish-species in Norwegian and European estuaries. It lives in or on sediments from which it also finds most of its food. The aim of the present work was to evaluate biomarkers in flounder for possible future use in monitoring programmes. There were clear biomarker responses in flounder following injection of model contaminants benzo[a]pyrene (B[a]P), PCB #156 and Cd, singly or in sequence. Cytochrome P4501A responded following injection of the organic contaminants and metallothionein (MT) following Cd injection. All groups receiving B[a]P, either singly or in combination with other contaminants, accumulated high levels of B[a]P-metabolites in bile. There was little change in glutathione-S-transferase activity (measured using CDNB as substrate) following the treatments. Starvation appeared to affect the response of hepatic MT to Cd, but none of the other biomarkers. PAH in sediments elicited strong biomarker responses in caged flounder, whereas sediment-associated metals appeared to be largely unavailable to flounder in this study.     

Rainfall interception in a lower montane forest in Ecuador: effects of canopy properties

Rainfall interception in forests is influenced by properties of the canopy that tend to vary over small distances. Our objectives were: (i) to determine the variables needed to model the interception loss of the canopy of a lower montane forest in south Ecuador, i.e. the storage capacity of the leaves S and of the trunks and branches S_t, and the fractions of direct throughfall p and stemflow p_t; (ii) to assess the influence of canopy density and epiphyte coverage of trees on the interception of rainfall and subsequent evaporation losses. The study site was located on the eastern slope of the eastern cordillera in the south Ecuadorian Andes at 1900–2000 m above sea level. We monitored incident rainfall, throughfall, and stemflow between April 1998 and April 2001. In 2001, the leaf area index (LAI), inferred from light transmission, and epiphyte coverage was determined. The mean annual incident rainfall at three gauging stations ranged between 2319 and 2561 mm. The mean annual interception loss at five study transects in the forest varied between 591 and 1321 mm, i.e. between 25 and 52% of the incident rainfall. Mean S was estimated at 1·91 mm for relatively dry weeks with a regression model and at 2·46 mm for all weeks with the analytical Gash model; the respective estimates of mean S_t were 0·04 mm and 0·09 mm, of mean p were 0·42 and 0·63, and of mean p_t were 0·003 and 0·012. The LAI ranged from 5·19 to 9·32. Epiphytes, mostly bryophytes, covered up to 80% of the trunk and branch surfaces. The fraction of direct throughfall p and the LAI correlated significantly with interception loss (Pearson's correlation coefficient r = −0·77 and 0·35 respectively, n = 40). Bryophyte and lichen coverage tended to decrease S_t and vascular epiphytes tended to increase it, although there was no significant correlation between epiphyte coverage and interception loss. Our results demonstrate that canopy density influences interception loss but only explains part of the total variation in interception loss. Copyright © 2004 John Wiley & Sons, Ltd.     

Unstable extension of Enceladus' lithosphere

Regions near Enceladus' equator, Sarandib and Diyar Planitia, contain extensive sets of parallel ridges and troughs that may be diagnostic of the region's formation conditions. We present photoclinometry profiles across these ridges and troughs, which indicate that they are periodic, low-slope features with dominant wavelengths of 3 to 4 km and amplitudes between 100 and 400 m. The morphology of these terrains is consistent with formation via unstable extension of the lithosphere. Our numerical modeling demonstrates that unstable extension can generate large-scale topography under Enceladus-like conditions. Comparison of our photoclinometry profiles with the dominant wavelengths produced by our numerical model permits estimation of the background heat flow at the time the Sarandib-Diyar province formed. We estimate heat flows of 110 to , suggesting that resurfacing of the planitiae was accompanied by strong, localized heating. The extension necessary to produce the ridges and troughs may have been caused by now-inactive diapirs, internal phase changes, or other mechanisms. Our heat flux estimates imply elastic thickness at the time of resurfacing of 0.4 to 1.4 km, which are sufficient to have allowed satellite reorientation if the province was underlain by a low-density region. It is therefore plausible that Enceladus has experienced multiple heating events, each leading to localized resurfacing and global reorientation.     

