Telescopic Observations of Lunar Hydration: Variations and Abundance

Honniball, C. I.; Lucey, P. G.; Ferrari-Wong, Chiara; Flom, Abigail; Li, Shuai; Kaluna, H. M.; Takir, D.

doi:10.1002/essoar.10502876.1

Cited by 2 publications

(2 citation statements)

References 40 publications

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“…This removes gravity-driven dry debris flows as a possible origin for the lobate features observed in Unit D. Following the logic established in previous works (e.g., Howard and Wilshire 1975;Hawke and Head 1977), the Unit D deposits would require the incorporation of liquid material to form the observed flow-like features. While some trace amounts of molecular water or water ice have been identified in the lunar regolith (Liu et al 2012;Honniball et al 2020) and in the permanently shadowed regions of the lunar poles (Li et al 2018), there is far less water present than would be necessary to cause such fluvial mobility of the identified deposits. This leaves only the inclusion of either volcanic melt or impact-generated melt.…”

Section: Units C and D-melt-bearing Ejecta Depositsmentioning

confidence: 99%

Morphologic mapping and interpretation of ejecta deposits from Tsiolkovskiy crater

Morse

Osinski

Tornabene

et al. 2021

Meteorit & Planetary Scien

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High-resolution images and elevation data sets from the Lunar Reconnaissance Orbiter along with spectral data from the Clementine mission are used to identify and map in detail the well-preserved Late Imbrian Tsiolkovskiy crater situated on the far side of the Moon. This study identifies five distinct morphologic units associated with Tsiolkovskiy crater and the surrounding ejecta blanket. Analysis of the spatial and stratigraphic relationships of each of the ejecta units shows an asymmetrical distribution of the overall ejecta blanket, as well as a consistent overprinting of ballistic ejecta by ponds and flows of impact melt-bearing material. This study shows that the asymmetric distribution of the ejecta blanket, including a distinct up-range "forbidden zone," is related to the impact direction and angle for the impactor that formed Tsiolkovskiy crater. The consistent presence of melt-bearing ponds and flows overlying the ballistic ejecta deposits indicates that two separate ejecta emplacement events occurred. We interpret this as an initial phase of ballistic ejecta emplacement during the excavation stage, followed by a second phase of melt-bearing ejecta emplacement. The second phase begins during the end of the excavation stage and continues throughout and beyond the modification stage of crater formation.

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Section: Units C and D-melt-bearing Ejecta Depositsmentioning

confidence: 99%

Morphologic mapping and interpretation of ejecta deposits from Tsiolkovskiy crater

Morse

Osinski

Tornabene

et al. 2021

Meteorit & Planetary Scien

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“…H 2 O exhibits a broad, shallow feature centered around 3.1 μm, while metal-OH, including in hydrated minerals that formed via aqueous alteration, exhibit a sharper, asymmetric feature centered around 2.7 μm (e.g., Clark 1999). The 3 μm region has been studied extensively on the Moon, which shows an absorption feature near 2.85 μm that has been linked to solar wind implantation or surficial H 2 O (Clark 2009;Pieters et al 2009;Sunshine et al 2009;McCord et al 2011;Wöhler et al 2017;Honniball et al 2020;Chauhan et al 2021;Laferriere et al 2022;Wilk et al 2024). The 3 μm band has also been extensively studied on the volatile-rich, carbonaceous C-type asteroids, some of which exhibit absorption at 2.7 μm or 3.1 μm with band depths as high as tens of percent (e.g., Campins et al 2010;Rivkin & Emery 2010;Takir & Emery 2012;Kitazato et al 2019;Rivkin et al 2022).…”

Section: Introductionmentioning

confidence: 99%

Detection of a 2.85 μm Feature on Five Spinel-rich Asteroids from JWST

Gomez Barrientos,

de Kleer,

Ehlmann

et al. 2024

ApJL

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Ground-based observations of “Barbarian” L-type asteroids at 1–2.5 μm indicate that their near-infrared spectra are dominated by the mineral spinel, which has been attributed to a high abundance of calcium-aluminum inclusions (CAIs)—the first solids to condense out of the protoplanetary disk during the formation of the solar system. However, the spectral properties of these asteroids from 2.5–5 μm, a wavelength region that covers signatures of hydrated minerals, water, and organics, have not yet been explored. Here, we present 2–5 μm reflectance spectra of five spinel-rich asteroids obtained with the NIRSpec instrument on the James Webb Space Telescope. All five targets exhibit a ∼2.85 μm absorption feature with a band depth of 3%–6% that appears correlated in strength with that of the 2 μm spinel absorption feature. The shape and position of the 2.85 μm feature are not a good match to the 2.7 μm feature commonly seen in carbonaceous CM meteorites or C-type asteroids. The closest spectral matches are to the Moon and Vesta, suggesting commonalities in aqueous alteration across silicate bodies, infall of hydrated material, and/or space weathering by solar wind H implantation. Lab spectra of CO/CV chondrites, CAIs, as well as the minerals cronstedtite and spinel, also show a similar feature, providing clues into the origin of the 2.85 μm feature.

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Telescopic Observations of Lunar Hydration: Variations and Abundance

Cited by 2 publications

References 40 publications

Morphologic mapping and interpretation of ejecta deposits from Tsiolkovskiy crater

Morphologic mapping and interpretation of ejecta deposits from Tsiolkovskiy crater

Detection of a 2.85 μm Feature on Five Spinel-rich Asteroids from JWST

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