Automated determination of the orientation of dust devil tracks in mars orbiter images

The paper presents and evaluates three methods for automatically estimating the main orientation of Martian dust devil tracks in MOC and HiRISE images. Inferring such information about dust devils from their tracks is important to better understand the near surface wind. The methods considered were based on gradient direction, directional openings and morphological granulometry. The accuracy of the methods was asserted by comparing the results to a set of directions estimated visually and assumed to be the ground truth. The higher accuracy was reached using directional openings. Besides, the directions inferred by this method were compared to those predicted by the GCM and the results agreed. © 2013 COSPAR.

Detecção de Crateras de Impacto em Imagens Digitais. Estudo de caso: Superfície de Marte

Coordenação de Aperfeiçoamento de Pessoal de Nível Superior (CAPES)

Detecção automática de rastros de Dust Devils na superfície de Marte

Conselho Nacional de Desenvolvimento Científico e Tecnológico (CNPq)

A zona de contato entre as formações Motuca e Sambaíba, Permo-Triássico da bacia do Parnaíba, regiões de Filadélfia (TO), Riachão (MA) e Loreto (MA)

O intervalo que compreende o final do Paleozóico e início do Mesozóico foi marcado por mudanças globais paleogeográficas e paleoclimáticas, em parte atribuídas a eventos catastróficos. A intensa continentalização do supercontinente Pangéia, com a implantação de extensos desertos, sucedeu os ambientes costeiros-plataformais do início do Permiano. Os registros desses eventos no norte do Brasil são encontrados nas bacias intracratônicas, particularmente na Bacia do Parnaíba, representados pela zona de contato entre as formações Motuca e Sambaíba. A Formação Motuca é constituída predominantemente por pelitos vermelhos laminados com lentes de gipsita, calcita e marga. Na porção leste da Bacia do Parnaíba, as fácies da Formação Motuca tornam-se mais arenosas com a ocorrência expressiva de arenitos com estratificação cruzada sigmoidal. A Formação Sambaíba consiste em arenitos de coloração creme alaranjada com estratificação plano-paralela e estratificação cruzada de médio a grande porte. Em geral, o contato entre as unidades é brusco, representado pela passagem de arenitos finos com laminação cruzada cavalgante e acamamento flaser/wavy da Formação Motuca para arenitos médios com falhas/microfalhas sinsedimentares e laminações convolutas da Formação Sambaíba. Foram individualizadas 14 fácies sedimentares, agrupadas em quatro associações: AF1 – Lacustre raso / Planície de lama (mudflat), AF2 – “Panela” salina (saline pan), AF3 – Lençol de areia e AF4 – Campo de dunas. A AF1 foi depositada dominantemente por processos de decantação em um extenso ambiente lacustre raso de baixa energia, influenciado por influxos esporádicos de areias oriundos de rios efêmeros. Este sistema lacustre foi, provavelmente, influenciado por períodos de contração e expansão, devido às variações das condições climáticas predominantemente áridas. Os mais expressivos períodos de contração ocorreram na porção oeste da Bacia do Parnaíba, representados pelo desenvolvimento de planícies de lama (mudflats) associadas a lagoas efêmeras saturadas em carbonatos e a “panelas” salinas (saline pans- AF2). Os lençóis de areia (AF3) são planícies arenosas extensas, localmente com área úmidas, intensamente retrabalhadas por processos eólicos. A AF4 é interpretada como parte de um erg composto por dunas/draas em zona saturada em areia, com interdunas secas subordinadas. Intervalos deformados lateralmente contínuos por centenas de quilômetros ocorrem na zona de contato entre as formações Motuca e Sambaíba. Pelitos com camadas contorcidas e brechadas (Formação Motuca) e arenitos com falhas/microfalhas sinsedimentares, laminação convoluta e diques de injeção preenchidos por argilitos (Formação Sambaíba) são interpretados como sismitos induzidos por terremotos de alta magnitude (>8 na escala Ritcher). Anomalias geoquímicas de elementos traços como Mn, Cr, Co, Cu e Ni na zona de contato entre as formações, juntamente com a presença de micropartículas de composição metálica na matriz argilosa dos sismitos, corroboram com impactos de meteoritos no limite c, possivelmente do astroblema Riachão.

