Results 71 to 80 of about 3,499 (221)

CI chondrite Oued Chebeika 002 links asteroids Bennu and Ryugu to common parent body

Meteoritics &Planetary Science, Volume 61, Issue 5, Page 801-818, May 2026.
Abstract CI chondrites are a compositionally primitive group of meteorites that have undergone extensive aqueous alteration, providing insights into the evolution of primitive planetesimals. Oued Chebeika 002 is the most pristine CI chondrite to date.
Megan Broussard, Katharina Lodders, Paul K. Carpenter, Piers Koefoed, Karen Ziegler, Kunihiko Nishiizumi, Marc W. Caffee, Laurence A. J. Garvie, Ryan C. Ogliore, Anthony J. Irving, Bradley L. Jolliff, Kun Wang   +11 more
wiley   +1 more source

On the filtering and processing of dust by planetesimals 1. Derivation of collision probabilities for non-drifting planetesimals

, 2013
A&A, 572, A72 (2014). 31 pages, 29 figures. (Final version)International audienceContext. Circumstellar disks are known to contain a significant mass in dust ranging from micron to centimeter size.
Guillot, Tristan, Tristan Guillot, Ida, Shigeru, Chris W. Ormel, Ormel, Chris, W., Ormel, Chris,, Shigeru Ida   +6 more
core   +1 more source

Planetesimal Drift in Eccentric Disks: Possible Outward Migration

The Astrophysical Journal
Radial drift of solid particles in the protoplanetary disk is often invoked as a threat to planet formation, as it removes solid material from the disk before it can be assembled into planets.
Kedron Silsbee
doaj   +1 more source

The Efficient Delivery of Highly Siderophile Elements to the Core Creates a Mass Accretion Catastrophe for the Earth

Journal of Geophysical Research: Planets, Volume 131, Issue 4, April 2026.
Abstract The excess abundance of highly siderophile elements (HSEs), as inferred for the terrestrial planets and the Moon, is thought to record a “late veneer” of impacts after the giant impact phase of planet formation. Estimates for total mass accretion during this period typically assume all HSEs delivered remain entrained in the mantle.
Richard J. Anslow, Maylis Landeau, Amy Bonsor, Jonathan Itcovitz, Oliver Shorttle   +4 more
wiley   +1 more source

Planetesimals Around White Dwarfs [PDF]

, 2014
Evidence is convincing that a big fraction of extrasolar planetesimals can survive the red giant stage of a star and persist into the white dwarf phase. We argue that eventually, some of them do get perturbed into the tidal radius of the white dwarf and ...
Xu, Siyi
core  

Pebbles versus planetesimals The outcomes of population synthesis models

, 2020
In the core accretion scenario, a massive core forms first and then accretes an envelope. When discussing how this core forms some divergences appear.
Coleman, G. A. L., W. Benz, Y. Alibert, Alibert, Y., Jungo, N., Benz, W, Burn, R., Brugger, N, R. Burn, Burn, R, Alibert, Y, Coleman, GAL, Benz, W., N. Brügger, G. A. L. Coleman   +14 more
core   +1 more source

Size–Frequency Distribution of Terrestrial Leftover Planetesimals and S-complex Implanted Asteroids

The Astrophysical Journal
The isotopic composition of meteorites linked to S-complex asteroids has been used to suggest that these asteroids originated in the terrestrial planet’s region, i.e., within 1.5 au, and later got implanted into the main asteroid belt (MAB).
Rogerio Deienno, André Izidoro, David Nesvorný, William F. Bottke, Fernando Roig, Simone Marchi   +5 more
doaj   +1 more source

Pebble formation by ice condensation

EPJ Web of Conferences, 2013
Pebbles with sizes of centimeters to decimeters are needed in order to form kilometer-sized planetesimals, which in turn are needed for planet formation to proceed. The well-studied mechanism of coagulation is efficient only up to millimeter-sized dust
Ros Katrin
doaj   +1 more source

Are Pebble Pile Planetesimals Doomed? [PDF]

Monthly Notices of the Royal Astronomical Society, 2019
In parabolic flight experiments we studied the wind induced erosion of granular beds composed of spherical glass beads at low gravity and low ambient pressure. Varying g-levels were set by centrifugal forces. Expanding existing parameter sets to a pressure range between $p=300-1200\,$Pa and to g-levels of $g=1.1-2.2\,\rm m\,s^{-2}$ erosion thresholds ...
Tunahan Demirci, Maximilian Kruss, Jens Teiser, Tabea Bogdan, Felix Jungmann, Niclas Schneider, Gerhard Wurm   +6 more
openaire   +3 more sources

The effects of pressure on immiscibility in metallic, core‐forming liquids: Implications for protoplanetary differentiation

Meteoritics &Planetary Science, Volume 61, Issue 4, Page 720-738, April 2026.
Abstract Mechanisms for metal core formation in rocky planetesimals and planetary embryos remain poorly constrained, in part due to complexities arising from immiscibility in core‐forming liquids at low pressures. To assess the pressure dependence of immiscibility and its role in protoplanetary differentiation, we performed experiments at 3 and 5 GPa ...
Geoffrey David Bromiley, Hidenori Terasaki, Matthew Varnam   +2 more
wiley   +1 more source