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Artículos de revistas sobre el tema "Atmosphère primordiale"

Autor: Grafiati

Publicado: 14 de diciembre de 2024

Última modificación: 31 de julio de 2025

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1

Ragossnig, Florian, Alexander Stökl, Ernst Dorfi, Colin P. Johnstone, Daniel Steiner, and Manuel Güdel. "Interaction of infalling solid bodies with primordial atmospheres of disk-embedded planets." Astronomy & Astrophysics 618 (October 2018): A19. http://dx.doi.org/10.1051/0004-6361/201832681.

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Context. Planets that form early enough to be embedded in the circumstellar gas disk accumulate thick atmospheres of nebular gas. Models of these atmospheres need to specify the surface luminosity (i.e. energy loss rate) of the planet. This luminosity is usually associated with a continuous inflow of solid bodies, where the gravitational energy released from these bodies is the source of energy. However, if these bodies release energy in the atmosphere instead of at the surface, this assumption might not be justified. Aims. Our aim is to explore the interactions of infalling planetesimals with

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2

Modirrousta-Galian, Darius, and Jun Korenaga. "The Diffusion Limit of Photoevaporation in Primordial Planetary Atmospheres." Astrophysical Journal 965, no. 1 (2024): 97. http://dx.doi.org/10.3847/1538-4357/ad276f.

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Abstract Photoevaporation is thought to play an important role in early planetary evolution. In this study, we investigate the diffusion limit of X-ray- and ultraviolet-induced photoevaporation in primordial atmospheres. We find that compositional fractionation resulting from mass loss is more significant than currently recognized, because it is controlled by the conditions at the top of the atmosphere, where particle collisions are less frequent. Such fractionation at the top of the atmosphere develops a compositional gradient that extends downward. The mass outflow eventually reaches a stead

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3

Chance, Quadry, Sarah Ballard, and Keivan Stassun. "Signatures of Impact-driven Atmospheric Loss in Large Ensembles of Exoplanets." Astrophysical Journal 937, no. 1 (2022): 39. http://dx.doi.org/10.3847/1538-4357/ac8a97.

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Abstract The results of large-scale exoplanet transit surveys indicate that the distribution of small planet radii is likely sculpted by atmospheric loss. Several possible physical mechanisms exist for this loss of primordial atmospheres, each of which produces a different set of observational signatures. In this study, we investigate the impact-driven mode of atmosphere loss via N-body simulations. We compare the results from giant impacts, at a demographic level, to results from another commonly invoked method of atmosphere loss, photoevaporation. Applying two different loss prescriptions to

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4

Kimura, Tadahiro, and 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, no. 3 (2020): 3755–66. http://dx.doi.org/10.1093/mnras/staa1778.

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ABSTRACT Recent detection of exoplanets with Earth-like insolation attracts growing interest in how common Earth-like aqua planets are beyond the Solar system. While terrestrial planets are often assumed to capture icy or water-rich planetesimals, a primordial atmosphere of nebular origin itself can produce water through oxidation of the atmospheric hydrogen with oxidizing minerals from incoming planetesimals or the magma ocean. Thermodynamically, normal oxygen buffers produce water comparable in mole number equal to or more than hydrogen. Thus, the primordial atmosphere would likely be highly

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5

Montoya, 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, no. 78 (July 31, 2020): 67. http://dx.doi.org/10.22134/trace.78.2020.735.

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El actual estudio etnográfico da cuenta de que lo chon –un aspecto de la persona, generalmente, asociado a lo animal– está relacionado con un estado de permanente hostilidad, presente en el mundo desde tiempos primordiales. Este aspecto, a la vez que potencia la vulnerabilidad entre los humanos, resalta la fortaleza de otros seres, como Dios y el Pukuj. En la búsqueda de lidiar con esa atmósfera de hostilidad y, de mitigar su propia vulnerabilidad, la humanidad experimenta múltiples transformaciones morales-corporales.Abstract: This ethnographic study shows that the chon –an aspect of the pers

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6

Sinclair, Catriona A., Mark C. Wyatt, Alessandro Morbidelli, and David Nesvorný. "Evolution of the Earth’s atmosphere during Late Veneer accretion." Monthly Notices of the Royal Astronomical Society 499, no. 4 (2020): 5334–62. http://dx.doi.org/10.1093/mnras/staa3210.