Detecção automática e análise temporal de slope streaks na superfície de Marte

Coordenação de Aperfeiçoamento de Pessoal de Nível Superior (CAPES)

Book Review of Stone by Stone: Exploring Ancient Sites on the Canadian Plains by Liz Bryan

Liz Bryan begins her book with a description of the Canadian Plains:" . .. a voluptuous landscape of hills and valleys and plains, of lakes and tiny twinkling potholes, of flower-filled coulees and vast sand dunes." Her emphasis throughout on the landscape of southern Saskatchewan and Alberta is necessary since the ancient monuments she describes only truly resonate within this setting. Indeed, almost every page of this attractive book is adorned with at least two color images-of scenery, stone features, artifacts, and aboriginal events. She then proceeds to an eclectic overview of the archaeological record of the Plains of Saskatchewan and Alberta, including the earliest human evidence, such as the Clovis points from the Wally's Beach site, Alberta, where the trackways of mammoths, camels, and muskoxen were miraculously and briefly exposed in the late 1990s. There is one perplexing error, however-the attribution of the extinction of the ice age bestiary, about 12,000 years ago, to the meteorite that felled the dinosaurs!

Insights into the morphology of the Serra da Cangalha impact structure from geophysical modeling

Forward modeling is commonly applied to gravity field data of impact structures to determine the main gravity anomaly sources. In this context, we have developed 2.5-D gravity models of the Serra da Cangalha impact structure for the purpose of investigating geological bodies/structures underneath the crater. Interpretation of the models was supported by ground magnetic data acquired along profiles, as well as by high resolution aeromagnetic data. Ground magnetic data reveal the presence of short-wavelength anomalies probably related to shallow magnetic sources that could have been emplaced during the cratering process. Aeromagnetic data show that the basement underneath the crater occurs at an average depth of about 1.9 km, whereas in the region beneath the central uplift it is raised to 0.51 km below the current surface. These depths are also supported by 2.5-D gravity models showing a gentle relief for the basement beneath the central uplift area. Geophysical data were used to provide further constraints for numeral modeling of crater formation that provided important information on the structural modification that affected the rocks underneath the crater, as well as on shock-induced modifications of target rocks. The results showed that the morphology is consistent with the current observations of the crater and that Serra da Cangalha was formed by a meteorite of approximately 1.4 km diameter striking at 12 km s-1.

Edelgase in Enstatit-Chondriten

Zusammenfassung - Die vorliegende Dissertation beschreibt die massenspektrometrische Bestimmung der Edelgaskonzentrationen und -isotopenverhältnisse von insgesamt 47 Enstatit-Chondriten (E-Chondriten). E-Chondrite bilden eine Meteoritengruppe, die sich durch einen hohen Reduktionsgrad auszeichnet. Es gibt Hinweise darauf, dass sie im inneren Bereich des Sonnensystems entstanden. Ihre chemischen und mineralogischen Eigenschaften können daher auch Aufschluss über die Genese der terrestrischen Planeten geben. Die Edelgasmessungen hatten im wesentlichen die Berechnung von Bestrahlungsaltern sowie die Untersuchung der getrappten Edelgaskomponenten zum Ziel. Die Bestrahlungsalter der E-Chondrite liegen zwischen 0.5 und 50 Millionen Jahren. Eine zweifelsfreie Aussage über Häufungen in der Altersverteilung, die auf große Impaktereignisse auf dem Mutterkörper hinweisen könnten, lässt sich aufgrund der relativ hohen Unsicherheit der Alter (20 Prozent) nicht treffen.Etwa 10 Prozent der E-Chondrite enthalten signifikante solare Gasanteile. Alle zählen zum nicht-equilibrierten petrologischen Typ 3.In der elementaren Zusammensetzung der getrappten schweren Edelgase fällt auf, dass EH3-Chondrite (H für high iron) vorrangig ein stärker fraktioniertes (planetares), relativ Ar-armes Edelgasmuster aufweisen, während alle übrigen Typen E4-6 von einer sog. subsolaren, relativ Ar-reichen Signatur dominiert werden. Diese Verteilung und Zusammensetzung lassen sich nicht ohne weiteres mit dem Modell zur Entstehung der petrologischen Typen durch Metamorphose, wie es für die gewöhnlichen Chondrite formuliert wurde, erklären.

