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Interior Surface Atmosphere Interactions Of Rocky Planets Simulation Of Volcanic Outgassing And Volatile Chemical Speciation In The C O H System
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Book Synopsis Interior-surface-atmosphere Interactions of Rocky Planets: Simulation of Volcanic Outgassing and Volatile Chemical Speciation in the C-O-H System by : Gianluigi Ortenzi
Download or read book Interior-surface-atmosphere Interactions of Rocky Planets: Simulation of Volcanic Outgassing and Volatile Chemical Speciation in the C-O-H System written by Gianluigi Ortenzi and published by . This book was released on 2021 with total page pages. Available in PDF, EPUB and Kindle. Book excerpt:
Book Synopsis The Atmospheric Fingerprints of Volcanism by : Philippa Kate Liggins
Download or read book The Atmospheric Fingerprints of Volcanism written by Philippa Kate Liggins and published by . This book was released on 2022 with total page 0 pages. Available in PDF, EPUB and Kindle. Book excerpt:
Book Synopsis Atmosphere and Climate Evolution on Earth and Earth-like Planets by : Benjamin Hayworth
Download or read book Atmosphere and Climate Evolution on Earth and Earth-like Planets written by Benjamin Hayworth and published by . This book was released on 2022 with total page 0 pages. Available in PDF, EPUB and Kindle. Book excerpt: Long-term atmospheric and climate evolution on terrestrial planets is primarily controlled by the silicate weathering feedback and evolution of the host-star. The former acts to regulate the climate of rocky planets by controlling the concentration of greenhouse gases in the atmosphere - shaping the habitability of said planet. In this dissertation, In Chapter 2, I explore how the silicate-weathering and ice-albedo feedbacks control the climate of early Mars when sufficient amounts of atmospheric H2 are present. This study can help us constrain the possible martian environments that allowed surface liquid water in its distant past. Explaining the evidence for surface liquid water on early Mars has been a challenge for climate modelers, as the sun was ~30% less luminous during the late-Noachian. I propose that the additional greenhouse forcing of CO2-H2 collision-induced absorption is capable of bringing the surface temperature above freezing and can put early Mars into a limit-cycling regime. Limit cycles occur when insolation is low and CO2 outgassing rates are unable to balance with the rapid drawdown of CO2 during warm weathering periods. Planets in this regime will alternate between global glaciation and transient warm climate phases. This mechanism is capable of explaining the geomorphological evidence for transient warm periods in the martian record. Previous work has shown that collision-induced absorption of CO2-H2 was capable of deglaciating early Mars, but only with high H2 outgassing rates (greater than ~600 Tmol/yr) and at high surface pressures (between 3 to 4 bars). I use new theoretically derived collision-induced absorption coefficients for CO2-H2 to reevaluate the climate limit cycling hypothesis for early Mars. The long-term habitability of a planet is often assumed to be controlled by its ability to cycle carbon between the solid planetary interior and atmosphere. This process allows the planet to respond to external forcings (i.e. changes in insolation, changes in volcanic outgassing rates, etc.) and regulate its surface temperature through negative feedbacks on atmospheric CO2 involved in silicate weathering. In Chapter 3, I explore how the different, non-linear dependencies on pCO2 between continental weathering and seafloor weathering rates can control how a habitable planet responds to external forcings. The evolution of a planet's host-star may not only impact its habitability, but its prebiotic environment. In Chapter 4, I explore what impact an active young Sun may have had on the young Earth's prebiotic environment at the dawn of life. Earth's Hadean atmosphere is thought to have been dominated by N2 and CO2 except in the aftermath of large impacts, when CO and CH4 may have become abundant. Here, I investigate the effect of high fluences of solar energetic particles (SEPs) from the more rapidly rotating, magnetically active young Sun. These particles would have penetrated deeply into Earth's atmosphere, ionizing and dissociating ambient gases as they did so. If the level of solar activity was very high, as it would have been if the Sun began its life as a rapid rotator, rapid dissociation of CO2 would have created an atmosphere rich in CO and O2. Such an atmosphere would have been too oxidized to be conducive to the origin of life in a surface environment. As the solar rotation rate slowed, the SEP fluence would have dropped off, causing O2 to disappear but allowing CO to remain abundant. Thermodynamic free energy from the 'water-gas shift' reaction, CO + H2O -> CO2 + H2, could have exceeded 50-60 kJ/mol -- more than enough to power nucleotide polymerization or ATP synthesis. Hence, charged particle bombardment could have played an important role in the origin of life. These same types of processes may operate on Earth-like planets orbiting other G-type stars, most of which are more magnetically active than the Sun.