Testing fundamental physics with distant star clusters: theoretical models for pressure-supported stellar systems

We investigate the mean velocity dispersion and the velocity dispersion profile of stellar systems in modified Newtonian dynamics (MOND), using the N -body code n-mody , which is a particle-mesh-based code with a numerical MOND potential solver developed by Ciotti, Londrillo & Nipoti. We have calculated mean velocity dispersions for stellar systems following Plummer density distributions with masses in the range of 10⁴ to  10⁹ M_⊙  and which are either isolated or immersed in an external field. Our integrations reproduce previous analytic estimates for stellar velocities in systems in the deep MOND regime  ( a _i, a _e≪ a ₀)  , where the motion of stars is either dominated by internal accelerations  ( a _i≫ a _e)  or constant external accelerations  ( a _e≫ a _i)  . In addition, we derive for the first time analytic formulae for the line-of-sight velocity dispersion in the intermediate regime  ( a _i∼ a _e∼ a ₀)  . This allows for a much-improved comparison of MOND with observed velocity dispersions of stellar systems. We finally derive the velocity dispersion of the globular cluster Pal 14 as one of the outer Milky Way halo globular clusters that have recently been proposed as a differentiator between Newtonian and MONDian dynamics.     

Geology of the Selk crater region on Titan from Cassini VIMS observations

Observations of Titan obtained by the Cassini Visual and Infrared Mapping Spectrometer (VIMS) have revealed Selk crater, a geologically young, bright-rimmed, impact crater located ∼800 km north-northwest of the Huygens landing site. The crater rim-crest diameter is ∼90 km; its floor diameter is ∼60 km. A central pit/peak, 20-30 km in diameter, is seen; the ratio of the size of this feature to the crater diameter is consistent with similarly sized craters on Ganymede and Callisto, all of which are dome craters. The VIMS data, unfortunately, are not of sufficient resolution to detect such a dome. The inner rim of Selk crater is fluted, probably by eolian erosion, while the outer flank and presumed ejecta blanket appear dissected by drainages (particularly to the east), likely the result of fluvial erosion. Terracing is observed on the northern and western walls of Selk crater within a 10-15 km wide terrace zone identified in VIMS data; the terrace zone is bright in SAR data, consistent with it being a rough surface. The terrace zone is slightly wider than those observed on Ganymede and Callisto and may reflect differences in thermal structure and/or composition of the lithosphere. The polygonal appearance of the crater likely results from two preexisting planes of weakness (oriented at azimuths of 21° and 122° east of north). A unit of generally bright terrain that exhibits similar infrared-color variation and contrast to Selk crater extends east-southeast from the crater several hundred kilometers. We informally refer to this terrain as the Selk “bench.” Both Selk and the bench are surrounded by the infrared-dark Belet dune field. Hypotheses for the genesis of the optically bright terrain of the bench include: wind shadowing in the lee of Selk crater preventing the encroachment of dunes, impact-induced cryovolcanism, flow of a fluidized-ejecta blanket (similar to the bright crater outflows observed on Venus), and erosion of a streamlined upland formed in the lee of Selk crater by fluid flow. Vestigial circular outlines in this feature just east of Selk’s ejecta blanket suggest that this might be a remnant of an ancient, cratered crust. Evidently the southern margin of the feature has sufficient relief to prevent the encroachment of dunes from the Belet dune field. We conclude that this feature either represents a relatively high-viscosity, fluidized-ejecta flow (a class intermediate to ejecta blankets and long venusian-style ejecta flows) or a streamlined upland remnant that formed downstream from the crater by erosive fluid flow from the west-northwest.     

Zum mittleren Kluftabstand aus der Anzahl von Kluftanschnittlinien

ZusammenfassungZum mittleren Kluftabstand aus der Anzahl von Kluftschnittlinien Der mittlere Kluftabstand wird anhand von zwei Methoden bestimmt: In der ersten Methode werden Kluftgefüge typisiert und durch drei senkrecht aufeinanderstehende Kluftscharen approximiert. Von diesen drei Kluftscharen wie dem gesamten Kluftgefüge wird der mittlere Kluftabstand ermittelt. Je nach Gefügetyp stellt der mittlere Kluftkörper einen Quader, ein Prisma mit quadratischer Grundfläche oder einen Würfel dar. Gemessen wird die Anzahl von Kluftanschnittlinien bzw. Sehnen entlang von Meßgeraden, die parallel zu Gefügekoordinaten orientiert werden.Die zweite Methode ermöglicht, den Kluftabstand vonn Kluftscharen festzustellen. Meßgrößen sind wiederum die Anzahl von Kluftanschnittlinien und außerdem die Raumstellung der Klüfte. Die Meßgeraden können beliebig orientiert sein.Dazu werden die Gleichungen für den mittleren Kluftabstand hergeleitet. An einem Verwitterungsprofil eines oberdevonischen Siltsteines werden beide Methoden getestet.