Weathering of Fe-bearing minerals under extraterrestrial conditions, investigated by Mössbauer spectroscopy

The weathering of Fe-bearing minerals under extraterrestrial conditions was investigated by Mössbauer (MB) spectroscopy to gain insights into the role of water on the planet Mars. The NASA Mars Exploration Rovers Spirit and Opportunity each carry a miniaturized Mössbauer spectrometer MIMOS II for the in situ investigation of Martian soils and rocks as part of their payload. The MER flight instruments had to be modified in order to work over the Martian diurnal temperature range (180 K – 290 K) and within the unique electronic environment of the rovers. The modification required special calibration procedures. The integration time necessary to obtain a good quality Mössbauer spectrum with the MIMOS II flight instruments was reduced by 30 % through the design of a new collimator. The in situ investigation of rocks along the rover Spirit's traverse in Gusev crater revealed weakly altered olivine basalt on the plains and pervasively altered basalt in the Columbia Hills. Correlation plots of primary Fe-bearing minerals identified by MB spectroscopy such as olivine versus secondary Fe-bearing phases such as nanophase Fe oxides showed that olivine is the mineral which is primarily involved in weathering reactions. This argues for a reduced availability of water. Identification of the Fe-oxyhydroxide goethite in the Columbia Hills is unequivocal evidence for aqueous weathering processes in the Columbia Hills. Experiments in which mineral powders were exposed to components of the Martian atmosphere showed that interaction with the atmosphere alone, in the absence of liquid water, is sufficient to oxidize Martian surface materials. The fine-grained dust suspended in the Martian atmosphere may have been altered solely by gas-solid reactions. Fresh and altered specimens of Martian meteorites were investigated with MIMOS II. The study of Martian meteorites in the lab helped to identify in Bounce Rock the first rock on Mars which is similar in composition to basaltic shergottites, a subgroup of the Martian meteorites. The field of astrobiology includes the study of the origin, evolution and distribution of life in the universe. Water is a prerequisite for life. The MER Mössbauer spectrometers identified aqueous minerals such as jarosite and goethite. The identification of jarosite was crucial to evaluate the habitability of Opportunity's landing site at Meridiani Planum during the formation of the sedimentary outcrop rocks, because jarosite puts strong constrains on pH levels. The identification of olivine in rocks and soils on the Gusev crater plains provide evidence for the sparsity of water under current conditions on Mars. Ratios of Fe2+/Fe3+ were obtained with Mössbauer spectroscopy from basaltic glass samples which were exposed at a deep sea hydrothermal vent. The ratios were used as a measure of potential energy for use by a microbial community. Samples from Mars analogue field sites on Earth exhibiting morphological biosignatures were also investigated.

Carbonate conical mounds of the eastern Anti-Atlas(Morocco) and their relationship with potential analogues on Mars

Longstanding debates concerning the origin of the Kess Kess Emsian carbonate mounds exposed at Hamar Laghdad Ridge (eastern Anti-Atlas, Morocco) centre around the processes that induced precipitation of carbonate mud and the preservation of steep morphologies. Although in the last years an origin related to hydrothermalism seemed to be more likely, to date the Kess Kess are still considered controversial vent deposits. This study combines in updated research review information from previous work and new detailed field observations coupled with new analytical results to define a consistent framework and some new insight of current knowledge about the origin of these mounds. We obtain a complete minero-petrographic and palaeobiological data set and a detailed geochemical characterization of the different lithologies and facies of the Hamar Laghdad stratigraphic succession, including mounds, and we compared the results with the data from Maïder Basin mounds (Anti-Atlas, Morocco). Our data support the hydrothermal model proposed for the genesis and development of the Kess Kess mounds. The mechanisms linked to the mounds formation and growth are discussed in the light of the new finding of fluid-sediment interaction within a scenario driven by late magmatic fluids circulation. Conical mounds and other fluids related morphologies were also reported from Crommelin crater area (Arabia Terra, Mars). These mounds consist in meter-sized conical buildups hosted in the Equatorial Layered Deposits (ELDs) deposed during a regional groundwater fluid upwelling. Geometries and geological conditions that might have controlled the development of such morphologies were discussed. According to our data the morphological and stratigraphical characteristics of Crommelin area mounds are most consistent with a formation by fluids advection. Then we compare terrestrial and Martian data and examine the geological settings of hydrothermal mound occurrences on Earth in order to describe potential target areas for hydrothermal structures on Mars.

