Theoretical models of planetary system formation: mass vs semi-major axis [PDF]
, 2013 Planet formation models have been developed during the last years in order to try to reproduce the observations of both the solar system, and the extrasolar planets. Some of these models have partially succeeded, focussing however on massive planets, and
Alibert, Y. +6 more
core +5 more sources
Rapid Dust Growth during Hydrodynamic Clumping due to Streaming Instability
The Astrophysical Journal, 2023 Streaming instability is considered to be one of the dominant processes in promoting planetesimal formation by the gravitational collapse of dust clumps.
Ryosuke T. Tominaga, Hidekazu Tanaka
doaj +1 more source
Wind-shearing in gaseous protoplanetary disks and the evolution of binary planetesimals
, 2011 One of the first stages of planet formation is the growth of small planetesimals. This early stage occurs much before the dispersal of most of the gas from the protoplanetary disk. Due to their different aerodynamic properties, planetesimals of different
Andrews +15 more
core +1 more source
Debris discs around M stars: non-existence versus non-detection [PDF]
, 2013 Motivated by the reported dearth of debris discs around M stars, we use survival models to study the occurrence of planetesimal discs around them. These survival models describe a planetesimal disc with a small number of parameters, determine if it may ...
Heng, Kevin, Malik, Matej
core +2 more sources
Predictions for the secondary CO, C and O gas content of debris discs from the destruction of volatile-rich planetesimals [PDF]
, 2017 QK, LM and MCW acknowledge support from the European Union through ERC grant number 279973. QK and MCW acknowledge funding from STFC via the Institute of Astronomy, Cambridge Consolidated Grant.
Q. Kral, L. Matrá, M. Wyatt, G. Kennedy
semanticscholar +1 more source
A Lagrangian model for dust evolution in protoplanetary disks: formation of wet and dry planetesimals at different stellar masses [PDF]
Astronomy & Astrophysics, 2018 We introduce a new Lagrangian smooth-particle method to model the growth and drift of pebbles in protoplanetary disks. The Lagrangian nature of the model makes it especially suited to following characteristics of individual (groups of) particles, such as
D. Schoonenberg, C. Ormel, S. Krijt
semanticscholar +1 more source
Numerical simulations for terrestrial planets formation
EPJ Web of Conferences, 2011 We investigate the formation of terrestrial planets in the late stage of planetary formation using two-planet model. At that time, the protostar has formed for about 3 Myr and the gas disk has dissipated.
Ji J., Zhang N.
doaj +1 more source
Feasibility of transit photometry of nearby debris discs [PDF]
, 2014 Dust in debris discs is constantly replenished by collisions between larger objects. In this paper, we investigate a method to detect these collisions.
Kalas, P. +2 more
core +3 more sources
Formation of Asteroid (16) Psyche by a Giant Impact
Journal of Geophysical Research: Planets, Volume 131, Issue 1, January 2026.Abstract Asteroid (16) Psyche is the largest likely metal‐rich asteroid in the Solar System and the target of the NASA Psyche mission. The mission aims to determine whether the asteroid is the core of a differentiated planetesimal that lost its mantle via a giant impact.
Saverio Cambioni +14 more
wiley +1 more source
Fast accretion of small planetesimals by protoplanetary cores
, 2003 We explore the dynamics of small planetesimals coexisting with massive protoplanetary cores in a gaseous nebula. Gas drag strongly affects the motion of small bodies leading to the decay of their eccentricities and inclinations, which are excited by the ...
Greenberg J. M. +4 more
core +2 more sources