An Exogenic Origin for the Volatiles Sampled by the LCROSS Impact

Mandt, K.; Mousis, O.; Hurley, D. M.; Bouquet, Alexis; Retherford, K. D.; Magaña, L. O.; Luspay‐Kuti, A.

doi:10.21203/rs.3.rs-777152/v1

Cited by 3 publications

(2 citation statements)

References 36 publications

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“…Our 1D model is based on the diffusion equation applied in our photochemical model previously applied to Titan (de La Haye et al 2008;Mandt et al 2012aMandt et al , 2012b, Pluto (Luspay-Kuti et al 2017;Mandt et al 2017), and Triton (Mandt & Luspay-Kuti 2019). This model calculates the abundance of atmospheric species as a function of altitude based on the composition of the atmosphere at the surface, the temperature profile, and diffusion processes.…”

Section: Scope Of This Studymentioning

confidence: 99%

TRAPPIST-1h as an Exo-Titan. I. The Role of Assumptions about Atmospheric Parameters in Understanding an Exoplanet Atmosphere

Mandt

Luspay‐Kuti

Lustig‐Yaeger

et al. 2022

ApJ

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The TRAPPIST-1 system is home to at least seven terrestrial planets and is a target of interest for future James Webb Space Telescope (JWST) observations. Additionally, these planets will be of interest to future missions making observations in the ultraviolet (UV). Although several of these planets are located in the traditional habitable zone, where liquid water could exist on the surface, TRAPPIST-1h is interesting to explore as a potentially habitable ocean world analog. In this study, we evaluate the observability of a Titan-like atmosphere on TRAPPIST-1h. The ability of the JWST or a future UV mission to detect specific species in the atmosphere at TRAPPIST-1h will depend on how far each species extends from the surface. In order to understand the conditions required for detection, we evaluate the input parameters used in one-dimensional models to simulate the structure of Titan-like atmospheres. These parameters include surface temperature and pressure, temperature profile as a function of distance from the surface, composition of the minor species relative to N2, and the eddy diffusion coefficient. We find that JWST simulated spectra for cloud- and haze-free atmospheres are most sensitive to surface temperature, temperature gradients with altitude, and surface pressure. The importance of temperature gradients in JWST observations shows that a simple isothermal scale height is not ideal for determining temperature or atmospheric mean molecular mass in transit spectra from exoplanet atmospheres. We demonstrate that UV transmission spectra are sensitive to the upper atmosphere, where the exobase can be used to approximate the vertical extent of the atmosphere.

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Section: Scope Of This Studymentioning

confidence: 99%

TRAPPIST-1h as an Exo-Titan. I. The Role of Assumptions about Atmospheric Parameters in Understanding an Exoplanet Atmosphere

Mandt

Luspay‐Kuti

Lustig‐Yaeger

et al. 2022

ApJ

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“…A confirmation of the presence of water ice itself came in 2009 with the impact of the Lunar CRater Observation and Sensing Satellite (LCROSS) into Cabeus crater, which identified spectroscopic signatures of water ice in the ejected debris plume from the sediment within the PSR (Colaprete et al., 2010). Further analysis of the spectroscopic signatures suggests that this ice likely was cometary in origin (Mandt et al., 2022).…”

Section: Introductionmentioning

confidence: 99%

Seasons of Ice: Water Ice Migration and Seasonal Transient Shadow at the Lunar Poles

Luchsinger

Chanover

2022

JGR Planets

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Lunar water ice can be broadly categorized as belonging to one of two populations: deep, ancient, stable deposits, and shallow, transient, recent deposits. However, a third state for lunar ice is also possible. Temporary sequestration occurs when ice is deposited into a transiently shadowed region at the lunar poles. These temporarily sequestered ice deposits are unstable over geologic time scales, but in the short term, are capable of a wide range of migration, sublimation, and retention patterns due to their thermally dependent sublimation and migration rates. We developed a model to characterize the range of possible migration and retention behaviors for temporarily sequestered ice deposits within locations with dynamic illumination conditions. We found that water ice migration, sublimation, and retention varies across the lunar polar environment, with neighboring locations experiencing different illumination and thermal conditions. We found that the residence times of temporarily sequestered ice deposits in some high latitude, non‐shadowed regions can be similar to or greater than the length of time spent above the long term stability temperature of ice during lunar winter months, leading to incomplete removal of surface or near surface ice during the day. We also found that shallowly buried, unstable ice deposits take longer to sublimate than surface deposits, leading to a temporal lag in escaping ice. This work suggests that temporary sequestration can lead to complex ice migration and retention patterns at high latitudes, with ice sublimation efficiency varying across the lunar polar environment due to local, small scale differences in illumination conditions.

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Estimation of the Influence of Contamination by Rocket Fuel Combustion Products on the Chemical and Isotopic Composition of the Lunar Regolith in the Polar Regions

Lorenz

Basilevsky²,

Dolgopolov³

et al. 2023

Advances in Geochemistry, Analytical Chemistry, and Planetary Sciences

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An Exogenic Origin for the Volatiles Sampled by the LCROSS Impact

Cited by 3 publications

References 36 publications

TRAPPIST-1h as an Exo-Titan. I. The Role of Assumptions about Atmospheric Parameters in Understanding an Exoplanet Atmosphere

TRAPPIST-1h as an Exo-Titan. I. The Role of Assumptions about Atmospheric Parameters in Understanding an Exoplanet Atmosphere

Seasons of Ice: Water Ice Migration and Seasonal Transient Shadow at the Lunar Poles

Estimation of the Influence of Contamination by Rocket Fuel Combustion Products on the Chemical and Isotopic Composition of the Lunar Regolith in the Polar Regions

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