Strukturelle, chemische und isotopische Analysen nanoskaliger präsolarer und früher solarer Kondensate

Neben astronomischen Beobachtungen mittels boden- und satellitengestützer Instrumente existiert ein weiterer experimenteller Zugang zu astrophysikalischen Fragestellungen in Form einer Auswahl extraterrestrischen Materials, das für Laboruntersuchungen zur Verfügung steht. Hierzu zählen interplanetare Staubpartikel, Proben, die von Raumfahrzeugen zur Erde zurückgebracht wurden und primitive Meteorite. Von besonderem Interesse sind sog. primitive kohlige Chondrite, eine Klasse von Meteoriten, die seit ihrer Entstehung im frühen Sonnensystem kaum verändert wurden. Sie enthalten neben frühem solarem Material präsolare Minerale, die in Sternwinden von Supernovae und roten Riesensternen kondensiert sind und die Bildung unseres Sonnensystems weitgehend unverändert überstanden haben. Strukturelle, chemische und isotopische Analysen dieser Proben besitzen demnach eine große Relevanz für eine Vielzahl astrophysikalischer Forschungsgebiete. Im Rahmen der vorliegenden Arbeit wurden Laboranalysen mittels modernster physikalischer Methoden an Bestandteilen primitiver Meteorite durchgeführt. Aufgrund der Vielfalt der zu untersuchenden Eigenschaften und der geringen Größen der analysierten Partikel zwischen wenigen Nanometern und einigen Mikrometern mussten hierbei hohe Anforderungen an Nachweiseffizienz und Ortsauflösung gestellt werden. Durch die Kombination verschiedener Methoden wurde ein neuer methodologischer Ansatz zur Analyse präsolarer Minerale (beispielsweise SiC) entwickelt. Aufgrund geringer Mengen verfügbaren Materials basiert dieses Konzept auf der parallelen nichtdestruktiven Vorcharakterisierung einer Vielzahl präsolarer Partikel im Hinblick auf ihren Gehalt diagnostischer Spurenelemente. Eine anschließende massenspektrometrische Untersuchung identifizierter Partikel mit hohen Konzentrationen interessanter Elemente ist in der Lage, Informationen zu nukleosynthetischen Bedingungen in ihren stellaren Quellen zu liefern. Weiterhin wurden Analysen meteoritischer Nanodiamanten durchgeführt, deren geringe Größen von wenigen Nanometern zu stark modifizierten Festkörpereigenschaften führen. Im Rahmen dieser Arbeit wurde eine quantitative Beschreibung von Quanteneinschluss-Effekten entwickelt, wie sie in diesen größenverteilten Halbleiter-Nanopartikeln auftreten. Die abgeleiteten Ergebnisse besitzen Relevanz für nanotechnologische Forschungen. Den Kern der vorliegenden Arbeit bilden Untersuchungen an frühen solaren Partikeln, sog. refraktären Metall Nuggets (RMN). Mit Hilfe struktureller, chemischer und isotopischer Analysen, sowie dem Vergleich der Ergebnisse mit thermodynamischen Rechnungen, konnte zum ersten Mal ein direkter Nachweis von Kondensationsprozessen im frühen solaren Nebel erbracht werden. Die analysierten RMN gehören zu den ersten Festkörperkondensaten, die im frühen Sonnensystem gebildet wurden und scheinen seit ihrer Entstehung nicht durch sekundäre Prozesse verändert worden zu sein. Weiterhin konnte erstmals die Abkühlrate des Gases des lokalen solaren Nebels, in dem die ersten Kondensationsprozesse stattfanden, zu 0.5 K/Jahr bestimmt werden, wodurch ein detaillierter Blick in die thermodynamische Geschichte des frühen Sonnensystems möglich wird. Die extrahierten Parameter haben weitreichende Auswirkungen auf die Modelle der Entstehung erster solarer Festkörper, welche die Grundbausteine der Planetenbildung darstellen.

