Sedimentary evolution of an active margin during middle and upper cretaceous times: the north Peruvian margin from late aptian up to senonian

The sedimentary evolution of the North Peruvian margin during upper Cretaceous can be summarized as follows:The upper Aptian transgression involved the whole margin, and was accompanied by minor, local, synsedimentary tectonic features. It could be coeval with the individualization of the Western ensialic marginal basin. The transgression reached its maximum during middle Albian, and is associated with anoxic deposits, and with the main activity of the marginal basin.A regression followed during the upper Albian. It was materialized during lower Cenomanian by intertidal deposits, by a westward deltaic progradation, and by synsedimentary tectonic features. This regressive maximum is correlatable with the tectonic closure and folding of the western marginal basin.Then, the great upper Cretaceous transgression affected the eastern parts of the margin. Major deepening stages occured during late Middle Cenomanian and at the base of the Turonian. During Turonian, a widespread, calm carbonate shelf developed. A new major transgressive pulse occured at the Turonian-Coniacian boundary. As a result of a general uplift, the whole margin emerged diachronically between Santonian and Campanian, leading to the deposition of continental Red Beds. The latter recorded a new tectonic phase of uppermost Senonian age.During upper Cretaceous times, the sedimentary evolution of the North Peruvian margin appears to be controlled both by the eustatic sea-level changes, and by the uppermost Albian to early Cenomanian, and the upper Senonian tectonic events.

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Zusammenfassung Die sedimentäre Entwicklung des nordperuanischen Kontinentalrandes zeigt während der Ober-Kreide folgende Etappen: die Transgression des Oberaptes erstreckt sich über den gesamten Kontinentalrand und geht mit leichten synsedimentären tektonischen Diskonformitäten einher, die gleichzeitig mit der Entstehung des westlichen Randbeckens zu sehen sind. Die Transgression erreicht ihren Höhepunkt im mittleren Alb, sie ist verbunden mit anoxischen Ablagerungen und mit den Hauptbewegungen im randlichen Becken. Im Oberalb folgt eine Regression. Sie zeigt sich im unteren Cenoman durch intertidale Ablagerungen, durch nach Westen progradierende Deltas und durch synsedimentäre Tektonik. Der Höhepunkt der Regression ist verbunden mit der tektonischen Isolation und Faltung des westlichen Randbeckens.Die große Transgression während der Oberkreide beeinflußt vor allen Dingen die östlichen Teile des Randes. Wesentliche Eintiefungsphasen erscheinen im oberen Mittelcenoman und an der Basis des Turons. Während des Turons entwickelt sich ein weiter Karbonatschelf. Ein größerer Transgressionsvorstoß erscheint an der Grenze von Turon zu Coniac. Als Ergebnis einer generellen Heraushebung wird der gesamte Kontinentrand diachron zwischen Santon und Campan herausgehoben und es entstehen kontinentale Rotablagerungen. Diese Sedimente dokumentieren eine neue tektonische Phase im obersten Senon. Während der Oberkreide wird die sedimentäre Weiterentwicklung des nordperuanischen Kontinentalrandes durch globale Meeresspiegelschwankungen zusammen mit tektonischen Ereignissen (Oberapt, Oberalb-unteres Cenoman, Senon und oberstes Senon) kontrolliert.

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Résumé L'évolution sédimentaire de la marge nord-péruvienne au Crétacé supérieur peut être résumée ainsi:La transgression de l'Aptien supérieur affecte toute la marge, et s'accompagne d'une légère instabilité tectonique localisée. Celle-ci peut être contemporaine de l'individualisation du bassin marginal occidental. La transgression atteint son maximum à l'Albien moyen. Elle est contemporaine de dépôts anoxiques et de l'activité du bassin marginal.Une régression survient au cours de l'Albien supérieur. Elle se matérialise au Cénomanien inférieur par l'installation d'une plate-forme carbonatée, puis par la progradation du delta oriental et par des mouvements tectoniques synsédimentaires. Cette régression est en relation avec la fermeture du bassin marginal occidental.La grande transgression du Crétacé supérieur affecte ensuite les zones orientales de la marge, les étapes majeures d'approfondissement se situant à la fin du Cénomanien moyen et à la base du Turonien. Au Turonien, une vaste plate-forme carbonatée s'installe, et un nouvel approfondissement survient à la limite Turonien-Coniacien. A la suite d'une surrection générale, la marge émerge de façon diachrone entre le Santonien et le Campanien, donnant lieu au dépôt des Couches Rouges continentales qui enregistrent au Sénonien terminal un nouvel événement tectonique.Au Crétacé supérieur, l'evolution sédimentaire de la marge nord-péruvienne semble donc contrôlée à la fois par les variations eustatiques, et par les événements tectoniques de l'Albien terminal-Cénomanien inférieur, et du Sénonien.

