Literatura académica sobre el tema "Atmosphère primordiale"
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Artículos de revistas sobre el tema "Atmosphère primordiale"
Ragossnig, Florian, Alexander Stökl, Ernst Dorfi, Colin P. Johnstone, Daniel Steiner y Manuel Güdel. "Interaction of infalling solid bodies with primordial atmospheres of disk-embedded planets". Astronomy & Astrophysics 618 (octubre de 2018): A19. http://dx.doi.org/10.1051/0004-6361/201832681.
Texto completoModirrousta-Galian, Darius y Jun Korenaga. "The Diffusion Limit of Photoevaporation in Primordial Planetary Atmospheres". Astrophysical Journal 965, n.º 1 (1 de abril de 2024): 97. http://dx.doi.org/10.3847/1538-4357/ad276f.
Texto completoChance, Quadry, Sarah Ballard y Keivan Stassun. "Signatures of Impact-driven Atmospheric Loss in Large Ensembles of Exoplanets". Astrophysical Journal 937, n.º 1 (1 de septiembre de 2022): 39. http://dx.doi.org/10.3847/1538-4357/ac8a97.
Texto completoKimura, Tadahiro y Masahiro Ikoma. "Formation of aqua planets with water of nebular origin: effects of water enrichment on the structure and mass of captured atmospheres of terrestrial planets". Monthly Notices of the Royal Astronomical Society 496, n.º 3 (22 de junio de 2020): 3755–66. http://dx.doi.org/10.1093/mnras/staa1778.
Texto completoMontoya, David. "Hostilidad perpetua, transformaciones transitorias: Persona, cuerpo y moralidad entre los tsotsiles de Chamula, Chiapas / Perpetual hostility, transitory transformations: Person, body and morality between the tsotsiles of Chamula, Chiapas". Revista Trace, n.º 78 (31 de julio de 2020): 67. http://dx.doi.org/10.22134/trace.78.2020.735.
Texto completoSinclair, Catriona A., Mark C. Wyatt, Alessandro Morbidelli y David Nesvorný. "Evolution of the Earth’s atmosphere during Late Veneer accretion". Monthly Notices of the Royal Astronomical Society 499, n.º 4 (16 de octubre de 2020): 5334–62. http://dx.doi.org/10.1093/mnras/staa3210.
Texto completoSaxena, Prabal, Lindy Elkins-Tanton, Noah Petro y Avi Mandell. "A model of the primordial lunar atmosphere". Earth and Planetary Science Letters 474 (septiembre de 2017): 198–205. http://dx.doi.org/10.1016/j.epsl.2017.06.031.
Texto completoYoung, Edward D., Anat Shahar y Hilke E. Schlichting. "Earth shaped by primordial H2 atmospheres". Nature 616, n.º 7956 (12 de abril de 2023): 306–11. http://dx.doi.org/10.1038/s41586-023-05823-0.
Texto completoLibby-Roberts, Jessica E., Zachory K. Berta-Thompson, Hannah Diamond-Lowe, Michael A. Gully-Santiago, Jonathan M. Irwin, Eliza M. R. Kempton, Benjamin V. Rackham et al. "The Featureless HST/WFC3 Transmission Spectrum of the Rocky Exoplanet GJ 1132b: No Evidence for a Cloud-free Primordial Atmosphere and Constraints on Starspot Contamination". Astronomical Journal 164, n.º 2 (19 de julio de 2022): 59. http://dx.doi.org/10.3847/1538-3881/ac75de.
Texto completoMicca Longo, Gaia, Luca Vialetto, Paola Diomede, Savino Longo y Vincenzo Laporta. "Plasma Modeling and Prebiotic Chemistry: A Review of the State-of-the-Art and Perspectives". Molecules 26, n.º 12 (16 de junio de 2021): 3663. http://dx.doi.org/10.3390/molecules26123663.
Texto completoTesis sobre el tema "Atmosphère primordiale"
Nunez, Elena. "The origin of terrestrial neon : an experimental study of isotopic fractionation of Neon during basalt degassing". Electronic Thesis or Diss., Orléans, 2024. http://www.theses.fr/2024ORLE1030.