Book Synopsis The Effect of Star-planet Interactions on Planetary Climate by : Aomawa L. Shields
Download or read book The Effect of Star-planet Interactions on Planetary Climate written by Aomawa L. Shields and published by . This book was released on 2014 with total page 148 pages. Available in PDF, EPUB and Kindle. Book excerpt: The goal of the work presented here is to explore the unique interactions between a host star, an orbiting planet, and additional planets in a stellar system, and to develop and test methods that include both radiative and gravitational effects on planetary climate and habitability. These methods can then be used to identify and assess the possible climates of potentially habitable planets in observed planetary systems. In this work I explored key star-planet interactions using a hierarchy of models, which I modifed to incorporate the spectrum of stars of different spectral types. Using a 1-D energy-balance climate model, a 1-D line-by-line, radiative-transfer model, and a 3-D general circulation model, I simulated planets covered by ocean, land, and water ice of varying grain size, with incident radiation from stars of different spectral types. I find that terrestrial planets orbiting stars with higher near-UV radiation exhibit a stronger ice-albedo feedback. Ice extent is much greater on a planet orbiting an F-dwarf star than on a planet orbiting a G-dwarf star at an equivalent flux distance, and ice-covered conditions occur on an F-dwarf planet with only a 2% reduction in instellation (incident stellar radiation) relative to the present instellation on Earth, assuming fixed CO2 (present atmospheric level on Earth). A similar planet orbiting the Sun at an equivalent flux distance requires an 8% reduction in instellation, while a planet orbiting an M-dwarf star requires an additional 19% reduction in instellation to become ice-covered, equivalent to 73% of the modern solar constant. The reduction in instellation must be larger for planets orbiting cooler stars due in large part to the stronger absorption of longer-wavelength radiation by icy surfaces on these planets, in addition to stronger absorption by water vapor, CO2, and clouds in their atmospheres, providing increased downwelling longwave radiation. The surface ice-albedo feedback effect becomes less important at the outer edge of the habitable zone, where atmospheric CO2 can be expected to be high. I show that ~3-10 bars of CO2 will entirely mask the climatic effect of ice and snow, leaving the traditional outer limit of the habitable zone unaffected by the spectral dependence of water ice and snow albedo. Simulations of the equilibrium climate response of a planet to increasing instellation from an F-, G-, or M-dwarf star indicate that the exit out of global ice cover is also sensitive to host star spectral energy distribution. Under fixed CO2 conditions, a planet orbiting an M-dwarf star exhibits a smaller resistance to melting out of a frozen state, requiring a smaller instellation to initiate deglaciation than planets orbiting hotter, brighter stars. This is due to the combined effects of surface ice and snow absorption of the large fraction of near-IR radiation emitted by M-dwarfs, and atmospheric near-IR absorption, which weakens the Hadley circulation, reducing the climate hysteresis (the range over which multiple stable equilibia are possible) of M-dwarf planets. Given their greater climatic stability, planets orbiting cooler, lower-mass stars may be the best candidates for long-term habitability and life beyond the Solar System. As lower-mass stars are likely candidates to host multiple rocky planets, it is important to consider whether gravitational interactions among planets may have significant effects on climate and habitability over long timescales. Using an n-body integrator with inputs from a method I developed to determine the locations of all planets in a given system at the same epoch using transit timing data, a specific case is explored- that of Kepler-62f (Borucki et al. 2013), a potentially habitable planet in a five-planet system orbiting a K-dwarf star. The maximum stable initial eccentricity possible for Kepler-62f is identified as e = 0.32. Simulations using a 3-D GCM indicate that Kepler-62f would have areas of the planet with surface temperatures above the freezing point of water with 1 bar or more of CO2 in its atmosphere. If it has an active carbon cycle, Kepler-62f could have ample amounts of greenhouse gases in its atmosphere to maintain atmospheric stability and habitable surface conditions while staying well below the maximum CO2 greenhouse limit. In a low-CO2 case (Earth-like levels), increases in planetary obliquity and orbital eccentricity coupled with an orbital configuration that places the summer solstice at or near pericenter generate regions of the planet with above-freezing surface temperatures, which may cause surface melting of an ice sheet formed during an annual cycle. If Kepler-62f is synchronously rotating and has an ocean, significant cloud cover could develop at the substellar point, increasing planetary albedo and reducing surface temperatures. The methods presented here serve as tested tools that can be used to assess the possible climates of potentially habitable planets in systems with a wide range of orbital architectures as they are discovered.