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The Relegation Algorithm

The relegation algorithm extends the method of normalization by Lie transformations. Given a Hamiltonian that is a power series = ₀+ ₁+ ... of a small parameter , normalization constructs a map which converts the principal part ₀into an integral of the transformed system — relegation does the same for an arbitrary function [G]. If the Lie derivative induced by [G] is semi-simple, a double recursion produces the generator of the relegating transformation. The relegation algorithm is illustrated with an elementary example borrowed from galactic dynamics; the exercise serves as a standard against which to test software implementations. Relegation is also applied to the more substantial example of a Keplerian system perturbed by radiation pressure emanating from a rotating source.This revised version was published online in October 2005 with corrections to the Cover Date.     

Distribuzione geografica dell'attivita' magnetica terrestre

Riassunto Richiamate le caratteristiche secondo cui le perturbazioni regolari ed irregolari del campo terrestre concorrono a definire l'attività geomagnetica, se ne analizza la distribuzione geografica mediante le grandezze:HR _H ,ZR _Z , e (10^–4.²). Di queste sono illustrati e discussi gli andamenti in funzione della latitudine geomagnetica, dedotti dai valori medi calcolati per quasi tutte le stazioni funzionanti durante l'Anno Polare 1932–33 ed il triennio successivo 1933–36. Si rileva particolarmente il massimo assoluto di attività della zone anulare delle aurore, e quello relativo delle regioni equatoriali. Segue un'indagine, a carattere piuttosto indicativo, sulla ripartizione geografica del grado di variazione dell'attività nel tempo, introducendo a tale scopo opportuni indici ed esponendone il comportamento. Conclude la Nota un cenno sugli andamenti stagionali dell'attività e della variabilità geomagnetica.     

BEEKEEPING AND LOCAL SELF-RELIANCE IN RURAL SOUTHERN AFRICA*

ABSTRACT. Beekeeping has the potential to supplement incomes in rural southern Africa. In light of regional economic constraints, self-reliance strategies that draw on local knowledge and skills take on a renewed importance. We consider the advantages and disadvantages of beekeeping and examine appropriate forms of development support. A short case study from Zimbabwe illustrates these issues.     

Streamflow response to regional climate model output in the mountainous watershed: a case study from the Swiss Alps

Regional climate model (RCM) outputs are often used in hydrological modeling, in particular for streamflow forecasting. The heterogeneity of the meteorological variables such as precipitation, temperature, wind speed and solar radiation often limits the ability of the hydrological model performance. This paper assessed the sensitivity of RCM outputs from the PRUDENCE project and their performance in reproducing the streamflow. The soil and water assessment tool was used to simulate the streamflow of the Rhone River watershed located in the southwestern part of Switzerland, with the climate variables obtained from four RCMs. We analyzed the difference in magnitude of precipitation, maximum and minimum air temperature, and wind speed with respect to the observed values from the meteorological stations. In addition, we also focused on the impact of the grid resolution on model performance, by analyzing grids with resolutions of 50 × 50 and 25 × 25 km². The variability of the meteorological inputs from various RCMs is quite severe in the studied watershed. Among the four different RCMs, the Danish Meteorological Institute provided the best performance when simulating runoff. We found that temperature lapse rate is significantly important in the mountainous snow and glacier dominated watershed as compared to other variables like precipitation, and wind speed for hydrological performance. Therefore, emphasis should be given to minimum and maximum temperature in the bias correction studies for downscaling climatic data for impact modeling in the mountainous snow and glacier dominated complex watersheds.     

Magnetic horizons of UHECR sources and the GZK feature

We study the effect of random extra-galactic magnetic fields on the propagation of protons of energy larger than 10¹⁹ eV. We show that for reasonable field values (in the 100 nG range) the transition between diffusive and ballistic regimes occurs in the same energy range as the GZK cutoff (a few 10¹⁹ eV). The usual interpretation of the flux reduction above the GZK energy in terms of a sudden reduction of the visible horizon is modified. Moreover, since the size of the diffusion sphere of a continuous source of cosmic rays is of the order of 10 Mpc, the local structure of the Universe and, therefore, of potential local astrophysical sources plays a dominant role in the expected spectrum. Under reasonable assumptions on the sources configurations the expected GZK cutoff is reduced.     

