A5089030798- Astro and Planetary Science
- Planetary Science and Exploration
- Space Exploration and Technology
- Geology and Paleoclimatology Research
- Isotope Analysis in Ecology
- Stellar, planetary, and galactic studies
- Geological and Geochemical Analysis
- Maritime and Coastal Archaeology
- Astronomy and Astrophysical Research
- Space Satellite Systems and Control
- Space Science and Extraterrestrial Life
- Archaeology and ancient environmental studies
- Historical Astronomy and Related Studies
- Methane Hydrates and Related Phenomena
- Astronomical and nuclear sciences
- Geomagnetism and Paleomagnetism Studies
- Geochemistry and Geologic Mapping
- Marine and environmental studies
- Gamma-ray bursts and supernovae
- Geological Studies and Exploration
- Geophysics and Gravity Measurements
- Geological formations and processes
- Geological and Geophysical Studies
- Astronomical Observations and Instrumentation
- Geological Formations and Processes Exploration
University of Münster
2021-2025
Max Planck Institute for Solar System Research
2018-2020
Freie Universität Berlin
2010-2019
Planetary Science Institute
2017
Planet
2012-2014
A New Dawn Since 17 July 2011, NASA's spacecraft has been orbiting the asteroid Vesta—the second most massive and third largest in solar system (see cover). Russell et al. (p. 684 ) use Dawn's observations to confirm that Vesta is a small differentiated planetary body with an inner core, represents surviving proto-planet from earliest epoch of formation; also confirmed as source howardite-eucrite-diogenite (HED) meteorites. Jaumann 687 report on asteroid's overall geometry topography, based...
INTRODUCTION Classic volcanism prevalent on terrestrial planets and volatile-poor protoplanets, such as asteroid Vesta, is based silicate chemistry often expressed by volcanic edifices (unless erased impact bombardment). In ice-rich bodies with sufficiently warm interiors, cryovolcanism involving liquid brines can occur. Smooth plains some icy satellites of the outer solar system have been suggested possibly cryovolcanic in origin. However, evidence for has proven elusive. Ceres a...
Thermochemical models have predicted that Ceres, is to some extent, differentiated and should an icy crust with few or no impact craters. We present observations by the Dawn spacecraft reveal a heavily cratered surface, heterogeneous crater distribution, apparent absence of large The morphology craters consistent ice in subsurface, which might favored relaxation, yet unrelaxed are also present. Numerous exhibit polygonal shapes, terraces, flowlike features, slumping, smooth deposits, bright...
Research Article| December 01, 2023 The Lunar Cratering Chronology H. Hiesinger; Hiesinger Institut für Planetologie, Westfälische Wilhelms-Universität, Wilhelm-Klemm-Str. 10, 48149 Münster, Germany hiesinger@uni-muenster.de; Search for other works by this author on: GSW Google Scholar C.H. van der Bogert; Bogert vanderbogert@uni-muenster.de G. Michael; Michael Institute of Geological Sciences, Planetary Sciences and Remote Sensing, Freie Universität Berlin, N. Schmedemann; Schmedemann W....
Abstract Prior to the arrival of Dawn spacecraft at Ceres, dwarf planet was anticipated be ice‐rich. Searches for morphological features related ice have been ongoing during Dawn's mission Ceres. Here we report identification pitted terrains associated with fresh Cerean impact craters. The exhibit strong similarities materials previously identified on Mars (where is implicated in pit development) and Vesta presence debated). We employ numerical models investigate formation Ceres discuss...
Abstract Craters on Ceres, such as Haulani, Kupalo, Ikapati, and Occator show postimpact modification by the deposition of extended plains material with pits, multiple lobate flows, widely dispersed deposits that form a diffuse veneer preexisting surface. Bright units in these features have negative spectral slope visible range, making it appear bluish respect to grey‐toned overall surface Ceres. We calculate drop height‐to‐runout length ratio several flow obtain coefficient friction <...
Abstract On Ceres, multispectral imaging data from the Dawn spacecraft show a distinct bluish characteristic for recently exposed material subsurface in, example, crater ejecta. Ejecta blankets of presumably old craters more reddish spectrum. We selected areas in which fresh Cerean was at specific time past, and no later geologic process is expected to have changed its surface composition or cratering record. For each area, we determined two color ratios retention age. The measured an...
The Sari\c{c}i\c{c}ek howardite meteorite shower consisting of 343 documented stones occurred on 2 September 2015 in Turkey and is the first fall. Cosmogenic isotopes show that experienced a complex cosmic ray exposure history, exposed during ~12-14 Ma regolith near surface parent asteroid, an ca.1 m sized meteoroid was launched by impact 22 +/- ago to Earth (as did one third all HED meteorites). SIMS dating zircon baddeleyite yielded 4550.4 2.5 4553 8.8 crystallization ages for basaltic...
Abstract Lunar impact craters can be used as a tool to derive information about the timing and sequence of emplacement geologic units surface processes on Moon. The production function (PF) derived from crater size‐frequency distribution (CSFD) measurements is an essential component in determining model age surface. PFs Neukum (1983) et al. (2001), https://doi.org/10.1007/978‐94‐017‐1035‐0_3 are defined only over diameter range between 10 m 300 km among most frequently PFs. However,...
Abstract The dwarf planet Ceres shows spatially well‐defined regions, which exhibit a negative (blue) spectral slope between 0.5 and 2.5 µm. Comparisons with planetary bodies known to blue properties of materials identified on Ceres's surface based infrared wavelength signatures indicate that the changes could be related physical material rather than variations in its composition. close association bluish regions fresh impact craters implies possible relationship an impact‐triggered...