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Minerals
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Ocean Worlds Mineralogy
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Ocean Worlds Mineralogy

A special issue of Minerals (ISSN 2075-163X). This special issue belongs to the section "Environmental Mineralogy and Biogeochemistry".

Deadline for manuscript submissions: closed (15 July 2022) | Viewed by 3807

Special Issue Editors

Dr. Maria Cristina De Sanctis

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Guest Editor
Istituto Nazionale di Astrofisica–Istituto di Astrofisica e Planetologia Spaziali, 00133 Rome, Italy
Interests: solar system science; planets and satellites; minor bodies and dwarf planets; space missions to solar system bodies; spectroscopy
Dr. Mauro Ciarniello

E-Mail Website
Guest Editor
Institute for Space Astrophysics and Planetology IAPS, National Institute of Astrophysics, 00133 Rome, Italy
Interests: planetary science; small bodies and dwarf planets; planetary rings; imaging spectroscopy; VIS-IR spectroscopy; photometry; radiative transfer in regoliths
Dr. Katrin Stephan

E-Mail Website
Guest Editor
Institute for Planetary Research, Deutsches Zentrum fur Luft- und Raumfahrt (DLR), D-12489 Berlin, Germany
Interests: imaging spectroscopy; mapping; hyperspectral remote sensing; hyperspectral image analysis; spatial analysis; satellite image processing; satellite image analysis; image processing; planetary science

Special Issue Information

Dear Colleagues,

We are pleased to announce the forthcoming Special Issue of Minerals entitled “Ocean Worlds Mineralogy”. The present issue seeks contributions focusing on the surface composition of outer Solar System bodies which may host or are known to host liquid water. Possible and confirmed ocean worlds are distributed among different classes of objects in the outer Solar System, from the asteroid main belt (Ceres), through the icy satellites of the giant planets (Europa, Ganymede, Callisto, Titan, Enceladus, Dione, and Triton), to Pluto. This is reflected in the variegated mineralogy, encompassing both refractory-dominated and volatile-rich surfaces.

We aim to collect results from the analysis of space-based and ground-based observations, including modeling and laboratory activity, which characterize the different mineralogical phases and their distribution in ocean worlds. We encourage contributions correlating the observed composition with the exogenic and endogenic processes shaping the target surfaces and investigating the connection between the surface geochemical properties and the subsurface liquid reservoirs. We also consider of particular interest the characterization of organic compounds in ocean worlds, and the link with the delivery and formation processes of organics on these targets, among which the chemistry of C-bearing molecules in a liquid environment is an ocean world prerogative. This appears to be of paramount importance for the identification of the paths leading to the formation of prebiotic material in extraterrestrial environments.

Dr. Maria Cristina De Sanctis
Dr. Mauro Ciarniello
Dr. Katrin Stephan

Guest Editors

Manuscript Submission Information

Manuscripts should be submitted online at www.mdpi.com by registering and logging in to this website. Once you are registered, click here to go to the submission form. Manuscripts can be submitted until the deadline. All submissions that pass pre-check are peer-reviewed. Accepted papers will be published continuously in the journal (as soon as accepted) and will be listed together on the special issue website. Research articles, review articles as well as short communications are invited. For planned papers, a title and short abstract (about 100 words) can be sent to the Editorial Office for announcement on this website.

Submitted manuscripts should not have been published previously, nor be under consideration for publication elsewhere (except conference proceedings papers). All manuscripts are thoroughly refereed through a single-blind peer-review process. A guide for authors and other relevant information for submission of manuscripts is available on the Instructions for Authors page. Minerals is an international peer-reviewed open access monthly journal published by MDPI.

Please visit the Instructions for Authors page before submitting a manuscript. The Article Processing Charge (APC) for publication in this open access journal is 2400 CHF (Swiss Francs). Submitted papers should be well formatted and use good English. Authors may use MDPI's English editing service prior to publication or during author revisions.

