¹Mireia Leon-Dasi, ²Sebastien Besse, ³Lauren M. Jozwiak, ⁴Erica R. Jawin, ¹Alain Doressoundiram
Icarus (in Press) Open Access Link to Article [https://doi.org/10.1016/j.icarus.2024.11642]
¹LESIA, Observatoire de Paris, Université PSL, CNRS, 5 Place Jules Janssen, Meudon, 92195, France
²European Space Agency (ESA), European Space Astronomy Centre (ESAC), Camino Bajo del Castillo s/n, Villanueva de la Cañada, 28692, Spain
³Planetary Exploration Group, Johns Hopkins University Applied Physics Laboratory, 1101 Johns Hopkins Road, Laurel, 20723, MD, United States
⁴Smithsonian Institution, National Air and Space Museum, 600 Independence Ave, Washington, 20560, DC, United States
Copyright Elsevier

Explosive volcanic activity on Mercury extended after the end of the widespread effusive volcanism era. While prior research has recognized a prolonged period of explosive volcanic activity, the specific eruption timing for individual pyroclastic deposits remains unknown. In this study, we explore the evolution of explosive volcanism by examining the relationship between the morphological degradation of the vents and spectral changes in the associated deposits. We find a diverse range of spectral properties in pyroclastic deposits, which are typically characterized by increased brightness, a red spectral slope, and a higher curvature compared to the average surface. Rather than presenting a unique spectral signature, these deposits exhibit spectral parameters that span the range of most units on Mercury. We observe a trend between the deposit spectra and the vent degradation characterized by a rapid initial darkening and flattening over time followed by stabilization. The oldest deposits reach a steady state with no further spectral changes. To explain these temporal variations in spectral properties, we propose three potential processes: space weathering, mixing with the background and changes in pyroclast size over time. We examine the implications of space weathering on spectral properties and discuss the eruption timeline for each scenario. The saturation of spectral changes induced by space weathering acts over a period of 1 Gyr. We suggest that a large portion of the pyroclastic deposits identified to date, which have a marked spectral contrast with the surrounding terrain, have been emplaced by recent explosive volcanic eruptions.

¹B.G. Rider-Stokes, ¹S.L. Jackson, ^2,3T.H. Burbine, ¹L.F. White, ¹R.C. Greenwood, ⁴E.M. MacLennan, ¹M. Anand, ⁵A. Yamaguchi, ¹M.M. Grady
Icarus (in Press) Link to Article [https://doi.org/10.1016/j.icarus.2024.116429]
¹School of Physical Sciences, The Open University, Milton Keynes MK7 6AA, UK
²Department of Astronomy, Mount Holyoke College, 50 College Street, South Hadley, MA 01075, USA
³Planetary Science Institute, 1700 East Fort Lowell, Suite 106, Tucson, AZ 85719, USA
⁴Department of Physics, University of Helsinki, Finland
⁵National Institute of Polar Research, Tachikawa, Tokyo 190-8518, Japan
Copyright Elsevier

It is hypothesized that the Solar System was once populated by Moon to Mars-sized planetary embryos, however, resulting debris from their disruptions is not easily discernible in the modern-day Solar System. Angrites are among the oldest differentiated materials in our Solar System, recording prolonged magmatism, and their parent body is expected to have been Moon to Mars-sized. Even so, no parent body in the modern-day Solar System has been identified. Our UV–Vis-NIR spectra of ten angrites, compared with 712 asteroids, reveal multiple candidates with spectral similarities through curve matching and band-structure analysis. Asteroid (246) Asporina provides the best analog for the angrite meteorites, potentially representing a fragment of a long-lost Moon to Mars-sized body that once resided in the inner Solar System, which was subsequently incorporated into the growing terrestrial planets.