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ABSTRACT Recent advances in our understanding of the dynamical history of the Solar system have altered the inferred bombardment history of the Earth during accretion of the Late Veneer, after the Moon-forming impact. We investigate how the bombardment by planetesimals left-over from the terrestrial planet region after terrestrial planet formation, as well as asteroids and comets, affects the evolution of Earth’s early atmosphere. We develop a new statistical code of stochastic bombardment for atmosphere evolution, combining prescriptions for atmosphere loss and volatile delivery derived from

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7

Saxena, Prabal, Lindy Elkins-Tanton, Noah Petro, and Avi Mandell. "A model of the primordial lunar atmosphere." Earth and Planetary Science Letters 474 (September 2017): 198–205. http://dx.doi.org/10.1016/j.epsl.2017.06.031.

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8

Rogers, James G., Caroline Dorn, Vivasvaan Aditya Raj, Hilke E. Schlichting, and Edward D. Young. "Most Super-Earths Have Less Than 3% Water." Astrophysical Journal 979, no. 1 (2025): 79. https://doi.org/10.3847/1538-4357/ad9f61.

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Abstract Super-Earths are highly irradiated, small planets with bulk densities approximately consistent with Earth. We construct combined interior atmosphere models of super-Earths that trace the partitioning of water throughout a planet, including an iron-rich core, silicate-rich mantle, and steam atmosphere. We compare these models with exoplanet observations to infer a 1σ upper limit on the total water mass fraction of ≲3% at the population level. We consider end-member scenarios that may change this value, including the efficiency of mantle outgassing, escape of high mean molecular weight

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9

Young, Edward D., Anat Shahar, and Hilke E. Schlichting. "Earth shaped by primordial H2 atmospheres." Nature 616, no. 7956 (2023): 306–11. http://dx.doi.org/10.1038/s41586-023-05823-0.

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10

Libby-Roberts, Jessica E., Zachory K. Berta-Thompson, Hannah Diamond-Lowe, 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, no. 2 (2022): 59. http://dx.doi.org/10.3847/1538-3881/ac75de.

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Abstract Orbiting an M dwarf 12 pc away, the transiting exoplanet GJ 1132b is a prime target for transmission spectroscopy. With a mass of 1.7 M ⊕ and radius of 1.1 R ⊕, GJ 1132b’s bulk density indicates that this planet is rocky. Yet with an equilibrium temperature of 580 K, GJ 1132b may still retain some semblance of an atmosphere. Understanding whether this atmosphere exists and its composition will be vital for understanding how the atmospheres of terrestrial planets orbiting M dwarfs evolve. We observe five transits of GJ 1132b with the Wide Field Camera 3 (WFC3) on the Hubble Space Teles

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11

Micca Longo, Gaia, Luca Vialetto, Paola Diomede, Savino Longo, and Vincenzo Laporta. "Plasma Modeling and Prebiotic Chemistry: A Review of the State-of-the-Art and Perspectives." Molecules 26, no. 12 (2021): 3663. http://dx.doi.org/10.3390/molecules26123663.

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We review the recent progress in the modeling of plasmas or ionized gases, with compositions compatible with that of primordial atmospheres. The plasma kinetics involves elementary processes by which free electrons ultimately activate weakly reactive molecules, such as carbon dioxide or methane, thereby potentially starting prebiotic reaction chains. These processes include electron–molecule reactions and energy exchanges between molecules. They are basic processes, for example, in the famous Miller-Urey experiment, and become relevant in any prebiotic scenario where the primordial atmosphere

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12

Melosh, H. J., and A. M. Vickery. "Impact erosion of the primordial atmosphere of Mars." Nature 338, no. 6215 (1989): 487–89. http://dx.doi.org/10.1038/338487a0.

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13

Davenport, Brian, Eliza M. R. Kempton, Matthew C. Nixon, et al. "TOI-421 b: A Hot Sub-Neptune with a Haze-free, Low Mean Molecular Weight Atmosphere." Astrophysical Journal Letters 984, no. 2 (2025): L44. https://doi.org/10.3847/2041-8213/adcd76.

