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Author: Henrik Hargitai
Publisher: Springer
ISBN: 9783319265599
Category : Science
Languages : en
Pages : 2600
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Book Description
This revised and updated second edition provides a complete snapshot of our current knowledge on the geological features on solid-surface Solar System bodies. They extend over a wide range of scales, from micrometers to global scales, and include landform types (structural or topographic features), parts of landforms, terrain types and surface textures, surface patterns, and features identified at wavelengths extending from visible to radio waves, including albedo features, thermal infrared features, and radar features. The extensive new content addresses findings from the Messenger, Cassini, New Horizons, Curiosity and Maven missions and provides information on at least ten new landform types, as well as articles on exoplanet landforms. Refinements in methods and formations theories are also covered. Today scientists have a huge set of images and other physical data which makes it possible to create models on the inner structure and thermal history of planetary bodies. Combined data sets lead to better supported models on the formation of surface features. These models give reliable explanations for the origin of planetary landforms. New, higher resolution images reveal new sets of meso- and microscale landforms, while images from previously not imaged dwarf planets, satellites, asteroids and cometary nuclei show landforms never seen before. In the future exoplanets are expected to continue to provide brand new types of relief features not predictable by our Earth-and Solar System bound imagination. There are so many different landforms on planetary surfaces that it is nearly impossible for anybody to overview all of them who does not work exactly with that certain feature type. The Encyclopedia helps with presenting the landforms in searchable, alphabetical order. The book contains more than a simple list of various features: it provides context and connections between them and point to their origin. For example sand dunes were found on Venus, Mars and Titan, fluvial valleys and shorelines are present on Mars and Titan, impact craters have many different types - all are presented and explained here. Beyond the texts, references, schematic figures, images and planetary maps accompany the description of landforms, providing a wide background for detailed analyses even for geomorphologists working in planetary science. This book helps the reader discover the great variety of planetary landforms. Its continual updating makes it the go-to reference in the field.
Author: Henrik Hargitai
Publisher: Springer
ISBN: 9783319265599
Category : Science
Languages : en
Pages : 2600
Get Book Here
Book Description
This revised and updated second edition provides a complete snapshot of our current knowledge on the geological features on solid-surface Solar System bodies. They extend over a wide range of scales, from micrometers to global scales, and include landform types (structural or topographic features), parts of landforms, terrain types and surface textures, surface patterns, and features identified at wavelengths extending from visible to radio waves, including albedo features, thermal infrared features, and radar features. The extensive new content addresses findings from the Messenger, Cassini, New Horizons, Curiosity and Maven missions and provides information on at least ten new landform types, as well as articles on exoplanet landforms. Refinements in methods and formations theories are also covered. Today scientists have a huge set of images and other physical data which makes it possible to create models on the inner structure and thermal history of planetary bodies. Combined data sets lead to better supported models on the formation of surface features. These models give reliable explanations for the origin of planetary landforms. New, higher resolution images reveal new sets of meso- and microscale landforms, while images from previously not imaged dwarf planets, satellites, asteroids and cometary nuclei show landforms never seen before. In the future exoplanets are expected to continue to provide brand new types of relief features not predictable by our Earth-and Solar System bound imagination. There are so many different landforms on planetary surfaces that it is nearly impossible for anybody to overview all of them who does not work exactly with that certain feature type. The Encyclopedia helps with presenting the landforms in searchable, alphabetical order. The book contains more than a simple list of various features: it provides context and connections between them and point to their origin. For example sand dunes were found on Venus, Mars and Titan, fluvial valleys and shorelines are present on Mars and Titan, impact craters have many different types - all are presented and explained here. Beyond the texts, references, schematic figures, images and planetary maps accompany the description of landforms, providing a wide background for detailed analyses even for geomorphologists working in planetary science. This book helps the reader discover the great variety of planetary landforms. Its continual updating makes it the go-to reference in the field.