Download or read book Deep Carbon written by Beth N. Orcutt and published by Cambridge University Press. This book was released on 2019-10-17 with total page 687 pages. Available in PDF, EPUB and Kindle. Book excerpt: A comprehensive guide to carbon inside Earth - its quantities, movements, forms, origins, changes over time and impact on planetary processes. This title is also available as Open Access on Cambridge Core.
Download or read book Volcanism on Io written by Ryan S. Morgan and published by ProQuest. This book was released on 2008 with total page 106 pages. Available in PDF, EPUB and Kindle. Book excerpt:
Book Synopsis Comparative Climatology of Terrestrial Planets by : Stephen J. Mackwell
Download or read book Comparative Climatology of Terrestrial Planets written by Stephen J. Mackwell and published by University of Arizona Press. This book was released on 2014-01-30 with total page 709 pages. Available in PDF, EPUB and Kindle. Book excerpt: "Through the contributions of more than sixty leading experts in the field, Comparative Climatology of Terrestrial Planets sets forth the foundations for this emerging new science and brings the reader to the forefront of our current understanding of atmospheric formation and climate evolution"--Provided by publisher.
Book Synopsis Volcanic Gases and the Reaction of Sulfur Dioxide with Aluminosilicate Glasses by : Christian Josef Renggli
Download or read book Volcanic Gases and the Reaction of Sulfur Dioxide with Aluminosilicate Glasses written by Christian Josef Renggli and published by . This book was released on 2018 with total page 0 pages. Available in PDF, EPUB and Kindle. Book excerpt: Volcanic gases are an important part of the volatile cycle in active planetary systems and contribute significantly to the mobilization and transport of metals to planetary surfaces. On Earth, Venus, Mars and Io, SO2 is the most abundant corrosive species in volcanic gases, and basalts are ubiquitous on these planetary bodies. The reaction between SO2 and silicate rocks forms oxidized sulfate and reduced sulfide. This reaction is a key process in the formation of porphyry deposits. In volcanic eruption plumes SO2 reacts with volcanic ash and is scavenged onto the surface of the ash particles. Knowledge of the reaction mechanisms between volcanic gas and rocks, minerals and glasses, and processes controlling the metal mobilization and transport in volcanic gas can constrain models of volatile and metal budgets of planetary crusts and surfaces. Using thermochemical modelling, I present a new model for the composition of volcanic gas on the Moon and compare it to a terrestrial volcanic gas from Erta Ale volcano (Ethiopia). The main species in lunar volcanic gas are H2, S2 and CO. This finding is in contrast to previous studies which suggested that CO was the sole driver of explosive volcanic eruptions on the Moon. This lunar volcanic gas has a lower capacity for metal transport compared to the Cl- and H2O-rich volcanic gas from Erta Ale volcano. To identify how SO2-glass reactions occur at high temperature and to investigate what might promote and limit these reactions, I present results from an experimental study. Pure SO2 was reacted with silicate glasses in the system anorthite-diopside-albite and with Fe-bearing natural basaltic glasses. The sulfate reaction products are relatively enriched in Ca compared to the silicate glass composition, in particular in experiments with Fe-free anorthite-diopside glasses. On these Fe-free glasses CaSO4 is the sole observed phase in the coatings at 800 °C, whereas at 600 °C minor amounts of MgSO4 were detected. At 800 °C, the flux of Ca from the silicate glass to the surface exceeds that of Mg by a factor of up to 330, whereas at 600 °C this factor is only 3. The rate of reaction is not constant, decreasing by an order of magnitude from 1 h to 24 h at 800 °C. The reaction of SO2 with tholeiitic basalt glasses produces coatings of CaSO4, MgSO4, Na2SO4 and oxides including Fe2O3 and TiO2. In addition, the reaction modifies the basalt glass because Ca, Mg and Na are lost to the coating. This results in the nucleation of crystalline spherulites and needles including SiO2, Al2O3, as well as Fe-Na-rich and Mg-rich pyroxenes. VIII The results suggest that the structural properties of the silicate glass substrate control the diffusive transport of Ca, Na, Mg, Fe and Ti to the surface which in turn controls the overall reaction rate and the formation of sulfates, oxides and silicates. These findings can be applied to predicting reactions on planetary surfaces and at shallow levels within their crusts.
Book Synopsis Practical Chemical Thermodynamics for Geoscientists by : Bruce Fegley
Download or read book Practical Chemical Thermodynamics for Geoscientists written by Bruce Fegley and published by Academic Press. This book was released on 2013 with total page 816 pages. Available in PDF, EPUB and Kindle. Book excerpt: -- Presents brief historical summaries and biographies of key thermodynamics scientists alongside the fundamentals they were responsible for.