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Abstract Common features of sub-Neptune atmospheres observed to date include signatures of aerosols at moderate equilibrium temperatures (∼500–800 K) and a prevalence of high mean molecular weight atmospheres, perhaps indicating novel classes of planets such as water worlds. Here we present a 0.83–5 μm JWST transmission spectrum of the sub-Neptune TOI-421 b. This planet is unique among previously observed counterparts in its high equilibrium temperature (T eq ≈ 920 K) and its Sun-like host star. We find marked differences between the atmosphere of TOI-421 b and those of sub-Neptunes previously

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14

NAKAZAWA, Kiyoshi, Hiroshi MIZUNO, Minoru SEKIYA, and Chushiro HAYASHI. "Structure of the primordial atmosphere surrounding the early-earth." Journal of geomagnetism and geoelectricity 37, no. 8 (1985): 781–99. http://dx.doi.org/10.5636/jgg.37.781.

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15

Scarsdale, Nicholas, Nicholas Wogan, Hannah R. Wakeford та ін. "JWST COMPASS: The 3–5 μm Transmission Spectrum of the Super-Earth L 98-59 c". Astronomical Journal 168, № 6 (2024): 276. http://dx.doi.org/10.3847/1538-3881/ad73cf.

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Abstract We present a JWST Near-InfraRed Spectrograph (NIRSpec) transmission spectrum of the super-Earth exoplanet L 98-59 c. This small (R p = 1.385 ± 0.085R ⊕, M p = 2.22 ± 0.26 R ⊕), warm (T eq = 553 K) planet resides in a multiplanet system around a nearby, bright (J = 7.933) M3V star. We find that the transmission spectrum of L 98-59 c is featureless at the precision of our data. We achieve precisions of 22 ppm in NIRSpec G395H’s NRS1 detector and 36 ppm in the NRS2 detector at a resolution R ∼ 200 (30 pixel wide bins). At this level of precision, we are able rule out primordial H2–He atm

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16

Ueda, Hisahiro, and Takazo Shibuya. "Composition of the Primordial Ocean Just after Its Formation: Constraints from the Reactions between the Primitive Crust and a Strongly Acidic, CO2-Rich Fluid at Elevated Temperatures and Pressures." Minerals 11, no. 4 (2021): 389. http://dx.doi.org/10.3390/min11040389.

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The Hadean was an enigmatic period in the Earth’s history when ocean formation and the emergence of life may have occurred. However, minimal geological evidence is left from this period. To understand the primordial ocean’s composition, we focused on the ocean’s formation processes from CO2- and HCl-bearing water vapor in the high-temperature atmosphere. When the temperature of the lower atmosphere fell below the critical point, high-temperature rain reached the ground surface. Then, hydrothermal reactions between the subcritical fluid and primordial crust started. Eventually, a liquid ocean e

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17

Misener, William, and Hilke E. Schlichting. "To cool is to keep: residual H/He atmospheres of super-Earths and sub-Neptunes." Monthly Notices of the Royal Astronomical Society 503, no. 4 (2021): 5658–74. http://dx.doi.org/10.1093/mnras/stab895.

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ABSTRACT Super-Earths and sub-Neptunes are commonly thought to have accreted hydrogen/helium envelopes, consisting of a few to ten percent of their total mass, from the primordial gas disc. Subsequently, hydrodynamic escape driven by core-powered mass-loss and/or photoevaporation likely stripped much of these primordial envelopes from the lower mass and closer-in planets to form the super-Earth population. In this work, we show that after undergoing core-powered mass-loss, some super-Earths can retain small residual H/He envelopes. This retention is possible because, for significantly depleted

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18

Kurosaki, Kenji, Yasunori Hori, Masahiro Ogihara, and Masanobu Kunitomo. "Evolution of a Water-rich Atmosphere Formed by a Giant Impact on an Earth-sized Planet." Astrophysical Journal 957, no. 2 (2023): 67. http://dx.doi.org/10.3847/1538-4357/acfe0a.

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Abstract The atmosphere of a terrestrial planet that is replenished with secondary gases should have accumulated hydrogen-rich gas from its protoplanetary disk. Although a giant impact blows off a large fraction of the primordial atmosphere of a terrestrial planet in the late formation stage, the remaining atmosphere can become water-rich via chemical reactions between hydrogen and vaporized core material. We find that a water-rich postimpact atmosphere forms when a basaltic or CI chondrite core is assumed. In contrast, little postimpact water is generated for an enstatite chondrite core. We i

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19

Trafton, L., S. A. Stern, and G. R. Gladstone. "The Pluto-Charon system: The escape of charon's primordial atmosphere." Icarus 74, no. 1 (1988): 108–20. http://dx.doi.org/10.1016/0019-1035(88)90033-4.

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20

Liu, Lin-gun. "The Proto-Atmosphere of Terrestrial Planets." European Journal of Applied Sciences 13, no. 02 (2025): 473–78. https://doi.org/10.14738/aivp.1302.18571.

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The theoretically derived composition of the proto-atmosphere, which evolved during accretion, of terrestrial planets is composed primarily of CO2, Ar and N2 when the mass of a planet became greater than 3.30 x 1026 g. This is identical to the atmospheric compositions of Venus and Mars observed today. Therefore, both Venus and Mars most likely retained their proto-atmospheres till now. The Earth is situated between Venus and Mars, there is no reason whatsoever that the Earth’s proto-atmosphere should be any different from those of Venus and Mars. Yet, today’s Earth atmospheric composition is d

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21

Howe, Alex R., Fred C. Adams, and Michael R. Meyer. "Survival of Primordial Planetary Atmospheres: Photodissociation-driven Mass Loss." Astrophysical Journal 894, no. 2 (2020): 130. http://dx.doi.org/10.3847/1538-4357/ab620c.

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22

Amaral, Laura N. R. do, Evgenya L. Shkolnik, R. O. Parke Loyd, and Sarah Peacock. "The Impact of Stellar Flares on the Atmospheric Escape of Exoplanets Orbiting M Stars. I. Insights from the AU Mic System." Astrophysical Journal 985, no. 1 (2025): 100. https://doi.org/10.3847/1538-4357/adc932.

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Abstract The X-ray and extreme ultraviolet (XUV) emission from M stars can drive the atmospheric escape on planets orbiting them. M stars are also known for their frequent emission of stellar flares, which will increase the high-energy flux received by their orbiting planets. To understand how stellar flares impact the primordial atmospheres of planets orbiting young M stars, we use UV spectroscopic data of flares from the Habitable Zones and M dwarf Activity across Time and Measurements of the Ultraviolet Spectral Characteristics of Low-mass Exoplanetary Systems programs as a proxy for the XU

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23

Kubyshkina, Daria, and Aline A. Vidotto. "How does the mass and activity history of the host star affect the population of low-mass planets?" Monthly Notices of the Royal Astronomical Society 504, no. 2 (2021): 2034–50. http://dx.doi.org/10.1093/mnras/stab897.

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ABSTRACT The evolution of the atmospheres of low- and intermediate-mass planets is strongly connected to the physical properties of their host stars. The types and the past activities of planet-hosting stars can, therefore, affect the overall planetary population. In this paper, we perform a comparative study of sub-Neptune-like planets orbiting stars of different masses and different evolutionary histories. We discuss the general patterns of the evolved population as a function of parameters and environments of planets. As a model of the atmospheric evolution, we employ the own framework comb

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24

Atri, Dimitra, and Shane R. Carberry Mogan. "Stellar flares versus luminosity: XUV-induced atmospheric escape and planetary habitability." Monthly Notices of the Royal Astronomical Society: Letters 500, no. 1 (2020): L1—L5. http://dx.doi.org/10.1093/mnrasl/slaa166.

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ABSTRACT Space weather plays an important role in the evolution of planetary atmospheres. Observations have shown that stellar flares emit energy in a wide energy range (1030–1038 erg), a fraction of which lies in X-rays and extreme ultraviolet (XUV). These flares heat the upper atmosphere of a planet, leading to increased escape rates, and can result in atmospheric erosion over a period of time. Observations also suggest that primordial terrestrial planets can accrete voluminous H/He envelopes. Stellar radiation can erode these protoatmospheres over time, and the extent of this erosion has im

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25

Lentz, Eric J., Peter H. Hauschildt, Jason P. Aufdenberg, and Ed Baron. "Model atmospheres of massive zero-metallicity stars." Symposium - International Astronomical Union 212 (2003): 416–17. http://dx.doi.org/10.1017/s0074180900212552.

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We have calculated detailed, fully non-LTE, model atomospheres for massive zero-metal stars. We find the atmospheres of massive primordial stars become unbound due to radiation pressure on lines and continua over a much larger fraction of their evolution than previously expected.

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26

Cannon, Kevin M., Stephen W. Parman, and John F. Mustard. "Primordial clays on Mars formed beneath a steam or supercritical atmosphere." Nature 552, no. 7683 (2017): 88–91. http://dx.doi.org/10.1038/nature24657.

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27

Tian, Meng, and Kevin Heng. "Atmospheric Chemistry of Secondary and Hybrid Atmospheres of Super Earths and Sub-Neptunes." Astrophysical Journal 963, no. 2 (2024): 157. http://dx.doi.org/10.3847/1538-4357/ad217c.

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Abstract The atmospheres of small exoplanets likely derive from a combination of geochemical outgassing and primordial gases left over from formation. Secondary atmospheres, such as those of Earth, Mars, and Venus, are sourced by outgassing. Persistent outgassing into long-lived, primordial, hydrogen–helium envelopes produces hybrid atmospheres of which there are no examples in the solar system. We construct a unified theoretical framework for calculating the outgassing chemistry of both secondary and hybrid atmospheres, where the input parameters are the surface pressure, oxidation, and sulfi

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28

Glover, Simon, and Daniel Wolf Savin. "cooling in primordial gas." Philosophical Transactions of the Royal Society A: Mathematical, Physical and Engineering Sciences 364, no. 1848 (2006): 3107–12. http://dx.doi.org/10.1098/rsta.2006.1867.

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Simulations of the thermal and dynamical evolution of primordial gas typically focus on the role played by H 2 cooling. H 2 is the dominant coolant in low-density primordial gas and it is usually assumed that it remains dominant at high densities. However, H 2 is not an effective coolant at high densities, owing to the low critical density at which it reaches local thermodynamic equilibrium and to the large opacities that develop in its emission lines. It is therefore important to quantify the contribution made to the cooling rate by emission from the other molecules and ions present in the ga

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29

Spite, M., P. Bonifacio, F. Spite, E. Caffau, L. Sbordone, and A. J. Gallagher. "Be and O in the ultra metal-poor dwarf 2MASS J18082002-5104378: the Be–O correlation." Astronomy & Astrophysics 624 (April 2019): A44. http://dx.doi.org/10.1051/0004-6361/201834741.

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Context. Measurable amounts of Be could have been synthesised primordially if the Universe were non-homogeneous or in the presence of late decaying relic particles. Aims. We investigate the Be abundance in the extremely metal-poor star 2MASS J1808-5104 ([Fe/H] = −3.84) with the aim of constraining inhomogeneities or the presence of late decaying particles. Methods. High resolution, high signal-to-noise ratio (S/N) UV spectra were acquired at ESO with the Kueyen 8.2 m telescope and the UVES spectrograph. Abundances were derived using several model atmospheres and spectral synthesis code. Result

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30

Amsler Moulanier, Alizée, Olivier Mousis, Alexis Bouquet, and Christopher R. Glein. "The Role of Ammonia in the Distribution of Volatiles in the Primordial Hydrosphere of Europa." Planetary Science Journal 6, no. 1 (2025): 1. https://doi.org/10.3847/psj/ad9925.

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Abstract The presence of a hydrosphere on Europa raises questions about its habitability, and studies of its volatile inventory can provide insight into its formation process. Different scenarios suggest that Europa's volatiles could be derived from cometary ices or devolatilized building blocks. The study of post-accretion processes—in particular, the “open-ocean” phase that likely occurred before the formation of the icy crust—is crucial to distinguishing these origins, as this phase is likely to have influenced the volatile inventory. The abundance of ammonia in Europa's building blocks is

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31

Mizuno, Hiroshi, and Kiyoshi Nakazawa. "Chapter 22. Primordial Atmosphere Surrounding a Protoplanet and Formation of Jovian Planets." Progress of Theoretical Physics Supplement 96 (1988): 266–73. http://dx.doi.org/10.1143/ptps.96.266.

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32

Zhou, Li, Bo Ma, Yonghao Wang, and Yinan Zhu. "Hubble WFC3 Spectroscopy of the Rocky Planet L 98–59 b: No Evidence for a Cloud-free Primordial Atmosphere." Astronomical Journal 164, no. 5 (2022): 203. http://dx.doi.org/10.3847/1538-3881/ac8fe9.

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Abstract We are using archived data from HST of transiting exoplanet L 98-59 b to place constraints on its potentially hot atmosphere. We analyze the data from five transit visits and extract the final combined transmission spectrum using Iraclis. Then we use the inverse atmospheric retrieval code TauREx to analyze the combined transmission spectrum. There is a weak absorption feature near 1.40 μm and 1.55 μm in the transmission spectrum, which can be modeled by a cloudy atmosphere with abundant hydrogen cyanide (HCN). However, the unrealistically high abundance of HCN derived cannot be explai

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33

Yalinewich, Almog, and Matthew E. Caplan. "Crater morphology of primordial black hole impacts." Monthly Notices of the Royal Astronomical Society: Letters 505, no. 1 (2021): L115—L119. http://dx.doi.org/10.1093/mnrasl/slab063.

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ABSTRACT In this work, we propose a novel campaign for constraining relativistically compact massive compact halo object (MACHO) dark matter, such as primordial black holes (PBHs), using the Moon as a detector. PBHs of about 1019 to 1022 g may be sufficiently abundant to have collided with the Moon in the history of the Solar system. We show that the crater profiles of a PBH collision differ from traditional impactors and may be detectable in high-resolution lunar surface scans now available. Any candidates may serve as sites for in situ measurements to identify high-pressure phases of matter

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34

Alam, Munazza K., Peter Gao, Jea Adams Redai, et al. "JWST COMPASS: The First Near- to Mid-infrared Transmission Spectrum of the Hot Super-Earth L 168-9 b." Astronomical Journal 169, no. 1 (2024): 15. https://doi.org/10.3847/1538-3881/ad8eb5.

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Abstract We present the first broadband near- to mid-infrared (3–12 μm) transmission spectrum of the highly irradiated (T eq = 981 K) M-dwarf rocky planet L 168-9 b (TOI-134 b) observed with the Near-infrared Spectrograph and Mid-infrared Instrument (MIRI) instruments aboard JWST. We measure the near-infrared transit depths to a combined median precision of 20 ppm across the three visits in 54 spectroscopic channels with uniform widths of 60 pixels (∼0.2 μm wide; R ∼ 100), and the mid-infrared transit depths to 61 ppm median precision in 48 wavelength bins (∼0.15 μm wide; R ∼ 50). We compare t

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35

Micca Longo, Gaia, and Savino Longo. "The role of primordial atmosphere composition in organic matter delivery to early Earth." Rendiconti Lincei. Scienze Fisiche e Naturali 31, no. 1 (2020): 53–64. http://dx.doi.org/10.1007/s12210-020-00878-x.

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36

Howk, J. Christopher. "Interstellar Lithium as a probe of the primordial abundance." Proceedings of the International Astronomical Union 5, S268 (2009): 335–36. http://dx.doi.org/10.1017/s1743921310004357.

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AbstractThe cosmic abundance of lithium continues to represent a conundrum, as predictions from BBN theory are inconsistent with measurements in the atmospheres of the lowest-metallicity stars. While there are worries that modifications of the stellar Li abundances may play a role in this discrepancy, no satisfactory solution has yet been found. We suggest an alternate approach to studying the cosmic abundance of Li: measurements of interstellar gas-phase Li in low-metallicity environments.

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37

Jaupart, Etienne, Sebatien Charnoz, and Manuel Moreira. "Primordial atmosphere incorporation in planetary embryos and the origin of Neon in terrestrial planets." Icarus 293 (September 2017): 199–205. http://dx.doi.org/10.1016/j.icarus.2017.04.022.

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38

Dorfi, Ernst A., and Florian Ragossnig. "Interaction of solid bodies with atmospheres of protoplanets." Proceedings of the International Astronomical Union 14, S345 (2018): 351–52. http://dx.doi.org/10.1017/s1743921319001996.

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AbstractDuring the early stages of planet formation accretion of small bodies add mass to the planet and deposit their energy kinetic energy. Caused by frictional heating and/or large stagnation pressures within the dense and extended atmospheres most of the in-falling bodies get destroyed by melting or break-up before they impact on the planet’s surface. The energy is added to the atmospheric layers rather than heating the planet directly. These processes can significantly alter the physical properties of protoplanets before they are exposed with their primordial atmospheres to the early stel

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39

Molaverdikhani, K., Ch Helling, B. W. P. Lew, et al. "Understanding the atmospheric properties and chemical composition of the ultra-hot Jupiter HAT-P-7b." Astronomy & Astrophysics 635 (March 2020): A31. http://dx.doi.org/10.1051/0004-6361/201937044.

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Aims. The atmospheres of ultra-hot Jupiters (UHJs) are commonly considered to be at thermochemical equilibrium. We aim to provide disequilibrium chemistry maps for a global understanding of the chemistry in the atmosphere of HAT-P-7b and assess the importance of disequilibrium chemistry on UHJs. Methods. We applied a hierarchical modeling approach using 97 1D atmospheric profiles from a 3D general circulation model of HAT-P-7b. For each atmospheric 1D profile, we evaluated our kinetic cloud formation model consistently with the local gas-phase composition in chemical equilibrium. This served a

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Malaney, Robert A. "Lithium-6 Nucleosynthesis in the ISM." Highlights of Astronomy 10 (1995): 465–66. http://dx.doi.org/10.1017/s1539299600011771.

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The nucleosynthesis of 6Li in the galaxy has become of considerable interest in the past year. This is largely because of the exciting developments relating to the first detection of this isotope outside of our own solar system. Not only has 6Li been recently detected in the atmospheres of halo dwarfs [1-2], but also in the local interstellar medium (ISM) [3-4].It is well known that knowledge of the primordial abundance of the lithium isotopes has important ramifications for cosmology, through the constraints they impose on standard big bang nucleosynthesis (SBBN) [5], and those imposed on non

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Oberhausen, E. "Natürliche Strahlenexposition einschließlich Radon." Nuklearmedizin 30, S 05 (1991): 220–25. http://dx.doi.org/10.1055/s-0038-1629578.

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ZusammenfassungDie natürliche Strahlenexposition des Menschen wird durch die kosmische Strahlung und die in der Erdrinde vorhandenen primordialen Radionuklide verursacht. Da es durch die Wechselwirkung der kosmischen Strahlung in der Atmosphäre auch zur Bildung von Radionukliden kommt, werden durch beide Komponenten sowohl eine externe als auch eine interne Strahlenexposition durch Aufnahme von Radionukliden mit der Nahrungverursacht. Die externe Strahlenexposition nimmt wegen der kosmischen Strahlung mit der Höhe über dem Meeresspiegel zu und ist wegen der primordialen Radionuklide abhängig v

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42

Ferus, Martin, Fabio Pietrucci, Antonino Marco Saitta, et al. "Formation of nucleobases in a Miller–Urey reducing atmosphere." Proceedings of the National Academy of Sciences 114, no. 17 (2017): 4306–11. http://dx.doi.org/10.1073/pnas.1700010114.

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The Miller–Urey experiments pioneered modern research on the molecular origins of life, but their actual relevance in this field was later questioned because the gas mixture used in their research is considered too reducing with respect to the most accepted hypotheses for the conditions on primordial Earth. In particular, the production of only amino acids has been taken as evidence of the limited relevance of the results. Here, we report an experimental work, combined with state-of-the-art computational methods, in which both electric discharge and laser-driven plasma impact simulations were

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Swindle, T. D., and J. H. Jones. "The xenon isotopic composition of the primordial Martian atmosphere: Contributions from solar and fission components." Journal of Geophysical Research: Planets 102, E1 (1997): 1671–78. http://dx.doi.org/10.1029/96je03110.

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Biersteker, John B., and Hilke E. Schlichting. "Losing oceans: The effects of composition on the thermal component of impact-driven atmospheric loss." Monthly Notices of the Royal Astronomical Society 501, no. 1 (2020): 587–95. http://dx.doi.org/10.1093/mnras/staa3614.

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ABSTRACT The formation of the Solar system’s terrestrial planets concluded with a period of giant impacts. Previous works examining the volatile loss caused by the impact shock in the moon-forming impact find atmospheric losses of at most 20–30 per cent and essentially no loss of oceans. However, giant impacts also result in thermal heating, which can lead to significant atmospheric escape via a Parker-type wind. Here we show that H2O and other high-mean molecular weight outgassed species can be efficiently lost through this thermal wind if present in a hydrogen-dominated atmosphere, substanti

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Gräfener, Götz, and Wolf-Rainer Hamann. "Wolf-Rayet Wind Models from Hydrodynamic Model Atmospheres." Proceedings of the International Astronomical Union 3, S250 (2007): 63–70. http://dx.doi.org/10.1017/s1743921308020346.

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AbstractWe present a parameter study of WR-type mass loss, based on the PoWR hydrodynamic model atmospheres. These new models imply that optically thick WR-type winds are generally formed close to the Eddington limit. This is demonstrated for the case of hydrogen rich WNL stars, which turn out to be extremely massive, luminous stars with progenitor masses above ≈ 80 M⊙. We investigate the dependence of WR-type mass loss on various stellar parameters, including the metallicity Z. The results depend strongly on the L/M ratio, the stellar temperature T*, and the assumed wind clumping. For high L/

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46

Schroeder I, Isaac R. H. G., Kathrin Altwegg, Hans Balsiger, et al. "16O/18O ratio in water in the coma of comet 67P/Churyumov-Gerasimenko measured with the Rosetta/ROSINA double-focusing mass spectrometer." Astronomy & Astrophysics 630 (September 20, 2019): A29. http://dx.doi.org/10.1051/0004-6361/201833806.

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The European Space Agency spacecraft Rosetta accompanied the Jupiter-family comet 67P/Churyumov-Gerasimenko for over 2 yr along its trajectory through the inner solar system. Between 2014 and 2016, it performed almost continuous in situ measurements of the comet’s gaseous atmosphere in close proximity to its nucleus. In this study, the 16O/18O ratio of H2O in the coma of 67P/Churyumov-Gerasimenko, as measured by the ROSINA DFMS mass spectrometer onboard Rosetta, was determined from the ratio of H216O/H218O and 16OH/18OH. The value of 445 ± 35 represents an ~11% enrichment of 18O compared with

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Afshordi, N., R. B. Mann, and R. Pourhasan. "A holographic big bang?" International Journal of Modern Physics D 24, no. 12 (2015): 1544029. http://dx.doi.org/10.1142/s0218271815440290.

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We present a cosmological model in which the Universe emerges out of the collapse of a five-dimensional (5D) star as a spherical three-brane. The initial singularity of the big bang becomes hidden behind a causal horizon. Near scale-invariant primordial curvature perturbations can be induced on the brane via a thermal atmosphere that is in equilibrium with the brane, circumventing the need for a separate inflationary process and providing an important test of the model.

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Sasaki, Sho, and Kiyoshi Nakazawa. "Origin of isotopic fractionation of terrestrial Xe: hydrodynamic fractionation during escape of the primordial H2He atmosphere." Earth and Planetary Science Letters 89, no. 3-4 (1988): 323–34. http://dx.doi.org/10.1016/0012-821x(88)90120-3.

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Gibson, Carl H. "Turbulence in the Ocean, Atmosphere, Galaxy, and Universe." Applied Mechanics Reviews 49, no. 5 (1996): 299–315. http://dx.doi.org/10.1115/1.3101929.

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Flows in natural bodies of fluid often become turbulent, with eddy-like motions dominated by inertial-vortex forces. Buoyancy, Coriolis, viscous, self-gravitational, electromagnetic, and other force constraints produce a complex phase space of wave-like hydrodynamic states that interact with turbulence eddies, masquerade as turbulence, and preserve information about previous hydrodynamic states as fossil turbulence. Evidence from the ocean, atmosphere, galaxy and universe are compared with universal similarity hypotheses of Kolmogorov (1941, 1962) for turbulence velocity u, and extensions to s

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Mukhopadhyay, Sujoy, and Rita Parai. "Noble Gases: A Record of Earth's Evolution and Mantle Dynamics." Annual Review of Earth and Planetary Sciences 47, no. 1 (2019): 389–419. http://dx.doi.org/10.1146/annurev-earth-053018-060238.

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Noble gases have played a key role in our understanding of the origin of Earth's volatiles, mantle structure, and long-term degassing of the mantle. Here we synthesize new insights into these topics gained from high-precision noble gas data. Our analysis reveals new constraints on the origin of the terrestrial atmosphere, the presence of nebular neon but chondritic krypton and xenon in the mantle, and a memory of multiple giant impacts during accretion. Furthermore, the reservoir supplying primordial noble gases to plumes appears to be distinct from the mid-ocean ridge basalt (MORB) reservoir

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