Author: Henrik Hargitai
Publisher: Springer
ISBN: 9781461431336
Category : Science
Languages : en
Pages : 2370
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Book Description
The technique of the mapping of planetary surfaces and the methods used for the identification of various planetary landforms improved much in the last 400 years. Until the 20th century, telescopic observers could interpret planetary landforms solely based on their appearance, while today various data sets acquired by space probes can be used for a more detailed analysis on the composition and origin of the surface features. Before the Greeks, the Earth and the Heavens were indisputably of different origin and nature. It was a major philosophical breakthrough - first appeared as an a priori theory, later based on observations - that the Heavens (planetary bodies) and the Earth share common features: gravity, composition and solar distance may be different, but the nature of the physical processes shaping the landforms are essentially the same. It has been a long way since we have arrived from the first telescopic description of lunar craters to the identification of various geological formations on Mars or on minor planets. Relief features of the Moon have first been observed by Galileo Galilee, via his telescope. During the next centuries, a multitude of Lunar landforms have been identified. Theories based on observations have been connected together by a scientific paradigm which explained their origin in a logical and seemingly undisputable manner. Telescopes showed a Lunar surface full of circular landforms, called craters, a landscape with no parallel on Earth. But the individual landforms had a morphological equivalent, volcanoes, which naturally led to the conclusion that craters had been created by volcanic processes. Maria ("seas") served as natural basins for water bodies. Observations clearly showed that water and air are hardly found on the Moon, the lack of clouds indicated the lack of precipitation. But the flat surface of the maria (obviously composed of marine sediments) and the meandering valleys suggested the presence of liquid water and a higher atmospheric pressure in the past - during the age of active volcanism and degassing. There were no observable active volcanic processes but some craters (though to be volcanoes) have been observed as being active: flashes of light - interpreted as eruptions - have been reported by several observers. The presence of pyroclasts thrown out from the volcanic vents of craters provided an independent evidence: meteor showers and individual meteorites falling from the sky - originating from Lunar craters. The logical and interconnected set of explanations based on observations proved to be completely false by the second half of the 20th century. The new paradigm interpreted the very same features in a new context. The case of Mars was different. There were no telescopes capable of observing relief forms (no shadows on Mars are visible from the Earth, because Mars always shows a nearly full Mars phase), so only albedo features could be seen and used for interpretation. The lack of visible relief features were interpreted as a lack of considerable topography: an unnoticed distortion in the observational data. The hue and contrast of dark and bright, orange, grey and white spots have changed seasonally, the polar areas clearly showed a polar cap made of ice and snow, but clouds have not been observed. Since Mars is farther away from the Sun than the Earth, it was evident that temperature values are lower there. Scientists concluded that Mars is an ancient, arid world. Then contemporary geology taught the theory according to which waters on the Earth are going to infiltrate underground in time, making the surface dry - observations showed that this had already happened on Mars. The last surface reservoirs of water were the polar caps. Some observers reported seeing a global network of linear features, but other have only seen very few of such albedo markings. These features were interpreted as "canals," made by a civilization for irrigation, carrying water from the poles to all around the flat plains of Mars. What was observable from the Earth were the broad stripes of irrigated vegetation (like those along the Nile), the canals themselves were too narrow to be visible from here. All theories converged - supposing that the features seen by some, but not seen by others, were real. There was no chance for verification until spacecrafts have been developed which were able to make local observations. Instead of canals, the first pictures returned revealed a surface full of craters - a landform not expected by anyone. A paradigm shift was needed to explain the features of the "new" Mars. On the Moon, features were observable, but the interpretation was wrong. On Mars, only blurred albedo markings could be observed, along with sharp lines of imagination, which again were interpreted falsely. In the case of Venus, there was no data on surface features. Only its bright cloud top could be observed from the Earth. But this fact along with the planet's orbital parameters provided enough information for a popular view on its surface conditions: a hot world (inferred from its proximity to the Sun) and also a rainy one (from its complete cloud cover). The conclusion: Venus is a global jungle possibly with dinosaurs, like the hot and wet world of the then-discovered Mesozoic era. Our current knowledge originated from these early attempts of interpreting surface conditions and geological origin of landforms from a very little set of available data. Today we have a huge set of images and other physical data which makes it possible to create models on the inner structure and thermal history of planetary bodies. Combined data sets lead to better supported models on the formation of surface features. Today we believe that most models give reliable explanation for the origin of planetary landforms. New, higher resolution images reveal new sets of meso- and microscale landforms, while images from previously not imaged dwarf planets, satellites, asteroids and cometary nuclei show landforms never seen before. In the future exoplanets are expected to provide brand new types of relief features no predictable by our Earth-and Solar System bound imagination. There are so many different landforms on planetary surfaces that it is nearly impossible for anybody to overview all of them who does not work exactly with that certain feature type. The Encyclopedia helps with presenting the landforms in searchable, alphabetical order. The book contains more than a simple list of various features: it provides context and connections between them and point to their origin. For example sand dunes were found on Venus, Mars and Titan, fluvial valleys and shorelines are present on Mars and Titan, impact craters have many different types - all are presented and explained here. Beyond the texts, references, schematic figures, images and planetary maps accompany the description of landforms, providing a wide background for detailed analyses even for geomorphologists working in planetary science. This book is to help the reader to discover the great variety of planetary landforms.