Diversity of lithologic components at Meridiani Planum, Mars: Insights from Mössbauer spectroscopic investigations

The two Mars Exploration Rovers (MER), Spirit and Opportunity, landed on the Martian surface in January 2004 and have since collected a wealth of information about their landing sites. As part of their payload, the miniaturised Mössbauer spectrometer MIMOS II contributes to the success of the mission by identifying Iron-bearing minerals and by determining Iron oxidation states in them. The basis of this work is the data set obtained at Opportunity’s landing site at Meridiani Planum. A portion of this data set is evaluated with different methods, with the aim to thoroughly characterize lithologic components at Meridiani Planum and possible relations between them.rnMIMOS II is able to measure Mössbauer spectra at different energies simultaneously, bearing information from different sampling depths of the investigated target. The ability of depth-selective Mössbauer spectroscopy to characterize weathered surface layers is illustrated through its application to two suitable rock targets that were investigated on Mars. In both cases, an enhanced concentration of Iron oxides at the rock surface was detected, pointing to a low degree of aqueous alteration. rnThe mineral hematite (α-Fe2O3) is present in the matrix of outcrop rocks and in spherules weathering from the outcrop. Simultaneous fitting of Mössbauer spectra was applied to data sets obtained on both target types to characterize the hematite component in detail. This approach reveals that two hematite populations are present, both in the outcrop matrix as well as in spherules. The hematite component with a comparably high degree of crystallinity and/or chemical purity is present in the outcrop matrix. The investigation of hematite at Meridiani Planum has shown that simultaneous fitting is a suitable and useful method to evaluate a large, correlated set of Mössbauer spectra.rnOpportunity encountered loose, cm-sized rocks along its traverse. Based on their composition and texture, these “cobbles” can be divided into three different groups. Outcrop fragments are impact-derived ejecta from local outcrop rocks. Cobbles of meteoritic origin contain the minerals kamacite (Fe,Ni) and troilite (FeS) and exhibit high Ni contents. Melt-bearing impact breccias bear similarities to local outcrop rocks and basaltic soil, with a phase composition and texture consistent with a formation scenario involving partial melting and inclusion of small, bright outcrop clasts. rnIron meteorites on the Martian surface experience weathering through the presence of even trace amounts of water due to their metallic nature. Opportunity encountered and investigated four Iron meteorites, which exhibit evidence for physical and chemical weathering. Discontinuous coatings contain Iron oxides, pointing to the influence of limited amounts of water. rnA terrestrial analogue site for Meridiani Planum is the Rio Tinto basin in south-west Spain. With its deposits of sulfate- and iron-oxide-bearing minerals, the region provides an adequate test bed for instrumentation for future Mars missions. In-situ investigations at Rio Tinto were carried out with a special focus on the combined use of Mössbauer spectroscopy with MIMOS II and Raman spectroscopy with a field-portable instrument. The results demonstrate that the two instruments provide complementary information about investigated samples.

Extraktion und nanoanalytische Charakterisierung refraktärer Nanometallpartikel frühester solarer Materie und Synthese metallischer Nanopartikel aus dotierten Ca-Mg-Al-Si-Schmelzen