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SummaryAbout the Mean Joint Spacing from the Number of Dissecting Lines Between Joints and Rock Faces The mean joint spacing is determined by two methods: The first method typifies the fabric and approximates the joints by three orthogonally sets of joints. The mean joint spacing is determined by these sets of joints as well as by the entire fabric of the joints. Depending upon the fabric type the mean rock block defined by joints is a rectangular parallelepiped, a prism with a quadratic basal surface or a cube. The number of dissecting lines between joints or chords are measured along secants, which are parallel to fabric coordinates. The second method allows to determine the spacing ofn shares of joints. Measuring units are once again the number of dissecting lines between joints and moreover the position in space of the joints. The orientation of the measuring secants may be at random.In addition to this equations are derived for the mean joint spacing. A weathering profile of Upper Devonian siltstone is used to test both methods.

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RésuméDistance de failles moyenne établie par le nombre des lignes de failles coupées La distance de failles moyenne se détermine à l'aide de deux méthodes: La première méthode sert à typiser les textures de failles et à rapprocher ces textures par trois séries de cassures orthogonales. Pour chacune de ces trois séries de cassures aussi bien que pour la texture de failles intégrale on établit la distance de failles moyenne. Selon le type de texture, le polyèdre moyen représente un parallélépipède orthogonal, un prisme à base quadratique ou un cube. On mesure le nombre des lignes de failles coupées respectivement des cordes le long des lignes de mesures qui se trouvent en relation avec les coordonnées de texture. La seconde méthode permet à déterminer la distance de failles den séries de cassures. Les quantités de mesure sont de nouveau le nombre des lignes de failles coupées et plus l'orientation des failles. Les lignes de mesure peuvent être orientées de manière quelconque.En outre on déduit les équations pour la distance de failles moyenne. On met à l'épreuve ces deux méthodes à l'exemple d'un profil de désagrégation dans le schiste argileux du Dévonien supérieur.

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Mit 12 Abbildungen     

The record of historic earthquakes in lake sediments of Central Switzerland

Deformation structures in lake sediments in Central Switzerland can be attributed to strong historic earthquakes. The type and spatial distribution of the deformation structures reflect the historically documented macroseismic intensities thus providing a useful calibration tool for paleoseismic investigations in prehistoric lake sediments.The Swiss historical earthquake catalogue shows four moderate to strong earthquakes with moment magnitudes of M_w=5.7 to M_w=6.9 and epicentral intensities of I₀=VII to I₀=IX that affected the area of Central Switzerland during the last 1000 years. These are the 1964 Alpnach, 1774 Altdorf, 1601 Unterwalden, and 1356 Basel earthquakes. In order to understand the effect of these earthquakes on lacustrine sediments, four lakes in Central Switzerland (Sarner See, Lungerer See, Baldegger See, and Seelisberg Seeli) were investigated using high-resolution seismic data and sediment cores. The sediments consist of organic- and carbonate-rich clayey to sandy silts that display fine bedding on the centimeter to millimeter scale. The sediments are dated by historic climate and environmental records, ¹³⁷Cs activity, and radiocarbon ages. Deformation structures occur within distinct zones and include large-scale slumps and rockfalls, as well as small-scale features like disturbed and contorted lamination and liquefaction structures. These deformations are attributed to three of the abovementioned earthquakes. The spatial distribution of deformation structures in the different lakes clearly reflects the historical macroseismic dataset: Lake sediments are only affected if they are situated within an area that underwent groundshaking not smaller than intensity VI to VII. We estimate earthquake size by relating the epicentral distance of the farthest liquefaction structure to earthquake magnitude. This relationship is in agreement with earthquake size estimations based on the historical dataset.