Book Synopsis Principles of Stable Isotope Geochemistry by : Zachary Sharp
Download or read book Principles of Stable Isotope Geochemistry written by Zachary Sharp and published by Prentice Hall. This book was released on 2007 with total page 368 pages. Available in PDF, EPUB and Kindle. Book excerpt: This is the first dedicated book to cover the basics of a wide range of stable isotope applications in a manner appropriate for someone entering the field. At the same time, it offers sufficient detail - and numerous references and examples - to direct research for further inquiry. Discusses diverse topics such as hydrology, carbon in plants, meteorites, carbonates, metamorphic rocks, etc. Explores the theory and principles of isotope fractionation. Offers unique, up-to-date discussion of meteorite (extraterrestrial) isotope data. Presents the subject in an interesting historical context, with the classic papers noted. A useful reference for students taking the course and professionals entering the field of Geochemistry.
Book Synopsis The Chemical Evolution of the Atmosphere and Oceans by : Heinrich D. Holland
Download or read book The Chemical Evolution of the Atmosphere and Oceans written by Heinrich D. Holland and published by Princeton University Press. This book was released on 1984-07-21 with total page 604 pages. Available in PDF, EPUB and Kindle. Book excerpt: In this first full-scale attempt to reconstruct the chemical evolution of the Earth's atmosphere and oceans, Heinrich Holland assembles data from a wide spectrum of fields to trace the history of the ocean-atmosphere system. A pioneer in an increasingly important area of scholarship, he presents a comprehensive treatment of knowledge on this subject, provides an extensive bibliography, and outlines problems and approaches for further research. The first four chapters deal with the turbulent first half billion years of Earth history. The next four chapters, devoted largely to the Earth from 3.9 to 0.6 b.y.b.p., demonstrate that changes in the atmosphere and oceans during this period were not dramatic. The last chapter of the book deals with the Phanerozoic Eon; although the isotopic composition of sulfur and strontium in seawater varied greatly during this period of Earth history, the chemical composition of seawater did not.
Book Synopsis Carbon in Earth's Interior by : Craig E. Manning
Download or read book Carbon in Earth's Interior written by Craig E. Manning and published by John Wiley & Sons. This book was released on 2020-04-03 with total page 373 pages. Available in PDF, EPUB and Kindle. Book excerpt: Carbon in Earth's fluid envelopes - the atmosphere, biosphere, and hydrosphere, plays a fundamental role in our planet's climate system and a central role in biology, the environment, and the economy of earth system. The source and original quantity of carbon in our planet is uncertain, as are the identities and relative importance of early chemical processes associated with planetary differentiation. Numerous lines of evidence point to the early and continuing exchange of substantial carbon between Earth's surface and its interior, including diamonds, carbon-rich mantle-derived magmas, carbonate rocks in subduction zones and springs carrying deeply sourced carbon-bearing gases. Thus, there is little doubt that a substantial amount of carbon resides in our planet's interior. Yet, while we know it must be present, carbon's forms, transformations and movements at conditions relevant to the interiors of Earth and other planets remain uncertain and untapped. Volume highlights include: - Reviews key, general topics, such as carbonate minerals, the deep carbon cycle, and carbon in magmas or fluids - Describes new results at the frontiers of the field with presenting results on carbon in minerals, melts, and fluids at extreme conditions of planetary interiors - Brings together emerging insights into carbon's forms, transformations and movements through study of the dynamics, structure, stability and reactivity of carbon-based natural materials - Reviews emerging new insights into the properties of allied substances that carry carbon, into the rates of chemical and physical transformations, and into the complex interactions between moving fluids, magmas, and rocks to the interiors of Earth and other planets - Spans the various chemical redox states of carbon, from reduced hydrocarbons to zero-valent diamond and graphite to oxidized CO2 and carbonates - Captures and synthesizes the exciting results of recent, focused efforts in an emerging scientific discipline - Reports advances over the last decade that have led to a major leap forward in our understanding of carbon science - Compiles the range of methods that can be tapped tap from the deep carbon community, which includes experimentalists, first principles theorists, thermodynamic modelers and geodynamicists - Represents a reference point for future deep carbon science research Carbon in Planetary Interiors will be a valuable resource for researchers and students who study the Earth's interior. The topics of this volume are interdisciplinary, and therefore will be useful to professionals from a wide variety of fields in the Earth Sciences, such as mineral physics, petrology, geochemistry, experimentalists, first principles theorists, thermodynamics, material science, chemistry, geophysics and geodynamics.