Author: Henrik Hargitai
Publisher: Springer
ISBN: 9781461431336
Category : Science
Languages : en
Pages : 0
Get Book Here
Book Description
The technique of the mapping of planetary surfaces and the methods used for the identification of various planetary landforms improved much in the last 400 years. Until the 20th century, telescopic observers could interpret planetary landforms solely based on their appearance, while today various data sets acquired by space probes can be used for a more detailed analysis on the composition and origin of the surface features. Before the Greeks, the Earth and the Heavens were indisputably of different origin and nature. It was a major philosophical breakthrough - first appeared as an a priori theory, later based on observations - that the Heavens (planetary bodies) and the Earth share common features: gravity, composition and solar distance may be different, but the nature of the physical processes shaping the landforms are essentially the same. It has been a long way since we have arrived from the first telescopic description of lunar craters to the identification of various geological formations on Mars or on minor planets. Relief features of the Moon have first been observed by Galileo Galilee, via his telescope. During the next centuries, a multitude of Lunar landforms have been identified. Theories based on observations have been connected together by a scientific paradigm which explained their origin in a logical and seemingly undisputable manner. Telescopes showed a Lunar surface full of circular landforms, called craters, a landscape with no parallel on Earth. But the individual landforms had a morphological equivalent, volcanoes, which naturally led to the conclusion that craters had been created by volcanic processes. Maria ("seas") served as natural basins for water bodies. Observations clearly showed that water and air are hardly found on the Moon, the lack of clouds indicated the lack of precipitation. But the flat surface of the maria (obviously composed of marine sediments) and the meandering valleys suggested the presence of liquid water and a higher atmospheric pressure in the past - during the age of active volcanism and degassing. There were no observable active volcanic processes but some craters (though to be volcanoes) have been observed as being active: flashes of light - interpreted as eruptions - have been reported by several observers. The presence of pyroclasts thrown out from the volcanic vents of craters provided an independent evidence: meteor showers and individual meteorites falling from the sky - originating from Lunar craters. The logical and interconnected set of explanations based on observations proved to be completely false by the second half of the 20th century. The new paradigm interpreted the very same features in a new context. The case of Mars was different. There were no telescopes capable of observing relief forms (no shadows on Mars are visible from the Earth, because Mars always shows a nearly full Mars phase), so only albedo features could be seen and used for interpretation. The lack of visible relief features were interpreted as a lack of considerable topography: an unnoticed distortion in the observational data. The hue and contrast of dark and bright, orange, grey and white spots have changed seasonally, the polar areas clearly showed a polar cap made of ice and snow, but clouds have not been observed. Since Mars is farther away from the Sun than the Earth, it was evident that temperature values are lower there. Scientists concluded that Mars is an ancient, arid world. Then contemporary geology taught the theory according to which waters on the Earth are going to infiltrate underground in time, making the surface dry - observations showed that this had already happened on Mars. The last surface reservoirs of water were the polar caps. Some observers reported seeing a global network of linear features, but other have only seen very few of such albedo markings. These features were interpreted as "canals," made by a civilization for irrigation, carrying water from the poles to all around the flat plains of Mars. What was observable from the Earth were the broad stripes of irrigated vegetation (like those along the Nile), the canals themselves were too narrow to be visible from here. All theories converged - supposing that the features seen by some, but not seen by others, were real. There was no chance for verification until spacecrafts have been developed which were able to make local observations. Instead of canals, the first pictures returned revealed a surface full of craters - a landform not expected by anyone. A paradigm shift was needed to explain the features of the "new" Mars. On the Moon, features were observable, but the interpretation was wrong. On Mars, only blurred albedo markings could be observed, along with sharp lines of imagination, which again were interpreted falsely. In the case of Venus, there was no data on surface features. Only its bright cloud top could be observed from the Earth. But this fact along with the planet's orbital parameters provided enough information for a popular view on its surface conditions: a hot world (inferred from its proximity to the Sun) and also a rainy one (from its complete cloud cover). The conclusion: Venus is a global jungle possibly with dinosaurs, like the hot and wet world of the then-discovered Mesozoic era. Our current knowledge originated from these early attempts of interpreting surface conditions and geological origin of landforms from a very little set of available data. Today we have a huge set of images and other physical data which makes it possible to create models on the inner structure and thermal history of planetary bodies. Combined data sets lead to better supported models on the formation of surface features. Today we believe that most models give reliable explanation for the origin of planetary landforms. New, higher resolution images reveal new sets of meso- and microscale landforms, while images from previously not imaged dwarf planets, satellites, asteroids and cometary nuclei show landforms never seen before. In the future exoplanets are expected to provide brand new types of relief features no predictable by our Earth-and Solar System bound imagination. There are so many different landforms on planetary surfaces that it is nearly impossible for anybody to overview all of them who does not work exactly with that certain feature type. The Encyclopedia helps with presenting the landforms in searchable, alphabetical order. The book contains more than a simple list of various features: it provides context and connections between them and point to their origin. For example sand dunes were found on Venus, Mars and Titan, fluvial valleys and shorelines are present on Mars and Titan, impact craters have many different types - all are presented and explained here. Beyond the texts, references, schematic figures, images and planetary maps accompany the description of landforms, providing a wide background for detailed analyses even for geomorphologists working in planetary science. This book is to help the reader to discover the great variety of planetary landforms.