Keywords

  • ocean worlds
  • mineralogy
  • composition
  • planetary surfaces
  • dwarf planets
  • icy bodies
  • prebiotic chemistry

Published Papers (2 papers)

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Research

12 pages, 9528 KiB  
Article
Spectral Analysis of Ceres’ Main Linear Features
by Andrea Longobardo, Filippo Giacomo Carrozzo, Anna Galiano, Jennifer E. C. Scully, Rutu Parekh, Ernesto Palomba, Maria Cristina De Sanctis, Eleonora Ammannito, Andrea Raponi, Federico Tosi, Mauro Ciarniello, Francesca Zambon, Edoardo Rognini, Maria Teresa Capria, Carol A. Raymond and Christopher T. Russell
Minerals 2022, 12(8), 1013; https://0-doi-org.brum.beds.ac.uk/10.3390/min12081013 - 12 Aug 2022
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Abstract
Linear features are very common on asteroid surfaces. They are generally formed after impact and provide information about asteroid evolution. This work focuses on a mineralogical and spectral analysis of the main linear features on the 1/Ceres surface, having both tectonic (Samhain Catena’s [...] Read more.
Linear features are very common on asteroid surfaces. They are generally formed after impact and provide information about asteroid evolution. This work focuses on a mineralogical and spectral analysis of the main linear features on the 1/Ceres surface, having both tectonic (Samhain Catena’s pit chains) and geomorphic origins, i.e., generated by ejecta material (Occator ejecta, Dantu’s secondary radial chains, secondary radial chains generated from the Urvara impact). The analysis is based on spectral parameters defined by the Dawn’s VIR imaging spectrometer data, as albedo and depths of the bands centered at approximately 2.7, 3.1, 3.4 and 3.9 mm. The geomorphic linear features show spectral variations with respect to the surroundings, i.e., ammoniated phyllosilicates band depth shallowing is caused by the presence of material originating in a different region or dehydration caused by impact. The Samhain Catena does not show any mineralogical variation, due to its tectonic origin. The spectral behavior of Ceres’ linear features is similar to that observed on other asteroids (Vesta, Eros) and can be diagnostic in discerning the origin of linear features. Then, we searched spectral signatures of organics in the Samhain Catena region, since they are expected to form at depth due to internal processes: the absence of such signatures indicates that either they form at a larger depth or that their subsurface distribution is uneven. Full article
(This article belongs to the Special Issue Ocean Worlds Mineralogy)
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27 pages, 9411 KiB  
Article
VIS-NIR/SWIR Spectral Properties of H2O Ice Depending on Particle Size and Surface Temperature
by Katrin Stephan, Mauro Ciarniello, Olivier Poch, Bernard Schmitt, David Haack and Andrea Raponi
Minerals 2021, 11(12), 1328; https://0-doi-org.brum.beds.ac.uk/10.3390/min11121328 - 27 Nov 2021
Cited by 7 | Viewed by 1994
Abstract
Laboratory measurements were performed to study the spectral signature of H2O ice between 0.4 and 4.2 µm depending on varying temperatures between 70 and 220 K. Spectral parameters of samples with particle sizes up to ~1360 µm, particle size mixtures, and [...] Read more.
Laboratory measurements were performed to study the spectral signature of H2O ice between 0.4 and 4.2 µm depending on varying temperatures between 70 and 220 K. Spectral parameters of samples with particle sizes up to ~1360 µm, particle size mixtures, and different particle shapes were analyzed. The band depth (BD) of the major H2O-ice absorptions at 1.04, 1.25, 1.5, and 2 µm offers an excellent indicator for varying particle sizes in pure H2O ice. The spectral changes due to temperature rather, but not exclusively, affect the H2O-ice absorptions located at 1.31, 1.57, and 1.65 µm and the Fresnel reflection peaks at 3.1 and 3.2 µm, which strongly weaken with increasing temperature. As the BDs of the H2O-ice absorptions at 1.31, 1.57, and 1.65 µm increase, the band centers (BCs) of the H2O-ice absorptions at 1.25 and 1.5 µm slightly shift to shorter wavelengths. However, the BCs of the strong H2O-ice absorptions can also be affected by saturation in the case of large particles. The collected spectra provide a useful spectral library for future investigations of icy satellites such as Ganymede and Callisto, the major targets of ESA’s JUICE mission. Full article
(This article belongs to the Special Issue Ocean Worlds Mineralogy)
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