Primitive kohlige Chondrite sind Meteorite, die seit ihrer Entstehung im frühen Sonnensystem kaum verändert wurden und dadurch einen Einblick in Prozesse geben, die zur Bildung und Veränderung der ersten festen Materie führten. Solche Prozesse können anhand von Bruchstücken dieser Meteorite detailliert im Labor studiert werden, sodass Rückschlüsse auf die Entwicklung unseres Sonnensystems im frühen Stadium getroffen werden können. Ca-, Al-reiche Einschlüsse (CAIs) aus chondritischen Meteoriten sind die ersten Festkörper des Sonnensystems und enthalten viele refraktäre Metallnuggets (RMNs), welche hauptsächlich aus den Elementen Os, Ir, Ru, Mo und Pt bestehen. Nach weit verbreiteter Ansicht sind diese Nuggets wahrscheinlich im Gleichgewicht mit dem solaren Nebel kondensiert, bereits früher oder gleichzeitig mit Oxiden und Silikaten. Die exakten Mechanismen, die zu ihren heute beobachteten Eigenschaften führten, sind allerdings unklar. Um frühere Arbeiten fortzuführen, wurde eine hohe Anzahl RMNs in vier unterschiedlichen Typen von Meteoriten detailliert studiert, darunter solche aus dem nahezu unveränderten Acfer 094, Allende (CV3ox), Leoville (CV3red) und Murchison (CM2). Die RMNs wurden in-situ, assoziiert mit ihren Wirtsmineralen und auch in Säurerückständen gefunden, deren Präparationsprozedur in dieser Arbeit speziell für RMNs durch eine zusätzliche Dichtetrennung verbessert wurde.rnDie Ergebnisse decken eine Reihe von Ungereimtheiten zwischen den beobachteten RMN-Eigenschaften und einer Kondensationsherkunft auf, sowohl für Kondensation in solarer Umgebung, als auch für Kondensation aus Material von Supernovae oder roten Riesen, für die die Kondensationssequenzen refraktärer Metalle speziell für diesen Vergleich berechnet wurden. Stattdessen wurden in dieser Arbeit neue Einblicke in die RMN-Entstehung und die Entwicklung der ersten Festkörper (CAIs) durch eine Kombination aus experimentellen, isotopischen, strukturellen und petrologischen Studien an RMNs gewonnen. Viele der beobachteten Eigenschaften sind mit Ausfällung der RMN aus einer CAI-Schmelze vereinbar. Ein solches Szenario wird durch entsprechende Untersuchungen an synthetisch hergestellten, mit refraktären Metallen im Gleichgewicht stehenden CAI-Schmelzen bestätigt. Es folgt aus den Ergebnissen, dass die Mehrzahl der RMNs isotopisch solar ist und alle untersuchten RMNs innerhalb von CAIs bei rascher Abkühlung (um bis zu 1000 °C/40 sek.) einer CAI-Schmelze gebildet wurden. rn

Analisi di morfologie carsiche o crio-carsiche in relazione alla mobilizzazione di fluidi nella regione di Arabia Terra, Marte.

This thesis tries to interpret the origin and evolution of karst-like forms present in Arabia Terra, a region of Mars that develops in the equatorial zone of the planet. The work has been carried out specifically in the craters Crommelin (4o 91’ N-10o 51’ E), 12000088 (3o 48’ N-1o 30’ E), NE 12000088 (4° 20’ N-2° 50’ E), C "2" (3° 54’ N-1° W), and in their surrounding areas. These craters contain layered deposits characterized by a high albedo and on which erosion is very pronounced. The area containing the craters is a plateau that has the same characteristics of albedo and texture. The preliminary morphological study has made use of instrumentation such as the Mars Reconnaissance Orbiter (MRO), in particular HiRISE images (High Resolution Imaging Science Experiment), CTX (Context Camera) and CRISM (Compact Reconnaissance Imaging Spectrometers for Mars). A regional geomorphological map has been drawn up containing the main morphotypes, and detailed geomorphological maps were prepared for different karst-like morphologies. The analysis of spectral data collected from CRISM instrumentation has allowed to identify the footprint of sulphate minerals in the external area. Data were collected for morphometric negative forms (karst-like) and positive forms (mud volcanoes, dikes and pingos). For the analysis of the relief forms DTMs (Digital Terrain Models) produced by the union of stereographic CTX couples or HiRISE were used. From the analysis of high-resolution images morphological footprints similar to periglacial environments have been identified, including the presence of patterned ground and polygonal cracks found all over the area of investigation, and relief structures similar to pingos present in the crater C "2". These observations allow us to imagine a geological past with a cold climate at the equator able to freeze the few fluids present in the Martian arid terrain. The development of karst-like landforms, on the other hand, can be attributed to a subsequent improval of the weather conditions that led to a normal climate regime for the equatorial areas, resulting in the degradation of the permafrost. The melt waters have thus allowed the partial dissolution of the sulphate layers. The karst-like forms look rather fresh suggesting them to be not that old.