Data analysis pipeline for EChO end-to-end simulations

Atmospheric spectroscopy of extrasolar planets is an intricate business. Atmospheric signatures typically require a photometric precision of 1×10^?4 in flux over several hours. Such precision demands high instrument stability as well as an understanding of stellar variability and an optimal data reduction and removal of systematic noise. In the context of the EChO mission concept, we here discuss the data reduction and analysis pipeline developed for the EChO end-to-end simulator EChOSim. We present and discuss the step by step procedures required in order to obtain the final exoplanetary spectrum from the EChOSim ‘raw data’ using a simulated observation of the secondary eclipse of the hot-Neptune 55 Cnc e.     

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.     

Globalization, industrial restructuring, and regional development in China

China's rapid growth and structural change since the reform in the late 1970s have generated many intriguing issues for scholarly research. This paper notices the drastic rise of China in foreign investment, export, and ICT production. Through a comprehensive review of the literature on globalization, industrial restructuring and regional development, this paper holds that the research on China is embedded in China's reform process, as well as theoretical development in economic geography. It highlights the important role of institutions and global-local interactions in industrial and regional development.     

Crustal thinning beneath the Rwenzori region, Albertine rift, Uganda, from receiver-function analysis

The Rwenzori mountains in western Uganda, with a maximum elevation of more than 5,000 m, are located within the Albertine rift valley. We have deployed a temporary seismic network on the Ugandan side of the mountain range to study the seismic velocity structure of the crust and upper mantle beneath this section of the rift. We present results from a receiver-function study revealing a simple crustal structure along the eastern rift flank with a more or less uniform crustal thickness of about 30 km. The complexity of inner-crustal structures increases drastically within the Rwenzori block. We apply different inversion techniques to obtain reliable results for the thickness of the crust. The observations expose a significantly thinner crust beneath the Rwenzori range with thickness values ranging from about 20–28 km beneath northern and central parts of the mountains. Our study therefore indicates the absence of a crustal root beneath the Rwenzori block. Beneath the Lake Edward and Lake George basins we detect the top of a layer of significantly reduced S-wave velocity at 15 km depth. This low-velocity layer may be attributed to the presence of partial melt beneath a region of recent volcanic activity.     

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     

A comparison of methods used to estimate the height of sand dunes on Mars

The collection of morphometric data on small-scale landforms from other planetary bodies is difficult. We assess four methods that can be used to estimate the height of aeolian dunes on Mars. These are (1) stereography, (2) slip face length, (3) profiling photoclinometry, and (4) Mars Orbiter Laser Altimeter (MOLA). Results show that there is good agreement among the methods when conditions are ideal. However, limitations inherent to each method inhibited their accurate application to all sites. Collectively, these techniques provide data on a range of morphometric parameters, some of which were not previously available for dunes on Mars. They include dune height, width, length, surface area, volume, and longitudinal and transverse profiles. The utilization of these methods will facilitate a more accurate analysis of aeolian dunes on Mars and enable comparison with dunes on other planetary surfaces.     

Sunglitter radiance modulation by internal waves

Summary Quantitative sunglitter radiance modulations at the ocean surface due to internal waves were calculated applying a simple first order theory. The results have been compared with the image data of internal wave signatures northeast of Nantucket Shoals off the coast of Massachusetts, U.S.A., taken by the Earth Terrain Camera (ETC) during the Skylab mission. The maximum magnitudes of sunglitter radiance modulations predicted by the theory are comparable to the satellite image data. The extreme values of calculated modulations depend only weakly on the wavelength of the internal wave signature. This is consistent with the analysed ETC data. On the other hand, the shapes of simulated and measured image intensity transects across an internal wave packet are different. This may possibly be explained by the assumed idealized sinusoidal type of thermocline used in the calculations. The theory predicts that sunglint signatures of internal waves are advected relative to positions of extreme slope regions of the thermocline due to currents.

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Strahldichtemodulation des Sonnenglitzerns durch interne Wellen

Zusammenfassung Quantitative Strahldichtemodulationen des Sonnenglitzerns an der Meeresoberfl?che durch interne Wellen werden unter Verwendung einer einfachen ersten Ordnungstheorie berechnet. Die Ergebnisse werden mit Bilddaten von internen Wellensignaturen nord?stlich von Nantucket Shoals vor der Küste von Massachusetts, U.S.A., verglichen, die w?hrend der Skylab-Mission von der Erdbeobachtungskamera (ETC) aufgenommen wurden. Die Werte der maximalen Strahldichtemodulation des Sonnenglitzerns, die von der Theorie vorhergesagt werden, sind mit den Satellitenbilddaten vergleichbar. Die Extremwerte der berechneten Modulationen h?ngen nur schwach von der Wellenl?nge der internen Wellensignaturen ab. Dieses stimmt mit den analysierten ETC Daten überein. Auf der anderen Seite sind die Kurvenverl?ufe zwischen den simulierten und gemessenen Bildintensit?tsprofilen entlang eines internen Wellenpaketes unterschiedlich. Dieses kann m?glicherweise durch den angenommenen idealisierten sinusf?rmigen Typ der Thermokline erkl?rt werden, der für die Berechnungen verwendet wurde. Die Theorie macht die Vorhersage, da? Signaturen des Sonnenglitzerns von internen Wellen durch Str?mungen advektiert werden relativ zu den Positionen der extremen Neigungsregionen der Thermokline.

     

Comparative aeronomy in the solar system

The coupled upper atmospheres, ionospheres and magnetospheres of the planets were the subject of a joint RAS–G/MIST discussion meeting hosted by the RAS on 10 January 2003, organized by Ingo Mueller-Wodarg and Emma Bunce . The scientific programme consisted of 10 presentations by speakers from the UK, France, USA and Australia.