|Title||Tectono-magmatic, sedimentary and hydrothermal history of Arsinoes and Pyrrhae Chaos, Mars|
|Publication Type||Journal Article|
|Year of Publication||2020|
|Authors||Luzzi E, Rossi APio, Carli C, Altieri F|
|Journal||Submitted for publication in Journal of Geophysical Research : Planets|
Arsinoes and Pyrrhae Chaos are two adjacent chaotic terrains located east to Valles Marineris and west to Arabia Terra, on Mars. In this work we produced a morpho-stratigraphic map of the area, characterized by a volcanic bedrock disrupted into polygonal mesas and knobs (Chaotic Terrain Unit) and two non-disrupted units interpreted as sedimentary and presenting a spectral variation, likely associated to hydrated minerals. The reconstructed geological history of the area starts with the collapse that caused the formation of the chaotic terrains. Since volcano-tectonic evidences are widespread all-over the area (e.g. fissure vents/graben, radial and concentric systems of faults, y-shaped conjunctions, lava flows, pit chains), and an intricate system of lava conduits is hypothesized for the occurrence of such features, we propose the possibility that the whole collapse was caused primarily by volcano-tectonic processes. On Earth, polygonal blocks and systems of concentric + radial fissures are originated in the frame of a particular caldera collapse called chaotic or piecemeal. In the study area on Mars, the chaotic collapse would have been triggered by repeated inflation and deflation of a putative magma chamber in depth under the terrain. In a late stage, after the end of the volcano-tectonic activity, a lacustrine/evaporitic depositional environment could have set, with the deposition of the non-disrupted units. The hydrated minerals found in the periphery of the Chaos could be the result of hydrothermal alteration of the basaltic bedrock.
Title Surface Expressions of Subsurface Sediment Mobilization Rooted into a Gas Hydrate-Rich Cryosphere on Mars Publication Type Journal Article Year of Publication 2019 Authors De Toffoli B, Pozzobon R, Massironi M, Mazzarini F, Conway S, Cremonese G Journal Scientific Reports Volume 9 ISSN 2045-2322 URL http://www.nature.com/articles/s41598-019-45057-7 DOI 10.1038/s41598-019-45057-7
Title Global-scale brittle plastic rheology at the cometesimals merging of comet 67P/Churyumov–Gerasimenko Publication Type Journal Article Year of Publication 2020 Authors Franceschi M, Penasa L, Massironi M, Naletto G, Ferrari S, Fondriest M, Bodewits D, Güttler C, Lucchetti A, Mottola S, Pajola M, Toth I, Deller J, Sierks H, Tubiana C Journal Proceedings of the National Academy of Sciences Pagination 201914552 ISSN 0027-8424, 1091-6490 URL http://www.pnas.org/lookup/doi/10.1073/pnas.1914552117 DOI 10.1073/pnas.1914552117
Title Abundance and size-frequency distributions of boulders in Linne crater's ejecta (Moon) Publication Type Journal Article Year of Publication 2018 Authors Pajola M, Pozzobon R, Lucchetti A, Rossato S, Baratti E, Galluzzi V, Cremonese G Journal arXiv:1812.00590 [astro-ph] Date Published dec Keywords Astrophysics - Earth and Planetary Astrophysics Abstract
This paper presents the abundances and the size-frequency distributions (SFD) of the ejected boulders surrounding the Linne crater, located on the Moon's Mare Serenitatis basin. By means of Lunar Reconnaissance Orbiter Camera high-resolution images we prepare a context geological map of the Linne crater as well as we identify 12000 boulders > 4.4 m, with a maximum measured size of 30.8 m. The cumulative number of boulders per km2 is fitted with a power-law curve with index -4.03 +0.09/-0.10. By studying the radial ejecta abundances, we find that the largest ones are located within the first 2 km from the crater's centre, while few tens of boulders with sizes < 8 m are detectable above 5 km from the crater's rim. We find that the Linne proximal ejecta blanket is slightly asymmetrical, as indicated in the geological map too, showing a density increase in the NE-SW direction. This may be the result of an oblique impact emplacement of the original impactor, or it may be explained with a perpendicular impact in the Mare Serenitatis location, but on a surface with lunar basalts with different local mechanical properties. By exploiting our boulders size density as a function of the distance from the crater's centre, we derive a possible regolith thickness at the Linne impact of 4.75 m, supporting similar values based on Earth-based radar and optical data in the Mare Serenitatis basin.
Title Geologic History of the Northern Portion of the South Pole-Aitken Basin on the Moon Publication Type Journal Article Year of Publication 2018 Authors Ivanov M.A, Hiesinger H., van der Bogert C.H, Orgel C., Pasckert J.H, Head J.W Journal Journal of Geophysical Research: Planets Volume 123 Pagination 2585–2612 ISSN 21699097 URL http://doi.wiley.com/10.1029/2018JE005590 DOI 10.1029/2018JE005590
Title Geology of the Hokusai quadrangle (H05), Mercury Publication Type Journal Article Year of Publication 2019 Authors Wright J, Rothery DA, Balme MR, Conway SJ Journal Journal of Maps Volume 15 Pagination 509–520 ISSN 1744-5647 URL https://www.tandfonline.com/doi/full/10.1080/17445647.2019.1625821 DOI 10.1080/17445647.2019.1625821
Title 3D digital outcrop model reconstruction of the Kimberley outcrop (Gale crater, Mars) and its integration into Virtual Reality for simulated geological analysis Publication Type Journal Article Year of Publication 2020 Authors Caravaca G, Le Mouélic S, Mangold N, L’Haridon J, Le Deit L, Massé M Journal Planetary and Space Science Volume 182 Pagination 104808 ISSN 00320633 URL https://linkinghub.elsevier.com/retrieve/pii/S0032063319302600 DOI 10.1016/j.pss.2019.104808
Title Geological mapping and chronology of lunar landing sites: Apollo 11 Publication Type Journal Article Year of Publication 2019 Authors Iqbal W., Hiesinger H., van der Bogert C.H. Journal Icarus Volume 333 Pagination 528–547 ISSN 00191035 URL https://linkinghub.elsevier.com/retrieve/pii/S0019103518307772 DOI 10.1016/j.icarus.2019.06.020