Book Synopsis Stable Isotope Geochemistry by : Jochen Hoefs
Download or read book Stable Isotope Geochemistry written by Jochen Hoefs and published by Springer Science & Business Media. This book was released on 2013-04-17 with total page 333 pages. Available in PDF, EPUB and Kindle. Book excerpt: Stable Isotope Geochemistry is an introduction to the use of stable isotopes in the fields of geoscience. It is subdivided into three parts: - theoretical and experimental principles; - fractionation mechanisms of light elements; - the natural variations of geologically important reservoirs. In this updated 4th edition many of the chapters have been expanded, especially those on techniques and environmental aspects. The main focus is on recent results and new developments. For students and scientists alike the book will be a primary reference with regard to how and where stable isotopes can be used to solve geological problems.
Download or read book Geochemistry written by Harry Y. McSween and published by Columbia University Press. This book was released on 2003 with total page 381 pages. Available in PDF, EPUB and Kindle. Book excerpt: Written expressly for undergraduate and graduate geologists, this book focuses on how geochemical principles can be used to solve practical problems. The attention to problem-solving reflects the authors'belief that showing how theory is useful in solving real-life problems is vital for learning. The book gives students a thorough grasp of the basic principles of the subject, balancing the traditional equilibrium perspective and the kinetic viewpoint. The first half of the book considers processes in which temperature and pressure are nearly constant. After introductions to the laws of thermodynamics, to fundamental equations for flow and diffusion, and to solution chemistry, these principles are used to investigate diagenesis, weathering, and natural waters. The second half of the book applies thermodynamics and kinetics to systems undergoing changes in temperature and pressure during magmatism and metamorphism. This revised edition incorporates new geochemical discoveries as examples of processes and pathways, with new chapters on mineral structure and bonding and on organic matter and biomarkers. Each chapter has worked problems, and the authors assume that the student has had a year of college-level chemistry and a year of calculus. Praise for the first edition "A truly modern geochemistry book.... Very well written and quite enjoyable to read.... An excellent basic text for graduate level instruction in geochemistry." --Journal of Geological Education "An up-to-date, broadly conceived introduction to geochemistry.... Given the recent flowering of geochemistry as an interdisciplinary science, and given the extent to which it now draws upon the fundamentals of thermodynamics and kinetics to understand earth and planetary processes, this timely and rigorous [book] is welcome indeed." --Geochimica et Cosmochimica Acta
Book Synopsis The Role of Halogens in Terrestrial and Extraterrestrial Geochemical Processes by : Daniel E. Harlov
Download or read book The Role of Halogens in Terrestrial and Extraterrestrial Geochemical Processes written by Daniel E. Harlov and published by Springer. This book was released on 2018-01-30 with total page 1029 pages. Available in PDF, EPUB and Kindle. Book excerpt: The book summarizes the knowledge and experiences concerning the role of halogens during various geochemical processes, such as diagenesis, ore-formation, magma evolution, metasomatism, mineralization, and metamorphism in the crust and mantle of the Earth. It comprises the role of halogens in other terrestrial worlds like volatile-rich asteroids, Mars, and the ice moons of Jupiter and Saturn. Review chapters outline and expand upon the basis of our current understanding regarding how halogens contribute to the geochemical/geophysical evolution and stability of terrestrial worlds overall.
Book Synopsis The Phanerozoic Carbon Cycle by : Robert A. Berner
Download or read book The Phanerozoic Carbon Cycle written by Robert A. Berner and published by Oxford University Press. This book was released on 2004-08-19 with total page 159 pages. Available in PDF, EPUB and Kindle. Book excerpt: The term "carbon cycle" is normally thought to mean those processes that govern the present-day transfer of carbon between life, the atmosphere, and the oceans. This book describes another carbon cycle, one which operates over millions of years and involves the transfer of carbon between rocks and the combination of life, the atmosphere, and the oceans. The weathering of silicate and carbonate rocks and ancient sedimentary organic matter (including recent, large-scale human-induced burning of fossil fuels), the burial of organic matter and carbonate minerals in sediments, and volcanic degassing of carbon dioxide contribute to this cycle. In The Phanerozoic Carbon Cycle, Robert Berner shows how carbon cycle models can be used to calculate levels of atmospheric CO[2 and O[2 over Phanerozoic time, the past 550 million years, and how results compare with independent methods. His analysis has implications for such disparate subjects as the evolution of land plants, the presence of giant ancient insects, the role of tectonics in paleoclimate, and the current debate over global warming and greenhouse gases
Book Synopsis Volcanic Degassing by : Clive Oppenheimer
Download or read book Volcanic Degassing written by Clive Oppenheimer and published by Geological Society of London. This book was released on 2003 with total page 438 pages. Available in PDF, EPUB and Kindle. Book excerpt:
