Relevant bibliographies by topics / Lunar outgassing

Academic literature on the topic 'Lunar outgassing'

Author: Grafiati
Published: 10 December 2022
Last updated: 28 January 2023

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Journal articles on the topic "Lunar outgassing"

1

Wilcoski, Andrew X., Paul O. Hayne, and Margaret E. Landis. "Polar Ice Accumulation from Volcanically Induced Transient Atmospheres on the Moon." Planetary Science Journal 3, no. 5 (May 1, 2022): 99. http://dx.doi.org/10.3847/psj/ac649c.

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Abstract Water ice exists at the lunar poles, but its origin, abundance, and distribution are not well understood. One potential source of water to the poles is the volcanic outgassing of volatiles from the lunar interior and subsequent condensation of erupted water vapor as surface ice. We investigate whether volcanic outgassing is a viable source for the accumulation of lunar polar water ice. We construct a model that accounts for volcanic outgassing, atmospheric escape to space, and surface ice accumulation over the period of peak lunar volcanic activity (4–2 Ga) and map the resulting water ice distribution and abundance using current surface temperature data from the Lunar Reconnaissance Orbiter. Our model suggests that ∼41% of the total H2O mass erupted over this period could have condensed as ice in the polar regions, with thicknesses up to several hundreds of meters. The south pole accumulates roughly twice the ice mass of the north, and the southern deposits are thicker. Typical modeled eruptions generate collisional atmospheres with lifetimes of ∼2500 yr. However, these atmospheres are episodic and generally do not persist between eruptions. Roughly 15% of an atmosphere’s water vapor mass forms a frost on the lunar nightside, while the transient atmosphere persists. Our work suggests that the volcanically active period of the early Moon would have been punctuated by short-lived, collisional atmospheres that enabled the efficient sequestration of large quantities (8.2 × 1015 kg) of water ice at the poles and the temporary diurnal availability of water ice and vapor at all latitudes.
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2

Boyce, Jeremy W., Allan H. Treiman, Yunbin Guan, Chi Ma, John M. Eiler, Juliane Gross, James P. Greenwood, and Edward M. Stolper. "The chlorine isotope fingerprint of the lunar magma ocean." Science Advances 1, no. 8 (September 2015): e1500380. http://dx.doi.org/10.1126/sciadv.1500380.

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The Moon contains chlorine that is isotopically unlike that of any other body yet studied in the Solar System, an observation that has been interpreted to support traditional models of the formation of a nominally hydrogen-free (“dry”) Moon. We have analyzed abundances and isotopic compositions of Cl and H in lunar mare basalts, and find little evidence that anhydrous lava outgassing was important in generating chlorine isotope anomalies, because 37Cl/35Cl ratios are not related to Cl abundance, H abundance, or D/H ratios in a manner consistent with the lava-outgassing hypothesis. Instead, 37Cl/35Cl correlates positively with Cl abundance in apatite, as well as with whole-rock Th abundances and La/Lu ratios, suggesting that the high 37Cl/35Cl in lunar basalts is inherited from urKREEP, the last dregs of the lunar magma ocean. These new data suggest that the high chlorine isotope ratios of lunar basalts result not from the degassing of their lavas but from degassing of the lunar magma ocean early in the Moon’s history. Chlorine isotope variability is therefore an indicator of planetary magma ocean degassing, an important stage in the formation of terrestrial planets.
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3

Day, James M. D., Frédéric Moynier, and Charles K. Shearer. "Late-stage magmatic outgassing from a volatile-depleted Moon." Proceedings of the National Academy of Sciences 114, no. 36 (August 21, 2017): 9547–51. http://dx.doi.org/10.1073/pnas.1708236114.

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The abundance of volatile elements and compounds, such as zinc, potassium, chlorine, and water, provide key evidence for how Earth and the Moon formed and evolved. Currently, evidence exists for a Moon depleted in volatile elements, as well as reservoirs within the Moon with volatile abundances like Earth’s depleted upper mantle. Volatile depletion is consistent with catastrophic formation, such as a giant impact, whereas a Moon with Earth-like volatile abundances suggests preservation of these volatiles, or addition through late accretion. We show, using the “Rusty Rock” impact melt breccia, 66095, that volatile enrichment on the lunar surface occurred through vapor condensation. Isotopically light Zn (δ66Zn = −13.7‰), heavy Cl (δ37Cl = +15‰), and high U/Pb supports the origin of condensates from a volatile-poor internal source formed during thermomagmatic evolution of the Moon, with long-term depletion in incompatible Cl and Pb, and lesser depletion of more-compatible Zn. Leaching experiments on mare basalt 14053 demonstrate that isotopically light Zn condensates also occur on some mare basalts after their crystallization, confirming a volatile-depleted lunar interior source with homogeneous δ66Zn ≈ +1.4‰. Our results show that much of the lunar interior must be significantly depleted in volatile elements and compounds and that volatile-rich rocks on the lunar surface formed through vapor condensation. Volatiles detected by remote sensing on the surface of the Moon likely have a partially condensate origin from its interior.
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4

