Results 41 to 50 of about 2,944 (214)

The missing large impact craters on Ceres

Nature Communications, 2016
Studying craters on atmosphere-less bodies can unlock information about planetesimal histories. Here, Marchi et al. present results from the NASA Dawn mission to Ceres showing that craters >100–150 km in size are largely absent, and find that Ceres ...
S. Marchi, A. I. Ermakov, C. A. Raymond, R. R. Fu, D. P. O’Brien, M. T. Bland, E. Ammannito, M. C. De Sanctis, T. Bowling, P. Schenk, J. E. C. Scully, D. L. Buczkowski, D. A. Williams, H. Hiesinger, C. T. Russell   +14 more
doaj   +1 more source

Silicate–sulfide interaction within quenched melts of space weathered Ryugu grains

Meteoritics &Planetary Science, Volume 60, Issue 7, Page 1480-1501, July 2025.
Abstract The first few microns of the surface of airless bodies are subject to severe changes due to the harsh environment of space, known as space weathering. The Hayabusa2 sample return mission from the asteroid Ryugu provides the first opportunity to study these effects on a carbonaceous and hydrated body.
Sylvain Laforet, Hugues Leroux, Corentin Le Guillou, Maya Marinova, Adrien Néri, Adrien Teurtrie, Francisco de la Peña, Damien Jacob, Alexandre Fadel, David Troadec   +9 more
wiley   +1 more source

Dust Evolution and the Formation of Planetesimals [PDF]

Space Science Reviews, 2016
The solid content of circumstellar disks is inherited from the interstellar medium: dust particles of at most a micrometer in size. Protoplanetary disks are the environment where these dust grains need to grow at least 13 orders of magnitude in size. Our understanding of this growth process is far from complete, with different physics seemingly posing ...
Anders Johansen, Tilman Birnstiel, Tilman Birnstiel, M. Fang   +3 more
openaire   +4 more sources

Selective sampling of asteroids, the Moon, and Mars: Factors affecting the numerical abundances of members of meteorite groups

Meteoritics &Planetary Science, Volume 60, Issue 7, Page 1502-1519, July 2025.
Abstract Meteorite collection inventories show that many related meteorite groups have very different numerical abundances (e.g., lunar versus Martian meteorites; Eagle Station pallasites versus main‐group pallasites; eucrites versus diogenites; ungrouped Antarctic irons versus ungrouped non‐Antarctic irons; carbonaceous chondrite‐related (CC) iron ...
Alan E. Rubin
wiley   +1 more source

Formation of pebble-pile planetesimals [PDF]

Astronomy & Astrophysics, 2014
The first stage of planet formation is the accumulation of dust and ice grains into mm-cm-sized pebbles. These pebbles can clump together through the streaming instability and form gravitationally bound pebble 'clouds'. Pebbles inside such a cloud will undergo mutual collisions, dissipating energy into heat.
Karl Wahlberg Jansson, Anders Johansen
openaire   +3 more sources

Magnesium phosphate in the Cold Bokkeveld (CM2) carbonaceous chondrite

Meteoritics &Planetary Science, EarlyView.
Abstract Hydrous Mg‐phosphate was first described from astromaterials in particles returned from the C‐type asteroid Ryugu, and has subsequently been found in samples of the B‐type asteroid Bennu and CI1 carbonaceous chondrites. This phase may have been highly significant as a source of bioessential compounds for early Earth.
Martin R. Lee, Tobias Salge, Ian Maclaren   +2 more
wiley   +1 more source

The Influence of Interior Structure and Thermal State on Impact Melt Generation Upon Large Impacts Onto Terrestrial Planets

Journal of Geophysical Research: Planets, Volume 130, Issue 7, July 2025.
Abstract We investigate the melt production of planetary impacts as a function of planet size (R/REarth $R/{R}_{\text{Earth}}$ = 0.1–1.5), impactor size (L $L$ = 1–1,000 km), and core size ratio (Rcore/R ${R}_{\text{core}}/R$ = 0.2–0.8) using a combination of parameterized convection models and fully dynamical 2D impact simulations.
Lukas Manske, Thomas Ruedas, Ana‐Catalina Plesa, Philipp Baumeister, Nicola Tosi, Natalia Artemieva, Kai Wünnemann   +6 more
wiley   +1 more source

Streaming Instability and Turbulence: Conditions for Planetesimal Formation

The Astrophysical Journal
The streaming instability (SI) is a leading candidate for planetesimal formation, which can concentrate solids through two-way aerodynamic interactions with the gas.
Jeonghoon Lim, Jacob B. Simon, Rixin Li, Philip J. Armitage, Daniel Carrera, Wladimir Lyra, David G. Rea, Chao-Chin Yang, Andrew N. Youdin   +8 more
doaj   +1 more source

Evidence for phosphate metasomatism in an olivine‐rich achondrites

Meteoritics &Planetary Science, Volume 60, Issue 6, Page 1302-1317, June 2025.
Abstract Brachinites, brachinite‐like achondrites (BLA), and other similar primitive achondrites offer important constraints on differentiation processes of the earliest formed planetesimals, as they quenched amidst early differentiation processes on their parent body. Geochemical data for all major mineral phases in two previously poorly characterized
Robert W. Nicklas, Melody Z.‐A. Chen, Evan J. Saltman, Ethan F. Baxter, Andrew J. Lonero, Anthony B. Love   +5 more
wiley   +1 more source

Planetesimal Growth in Evolving Protoplanetary Disks: Constraints from the Pebble Supply

The Astrophysical Journal, 2023
In the core accretion model, planetesimals grow by mutual collisions and engulfing millimeter-to-centimeter particles, i.e., pebbles. Pebble accretion can significantly increase the accretion efficiency and help explain the presence of planets on wide ...
Tong Fang, Hui Zhang, Shangfei Liu, Beibei Liu, Hongping Deng   +4 more
doaj   +1 more source