小型激光天文动力学空间计划概念

小型激光天文动力学空间计划是 :使用在太阳轨道上无拖曳航天器和地面站以激光干涉和脉冲测距的方法 ,精确地探讨天文动力学 ,检测相对论与时空基本定律 ,改进探测引力波的灵敏度以及更准确地测定太阳、行星和小行星的参数。 1 969年开始的月球激光 (反射 )测距 ,对地球物理、参考坐标的选定、相对论的检验均有重要的贡献。 3 0年来 ,激光技术的长足进步 ,使现在正是适合于开始进行研究空间有源 (主动 )测距和光波空间通讯的时候。激光天文动力学的兴起是必然的趋势 ,其精确度将比现在提高 3到 6个数量级 ,将是天文动力学革命性的发展。小型激光天文动力学空间计划可以起到带头作用。它的关键技术有三 ,即 :弱光锁相、极精确无拖曳航天和高衰减日冕仪。弱光锁相已有长足的进步。对高衰减日冕仪的研究 ,也有了初步的方案。LISA空间计划将于 2 0 0 6年 8月发射SMART -2 ,研究测试极精确无拖曳航天。小型激光天文动力学空间计划的关键技术已日趋成熟。在第一届国际激光天文动力学研讨会 ( 2 0 0 1 ,9.1 3 -2 3 )中介绍了各相关学科背景及前沿研究 ,讨论了激光天文动力学空间计划科学目标及相关技术 ,并召开了两次小型激光天文动力学空间计划预研究筹备会 ,建立了和欧洲的合作关系。会后着手进行此项对基础     

Lander radioscience for obtaining the rotation and orientation of Mars

The paper presents the concept, the objectives, the approach used, and the expected performances and accuracies of a radioscience experiment based on a radio link between the Earth and the surface of Mars. This experiment involves radioscience equipment installed on a lander at the surface of Mars. The experiment with the generic name lander radioscience (LaRa) consists of an X-band transponder that has been designed to obtain, over at least one Martian year, two-way Doppler measurements from the radio link between the ExoMars lander and the Earth (ExoMars is an ESA mission to Mars due to launch in 2013). These Doppler measurements will be used to obtain Mars’ orientation in space and rotation (precession and nutations, and length-of-day variations). More specifically, the relative position of the lander on the surface of Mars with respect to the Earth ground stations allows reconstructing Mars’ time varying orientation and rotation in space.Precession will be determined with an accuracy better by a factor of 4 (better than the 0.1% level) with respect to the present-day accuracy after only a few months at the Martian surface. This precession determination will, in turn, improve the determination of the moment of inertia of the whole planet (mantle plus core) and the radius of the core: for a specific interior composition or even for a range of possible compositions, the core radius is expected to be determined with a precision decreasing to a few tens of kilometers.A fairly precise measurement of variations in the orientation of Mars’ spin axis will enable, in addition to the determination of the moment of inertia of the core, an even better determination of the size of the core via the core resonance in the nutation amplitudes. When the core is liquid, the free core nutation (FCN) resonance induces a change in the nutation amplitudes, with respect to their values for a solid planet, at the percent level in the large semi-annual prograde nutation amplitude and even more (a few percent, a few tens of percent or more, depending on the FCN period) for the retrograde ter-annual nutation amplitude. The resonance amplification depends on the size, moment of inertia, and flattening of the core. For a large core, the amplification can be very large, ensuring the detection of the FCN, and determination of the core moment of inertia.The measurement of variations in Mars’ rotation also determines variations of the angular momentum due to seasonal mass transfer between the atmosphere and ice caps. Observations even for a short period of 180 days at the surface of Mars will decrease the uncertainty by a factor of two with respect to the present knowledge of these quantities (at the 10% level).The ultimate objectives of the proposed experiment are to obtain information on Mars’ interior and on the sublimation/condensation of CO₂ in Mars’ atmosphere. Improved knowledge of the interior will help us to better understand the formation and evolution of Mars. Improved knowledge of the CO₂ sublimation/condensation cycle will enable better understanding of the circulation and dynamics of Mars’ atmosphere.     

The impact of dust on the scaling properties of galaxy clusters

We investigate the effect of dust on the scaling properties of galaxy clusters based on hydrodynamic N -body simulations of structure formation. We have simulated five dust models plus radiative cooling and adiabatic models using the same initial conditions for all runs. The numerical implementation of dust was based on the analytical computations of Montier & Giard. We set up dust simulations to cover different combinations of dust parameters that make evident the effects of size and abundance of dust grains. Comparing our radiative plus dust cooling runs with a purely radiative cooling simulation, we find that dust has an impact on cluster scaling relations. It mainly affects the normalization of the scalings (and their evolution), whereas it introduces no significant differences in their slopes. The strength of the effect critically depends on the dust abundance and grain size parameters as well as on the cluster scaling. Indeed, cooling due to dust is effective in the cluster regime and has a stronger effect on the 'baryon driven' statistical properties of clusters such as   L _X– M , Y – M , S – M   scaling relations. Major differences, relative to the radiative cooling model, are as high as 25 per cent for the   L _X– M   normalization, and about 10 per cent for the Y – M and S – M normalizations at redshift zero. On the other hand, we find that dust has almost no impact on the 'dark matter driven'   T _mw– M   scaling relation. The effects are found to be dependent in equal parts on both dust abundances and grain size distributions for the scalings investigated in this paper. Higher dust abundances and smaller grain sizes cause larger departures from the radiative cooling (i.e. with no dust) model.