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Identificação e interpretação de indícios morfológicos associados a ambientes fluviomarinhos em Marte
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Marte é o planeta telúrico do Sistema Solar mais semelhante ao Planeta Terra, devido à sua
história de formação, estrutura planetária, composição química e pelas características da sua
morfologia/geomorfologia presentes na sua superfície. Estas particularidades apontam para
que, algures no seu passado geológico, tenha detido condições para conservar um oceano no
estado líquido no seu hemisfério Norte.
Através de uma análise morfológica e estratigráfica, feita através de imagens com alta resolução
captadas por três instrumentos (HRSC; CTX e HiRISE) abordo de duas sondas (Mars Express
e Mars Recognaissence Orbiter) que orbitam Marte e modelos digitais do terreno gerados a partir
desses dados, analisou-se e interpretou-se a morfologia de um depósito sedimentar situado nas
margens ocidentais do complexo vulcânico de Tharsis, proveniente de um vale denominado de
Isara Valles. Este depósito é classificado na literatura como um sistema aluvionar/deltaico, e
nele podem ser observadas fortes evidências de que, para além de ter sido depositado na
interface de um curso de água corrente e um corpo de água salgada estável, o qual pode ser
considerado um oceano, este corpo de água gigantesco, seria dotado de características
dinâmicas similares ao seus análogo terrestres, como presença de ondas, correntes e
movimentos intermitentes similares ao das marés, desencadeadas por numerosos fatores, como
o vento, e outros como uma sublimação de água por perda de atmosfera, que acabaram por
deixar o seu testemunho inscrito na superfície de Marte através de elementos geomorfológicos
como andares de rosão, dunas de acumulação, diferenças texturais de sedimentos por ação de
difusão e vales entalhados por recuos do nível médio das águas desse oceano desde o seu
surgimento até à sua total sublimação, possibilitando uma visão panorâmica das condições
ambientais marcianas e assumindo a sua habitabilidade em parte da sua história geológica.
Mars is the most similar telluric planet in the Solar System to Planet Earth, due to its history of formation, planetary structure, chemical composition and the characteristics of its morphology/geomorphology present on its surface. These particularities suggest that, somewhere in its geological past, it had the conditions to maintain a liquid ocean in its northern hemisphere. Through a morphological and stratigraphic analysis using high-resolution images captured by three instruments (HRSC; CTX and HiRISE) on board two probes (Mars Express and Mars Reconnaissance Orbiter) orbiting Mars and digital terrain models generated from these data, the morphology of a sedimentary deposit located on the western margins of the Tharsis volcanic complex, from a valley called Isara Valles, was analyzed and interpreted. This deposit is classified in the literature as an alluvial/deltaic system, and there is strong evidence that, in addition to having been deposited at the interface of a flowing watercourse and a stable body of salt water, which can be considered an ocean, this gigantic body of water would be endowed with dynamic characteristics similar to its terrestrial analogues, such as the presence of waves, currents and intermittent movements similar to tides, triggered by numerous factors, such as wind, and others such as the sublimation of water due to loss of atmosphere, which ended up leaving their mark on the surface of Mars through geomorphological elements such as rosette floors, accumulation dunes, textural differences in sediments due to diffusion and valleys carved by the retreat of the average water level of this ocean from its emergence until its total sublimation, providing a panoramic view of Martian environmental conditions and assuming its habitability during part of its geological history.
Mars is the most similar telluric planet in the Solar System to Planet Earth, due to its history of formation, planetary structure, chemical composition and the characteristics of its morphology/geomorphology present on its surface. These particularities suggest that, somewhere in its geological past, it had the conditions to maintain a liquid ocean in its northern hemisphere. Through a morphological and stratigraphic analysis using high-resolution images captured by three instruments (HRSC; CTX and HiRISE) on board two probes (Mars Express and Mars Reconnaissance Orbiter) orbiting Mars and digital terrain models generated from these data, the morphology of a sedimentary deposit located on the western margins of the Tharsis volcanic complex, from a valley called Isara Valles, was analyzed and interpreted. This deposit is classified in the literature as an alluvial/deltaic system, and there is strong evidence that, in addition to having been deposited at the interface of a flowing watercourse and a stable body of salt water, which can be considered an ocean, this gigantic body of water would be endowed with dynamic characteristics similar to its terrestrial analogues, such as the presence of waves, currents and intermittent movements similar to tides, triggered by numerous factors, such as wind, and others such as the sublimation of water due to loss of atmosphere, which ended up leaving their mark on the surface of Mars through geomorphological elements such as rosette floors, accumulation dunes, textural differences in sediments due to diffusion and valleys carved by the retreat of the average water level of this ocean from its emergence until its total sublimation, providing a panoramic view of Martian environmental conditions and assuming its habitability during part of its geological history.
Descrição
Palavras-chave
Marte Terra Oceanos Geomorfologia fluviomarinha