Crotts, Arlin P. S., and Cameron Hummels. "LUNAR OUTGASSING, TRANSIENT PHENOMENA, AND THE RETURN TO THE MOON. II. PREDICTIONS AND TESTS FOR OUTGASSING/REGOLITH INTERACTIONS." Astrophysical Journal 707, no. 2 (December 7, 2009): 1506–23. http://dx.doi.org/10.1088/0004-637x/707/2/1506.

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5

Crotts, Arlin P. S. "Lunar Outgassing, Transient Phenomena, and the Return to the Moon. I. Existing Data." Astrophysical Journal 687, no. 1 (November 2008): 692–705. http://dx.doi.org/10.1086/591634.

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6

Zhang, Tao, Xilun Ding, Kun Xu, Shuting Liu, Li He, Haifei Zhu, and Yisheng Guan. "Evacuation method and outgassing rate of a lunar regolith simulant for deep drilling tests." Acta Astronautica 157 (April 2019): 455–64. http://dx.doi.org/10.1016/j.actaastro.2019.01.022.

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7

Su, Xue, Youxue Zhang, Yang Liu, and Robert M. Holder. "Outgassing and in-gassing of Na, K and Cu in lunar 74220 orange glass beads." Earth and Planetary Science Letters 602 (January 2023): 117924. http://dx.doi.org/10.1016/j.epsl.2022.117924.

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8

Landis, Margaret E., Paul O. Hayne, Jean-Pierre Williams, Benjamin T. Greenhagen, and David A. Paige. "Spatial Distribution and Thermal Diversity of Surface Volatile Cold Traps at the Lunar Poles." Planetary Science Journal 3, no. 2 (February 1, 2022): 39. http://dx.doi.org/10.3847/psj/ac4585.

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Abstract The polar regions of the Moon host some of the most extreme low temperatures in the inner solar system due to its low obliquity, lack of atmosphere, and topographic relief. Some of these regions are already confirmed to host water ice. Proposed sources of water and other volatiles include lunar volcanic outgassing, solar wind, and comet impacts. Each of these possible sources would carry a potentially identifiable compositional signature beyond water. Determining the dominant sources of lunar volatiles, therefore, requires assessing the long-term thermal stability of an array of compounds. We present results of mapping the surface thermal stability locations of multiple key volatiles, including water, from the Diviner Lunar Radiometer data from 60° to 90° latitude in both hemispheres. We find the annual maximum temperature for each pixel of interest in the map (∼300 m) to determine which volatiles of interest would be stable there. We report on the thermal stability area of each volatile, as well as the geologic context in some cases. We find that while the thermal stability area for volatiles is larger in the south pole generally, both the north pole and south pole host areas where potential tracer volatiles from lunar volcanism, solar wind, and cometary impacts would be thermally stable for billions of years if such volatiles were ever delivered. We find several areas equatorward of ∼80° on the lunar nearside that could host water ice, where future missions could potentially access volatile deposits in order to place constraints on water delivery to the Moon.
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9

A’Hearn, Michael F. "The Deep Impact Project." Highlights of Astronomy 13 (2005): 746–48. http://dx.doi.org/10.1017/s1539299600017007.

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AbstractThe Deep Impact mission aims at understanding the third dimension of a cometary nucleus, the physical and chemical properties as a function of depth below the surface. General wisdom holds that comets, because they are small and spend most of their lives far from the sun, hold primordial ices in their interiors. However, it is universally agreed that the surface layers have evolved, whether from cosmic rays while residing in the Oort cloud or from solar heating during previous perihelion passages. Clearly, in order to interpret surface observations and outgassing, we must understand how the surface layers differ from the interior. Deep Impact is the first mission to carry out a macroscopic experiment on a planetary body since the Apollo program dropped a lunar module on the moon and measured the seismic response.
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10

Lawson, Stefanie L. "Recent outgassing from the lunar surface: The Lunar Prospector Alpha Particle Spectrometer." Journal of Geophysical Research 110, E9 (2005). http://dx.doi.org/10.1029/2005je002433.

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