Texto completoThe origin of Earth's volatile elements, crucial for understanding the evolution of the early Solar System, Earth's formation, and life, remains debated. Noble gases, due to their inertness and high volatility, serve as key tracers for major volatiles like CO2 and H2O in the mantle.The noble gas signatures in mantle plumes, particularly from Galapagos, Hawaii, and Iceland, suggest a solar-type neon acquired during Earth's formation. Two main models explain neon's origin in the mantle : (i) The neon was incorporated into a magma ocean through gravitational capture of a dense primary atmosphere, (ii) The neon was acquired from planetesimals irradiated by the early Sun during Earth's accretion. The residual concentration of mantle volatiles in volcanic rocks and minerals is often influenced by secondary processes and does not reflect primary mantle concentrations. In most oceanic basalts, the volatile phase is dominated by CO2. It's generally assumed that noble gas concentrations in this phase are similar between vesicles and depend on the extent and mechanism of gas loss from the magma. This thesis presents pioneering research on synthetic samples whose only volatiles are carbon dioxide (CO₂) and neon by exploring simple models of degassing in a closed system such as : (i) A depleted melt affected by a CO2-rich inputs and (ii) a system where the decompression is initiated. The observed isotopic similarity in natural samples, with values midway between the solar isotopic values and those of solar wind implantation, supports the hypothesis that the Earth's mantle may have captured a primordial nebula during the early stages of the planet's formation. Nevertheless, this experimental study presents compelling evidence that isotopic fractionation can occur during various stages of vesicle evolution in magma, suggesting that high isotopic ratios values in natural samples should be interpreted with caution. We conclude that none of the two scenarios of light-volatile acquisition can be for now rejected
Lunine, Jonathan Irving. "Volatiles in the Outer Solar System: I. Thermodynamics of Clathrate Hydrates. II. Ethane Ocean on Titan. III. Evolution of Primordial Titan Atmosphere". Thesis, 1985. https://thesis.library.caltech.edu/7490/1/Lunine_ji_1985.pdf.
Texto completoThree investigations are conducted into the physical chemistry of volatiles in the outer solar system and the role of volatiles in icy satellite evolution.
Part I:
The thermodynamic stability of clathrate hydrate is calculated under a wide range of temperature and pressure conditions applicable to solar system problems, using a statistical mechanical theory developed by Van der Waals and Platteeuw (1959) and existing experimental data on properties of clathrate hydrates and their components. At low pressure, dissociation pressures and partition functions (Langmuir constants) for CO clathrate (hydrate) have been predicted using the properties of clathrate containing, as guests, molecules similar to CO. The comparable or higher propensity of CO to incorporate in clathrate relative to N2 is used to argue for high CO to N2 ratios in primordial Titan if N2 were accreted as clathrate. The relative incorporation of noble gases in clathrate from a solar composition gas at low temperatures is calculated, and applied to the case of giant planet atmospheres and icy satellites. It is argued that non-solar but well-constrained noble gas abundances would be measured by Galileo in the Jovian atmosphere if the observed carbon enhancement were due to bombardment of the atmosphere by clathrate-bearing planetesimals sometime after planetary formation. The noble gas abundances of Titan's atmosphere are also predicted under the hypothesis that much of the satellite's methane accreted as clathrate. Double occupancy of clathrate cages by H2 and CH4 in contact with a solar composition gas is examined, and it is concluded that potentially important amounts of H2 may have incorporated in satellites as clathrate. The kinetics of clathrate formation is also examined, and it is suggested that, under thermodynamically appropriate conditions, essentially complete clathration of water ice could have occurred in high pressure nebulae around giant planets but probably not in the outer solar nebula; comets probably did not aggregate as clathrate. At moderate pressures, the phase diagram for methane clathrate hydrate in the presence of 15% ammonia (relative to water) is constructed, and application to the early Titan atmospheric composition is described. The high pressure stability of CH4, N2, and mixed CH4-N2 clathrate hydrate is calculated; conversion back to water and CH4 and/or N2 fluids or solids is predicted for pressures ≳12 kilobars and/or temperatures ≳320 K. The effect of ammonia is to shrink the T-P stability field of clathrate with increasing ammonia concentration. A preliminary phase diagram for the high pressure ammonia-water system is constructed using new data of Johnson et al. (1984). These results imply that 1) clathrate is stable throughout the interior of Oberon- and Rhea-sized icy satellites, and 2) clathrate incorporated in the inner-most icy regions of Titan would have decomposed, perhaps allowing buoyant methane to rise. Brief speculation on the implications of this conclusion for the origin of surficial methane on Titan is given. A list of suggested experiments and observations to test the theory and its predictions is presented.
Part II:
We propose a global Titanic ocean, one to several kilometers deep, the modern composition of which is predominantly ethane. If the ocean is in thermodynamic equilibrium with an atmosphere of 3' (mole fraction) methane then its composition is roughly 70% C2H6, 25% CH4, and 5% N2. Photochemical models predict that C2H6 is the dominant end-product of CH4 photolysis so that the evolving ocean is both the source and sink for ongoing photolysis. The coexisting atmosphere is compatible with Voyager data. Two consequences are pursued: the interaction of such an ocean with the underlying "bedrock" of Titan (assumed to be water-ice or ammonia hydrate) and with the primarily nitrogen atmosphere. It is concluded that although modest exchange of oceanic hydrocarbons with enclathrated methane in the bedrock can in principle occur, it is unlikely for reasonable regolith depths and probably physically inhibited by the presence of a layer of solid acetylene and complex polymeric hydrocarbons a couple of hundred meters thick at the base of the ocean. However, the surprisingly high solubility of water ice in liquid methane (Rebiai et al., 1983) implies that topographic features on Titan of order 100 meter in height can be eroded away on a time scale ≾109 years; "Karst" topography could be formed. Finally, the large solubility difference of N2 in methane versus ethane implies that the ocean composition is a strong determinant of atmospheric pressure; a simple radiative model of the Titan atmosphere is employed to demonstrate that significant surface pressure and temperature changes can occur as the oceanic composition evolves with time. The model suggests that the early methane-rich ocean may have been frozen; scenarios for evolution to the present liquid state are discussed.