Author: Thomas R. Watters
Publisher: Cambridge University Press
ISBN: 0521765730
Category : Science
Languages : en
Pages : 531
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Book Description
This book is an essential reference volume that surveys tectonic landforms on solid bodies throughout the Solar System.
Author: Henrik Hargitai
Publisher: Springer
ISBN: 3319628496
Category : Science
Languages : en
Pages : 371
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Book Description
This book approaches geological, geomorphological and topographical mapping from the point in the workflow at which science-ready datasets are available. Though there have been many individual projects on dynamic maps and online GISs, in which coding and data processing are given precedence over cartographic principles, cartography is more than “just” processing and displaying spatial data. However, there are currently no textbooks on this rapidly changing field, and methods tend to be shared informally. Addressing this gap in the literature, the respective chapters outline many topics pertaining to cartography and mapping such as the role and definition of planetary cartography and (vs?) Geographic Information Science; theoretical background and practical methodologies in geological mapping; science-ready versus public-ready products; a goal/procedure-focused practical manual of the most commonly used software in planetary mapping, which includes generic (ArcGIS and its extensions, JMARS) and specific tools (HiView, Cratertools etc.); extracting topographic information from images; thematic mapping: climate; geophysics; surface modeling; change detection; landing site selection; shared maps; dynamic maps on the web; planetary GIS interfaces; crowdsourcing; crater counting techniques; irregular bodies; geological unit symbology; mapping center activities; and web services. All chapters were prepared by authors who have actually produced geological maps or GISs for NASA / the USGS, DLR, ESA or MIIGAIK. Taken together, they offer an excellent resource for all planetary scientists whose research depends on mapping, and for students of astrogeology.
Author: Tracy K. P. Gregg
Publisher: Elsevier
ISBN: 0128139889
Category : Science
Languages : en
Pages : 362
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Book Description
Planetary Volcanism across the Solar System compares and contrasts the vast array of planetary bodies in the Solar System, including Earth. The wealth of spacecraft data for almost all major solid-surface bodies in the Solar System indicate that volcanism has been a dominant mechanism in shaping the landscapes of these bodies. The book addresses key questions surrounding our understanding of planetary volcanism, such as how to integrate the data into a coherent view of how volcanic activity arises, how this mechanism shapes planets, which volcanic landforms are ubiquitous throughout the Solar System, and which are unique. By placing a singular emphasis on comparing volcanic processes and landforms on all relevant Solar System bodies, and with the explicit objective of providing a systems-level understanding of this widespread phenomenon, users will find an up-to-date, accessible and comprehensive discussion of the major volcanic processes and landforms that shape and drive the evolution of planets, moons and smaller bodies. - Includes an introduction placing the book in the context of the larger Comparative Planetology series - Compares volcanic processes and landforms on all relevant Solar System bodies, providing a systems-level understanding of this widespread phenomenon - Offers a thorough examination of the major volcanic processes and landforms that shape and drive the evolution of planets, moons and smaller bodies - Includes information from new mission data and discoveries in recent years - Features over 100 color illustrations and charts to more clearly convey concepts - Offers additional online content, including figures, animations, video, and other multimedia content such as interviews with contributing authors
Author:
Publisher: Elsevier
ISBN: 0080547826
Category : Science
Languages : en
Pages : 7184
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Book Description
The quaternary sciences constitute a dynamic, multidisciplinary field of research that has been growing in scientific and societal importance in recent years. This branch of the Earth sciences links ancient prehistory to modern environments. Quaternary terrestrial sediments contain the fossil remains of existing species of flora and fauna, and their immediate predecessors. Quaternary science plays an integral part in such important issues for modern society as groundwater resources and contamination, sea level change, geologic hazards (earthquakes, volcanic eruptions, tsunamis), and soil erosion. With over 360 articles and 2,600 pages, many in full-color, the Encyclopedia of Quaternary Science provides broad ranging, up-to-date articles on all of the major topics in the field. Written by a team of leading experts and under the guidance of an international editorial board, the articles are at a level that allows undergraduate students to understand the material, while providing active researchers with the latest information in the field. Also available online via ScienceDirect (2006) – featuring extensive browsing, searching, and internal cross-referencing between articles in the work, plus dynamic linking to journal articles and abstract databases, making navigation flexible and easy. For more information, pricing options and availability visit www.info.sciencedirect.com. 360 individual articles written by prominent international authorities, encompassing all important aspects of quaternary science Each entry provides comprehensive, in-depth treatment of an overview topic and presented in a functional, clear and uniform layout Reference section provides guidence for further research on the topic Article text supported by full-color photos, drawings, tables, and other visual material Writing level is suited to both the expert and non-expert
Author: John L. Smellie
Publisher: Cambridge University Press
ISBN: 1107037395
Category : Nature
Languages : en
Pages : 497
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Book Description
Presents the distinctive processes and characteristics of glaciovolcanic eruptions, with reference to terrestrial and Mars occurrences.
Author: Richard Soare
Publisher: Elsevier
ISBN: 0128130199
Category : Science
Languages : en
Pages : 468
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Book Description
Dynamic Mars: Recent and Current Landscape Evolution of the Red Planet presents the latest observations, interpretations, and explanations of geological change at the surface or near-surface of this terrestrial body. These changes raise questions about a decades-old paradigm, formed largely in the aftermath of very coarse Mariner-mission imagery in the 1960s, suggesting that much of the interesting geological activity on Mars occurred deep in its past, eons ago. The book includes discussions of (1) Mars' ever-changing atmosphere and the impact of this on the planet's surface and near-surface; (2) the possible involvement of water in relatively new, if not contemporary, gully-like flows and slope streaks (i.e. recurring slope lineae); and (3) the identification of a broad suite of agents and processes (i.e. glacial, periglacial, aeolian, meteorological, volcanic, and meteoric) that are actively revising surface and near-surface landscapes, landforms, and features on a local, regional, and hemispheric scale.Highly illustrated and punctuated by data from the most recent Mars missions, Dynamic Mars is a valuable resource for all levels of research in the geological history of Mars, as well as of the three other terrestrial planets. - Utilizes observational and model-based data as well as geological context to frame the understanding of the dynamic surface and near-surface of Mars - Presents a broad spectrum of highly regarded experts and themes to discuss and evaluate the geological history of late and current Mars - Includes extensive and detailed imagery to clearly illustrate these themes, discussions, and evaluations
Author: Richard Soare
Publisher: Elsevier
ISBN: 0323993257
Category : Science
Languages : en
Pages : 420
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Book Description
Ices in the Solar-System: A Volatile-Driven Journey from the Inner Solar System to its Far Reaches details the evolution of ice on planetary bodies within the Solar System, including terrestrial planets and the Moon, Ceres and other dwarf planets or volatile asteroids, icy Galilean and Saturnian satellites, Triton and disparate Uranian moons, and Pluto, other Kuyper belt objects and comets. The book provides a view of different ice types throughout the Solar System, i.e., H2O, CO2, CH4, etc., that characterize icy processes on disparate bodies. Ice and icy processes at micro through macro scales are discussed. The book geographically spans the major planetary bodies of the Solar System, covering surface and subsurface geologies, geophysics and geochemistry of ices to answer questions such as the nature and extent of water ice and different frozen volatile species, how do ices give us clues to interiors and oceans, and more. - • Draws a pan solar-system view of various ice species • Identifies and addresses outstanding and sometimes puzzling questions about these ices • Describes the dynamic relationships between these ices and the geological history of the planets, moons, and smaller bodies where they occur • Studies these relationships using multiple analytical-scales and techniques