Part III:
A simple convective cooling model of a primordial, CH4-NH3-N2 Titan atmosphere is constructed, in an effort to understand the fate of volatiles accreted from a gaseous disk ("nebula") surrounding Saturn and released from accreting planetesimals during the satellite's formation. Near-surface temperatures are initially ≳400 K consistent with the large amount of energy supplied to the atmosphere during accretion. As a consequence of accretional heating, the upper mantle of the satellite consists of an ammonia-water liquid, extending to the surface. This "magma ocean" is the primary buffer of atmospheric cooling because it is ≳10 times as massive as the atmosphere. The radiative properties of the atmosphere are assumed independent of frequency and the resulting temperature profile is found to be adiabatic; if the atmosphere contains dark particulates surface temperatures could be lower than calculated here. Three major processes drive the cooling: (1) hydrodynamic escape of gas from the top of the atmosphere, which determines the cooling time scales, (2) atmospheric ablation by high velocity impacts (not modeled in detail here), and (3) formation of clathrate hydrate at the ocean-atmosphere interface, at T ≤ 250 K. Cooling time scales driven by escape are sufficiently long (108-109 years) to allow ~10 bars of N2 to be produced photochemically from NH3 in the gas phase (Atreya et al., 1978); however, the abundance of NH3 at temperatures ≾150 K (where the intermediate photochemical products condense out) is optically thick to the dissociative UV photons. Thus, N2 formation may proceed primarily by shock heating of the atmosphere during large body impacts, as well as by photochemistry (1) at T < 150 K if intermediate products supersaturate, or (2) in a warm stratosphere, with NH3 abundance fixed by its tropopause value. The clathrate formed during late stages of cooling sequesters primarily CH4, with some N2, and forces surface temperatures and pressures to drop rapidly. The clathrate is only marginally buoyant relative to the coexisting ammonia-water liquid. If it sinks, the atmosphere is driven to an N2-rich state with most of the methane sequestered in clathrate when the ocean surface freezes over at ~180 K. Implications of this scenario for the present surface state of Titan are contrasted with those obtained if the clathrate forms a buoyant crust at the surface.
Libros sobre el tema "Atmosphère primordiale"
Theoretical considerations on the effects of electromagnetic fields on primordial reducing atmospheres. 1990.
Buscar texto completoTrieloff, Mario. Noble Gases. Oxford University Press, 2017. http://dx.doi.org/10.1093/acrefore/9780190647926.013.30.
Texto completoCapítulos de libros sobre el tema "Atmosphère primordiale"
Pepin, Robert O. "On the Isotopic Composition of Primordial Xenon in Terrestrial Planet Atmospheres". En From Dust to Terrestrial Planets, 371–95. Dordrecht: Springer Netherlands, 2000. http://dx.doi.org/10.1007/978-94-011-4146-8_24.
Texto completoZalasiewicz, Jan y Mark Williams. "Primordial Climate". En The Goldilocks Planet. Oxford University Press, 2012. http://dx.doi.org/10.1093/oso/9780199593576.003.0007.
Texto completoNi, Sidao y Thomas J. Ahrens. "Giant impact-induced blow-off of primordial atmosphere". En Large Meteorite Impacts III. Geological Society of America, 2005. http://dx.doi.org/10.1130/0-8137-2384-1.427.
Texto completoArbib, Michael A. "Atmosphere, affordances, and emotion". En When Brains Meet Buildings, 221–86. Oxford University Press, 2021. http://dx.doi.org/10.1093/med/9780190060954.003.0004.
Texto completoMilgrom, Lionel R. "Where porphyrins come from …". En The Colours of Life, 23–64. Oxford University PressOxford, 1997. http://dx.doi.org/10.1093/oso/9780198553809.003.0002.
Texto completoWitten, T. y P. Pincus. "Overview". En Structured Fluids, 1–12. Oxford University PressOxford, 2004. http://dx.doi.org/10.1093/oso/9780198526889.003.0001.
Texto completoLahav, Noam. "Planet Earth". En Biogenesis, 132–40. Oxford University PressNew York, NY, 1999. http://dx.doi.org/10.1093/oso/9780195117547.003.0014.
Texto completoFradenburg Joy, L. O. Aranye. "‘Le Sigh’: Enactive and Psychoanalytic Insights into Medieval and Renaissance Paralanguage". En Distributed Cognition in Medieval and Renaissance Culture, 269–85. Edinburgh University Press, 2019. http://dx.doi.org/10.3366/edinburgh/9781474438131.003.0015.
Texto completoCulliney, John L. y David Jones. "Ecology Emergent". En The Fractal Self. University of Hawai'i Press, 2017. http://dx.doi.org/10.21313/hawaii/9780824866617.003.0004.
Texto completoRohling, Eelco J. "ENERGY BALANCE OF CLIMATE". En The Climate Question. Oxford University Press, 2019. http://dx.doi.org/10.1093/oso/9780190910877.003.0006.
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