Results 21 to 30 of about 11,561 (252)
Effect of turbulence on collisions of dust particles with planetesimals in protoplanetary disks [PDF]
, 2016 Planetesimals in gaseous protoplanetary disks may grow by collecting dust particles. Hydrodynamical studies show that small particles generally avoid collisions with the planetesimals because they are entrained by the flow around them.
Bec, J. +5 more
core +3 more sources
Collisional Processes in Extrasolar Planetsimal Disks - Dust Clumps in Fomalhaut's Debris Disk [PDF]
, 2002 This paper presents a model for the outcome of collisions between planetesimals in a debris disk and assesses the impact of collisional processes on the structure and size distribution of the disk. The model is presented by its application to Fomalhaut's
Dent, W. R. F., Wyatt, M. C.
core +3 more sources
Planet formation in slightly inclined binary systems
EPJ Web of Conferences, 2011 One of the major problems of planet formation in close binary systems, such as α Centauri AB, is the formation of planetary embryos or cores by mutual accretion of km-sized planetesimals.
Ge J., Xie J.-W., Zhou J.-L.
doaj +1 more source
, 2023 During the formation of our solar system, a large number of planetesimals were ejected into interstellar space by gravitational encounters with the planets. Debris disks observations and numerical simulations indicate that many other planetary systems, now known to be quite common, would have undergone a similar dynamical clearing process.
openaire +2 more sources
Circumbinary Planet Formation in the Kepler-16 System. II. A Toy Model for In-situ Planet Formation within a Debris Belt [PDF]
, 2014 Recent simulations have shown that the formation of planets in circumbinary configurations (such as those recently discovered by Kepler) is dramatically hindered at the planetesimal accretion stage.
Meschiari, Stefano
core +2 more sources
Planetesimal Accretion at Short Orbital Periods
The Astrophysical Journal, 2023 Formation models in which terrestrial bodies grow via the pairwise accretion of planetesimals have been reasonably successful at reproducing the general properties of the Solar System, including small-body populations. However, planetesimal accretion has
Spencer C. Wallace, Thomas R. Quinn
doaj +1 more source
Stochasticity & Predictability in Terrestrial Planet Formation [PDF]
, 2016 Terrestrial planets are thought to be the result of a vast number of gravitational interactions and collisions between smaller bodies. We use numerical simulations to show that practically identical initial conditions result in a wide array of final ...
Grimm, Simon L. +3 more
core +2 more sources
Gravoturbulent Formation of Planetesimals [PDF]
The Astrophysical Journal, 2006 We explore the effect of magnetorotational turbulence on the dynamics and concentrations of boulders in local box simulations of a sub-Keplerian protoplanetary disc. The solids are treated as particles each with an independent space coordinate and velocity. We find that the turbulence has two effects on the solids.
Johansen, Anders +2 more
openaire +2 more sources
The Formation of Uranus and Neptune in Solid-Rich Feeding Zones: Connecting Chemistry and Dynamics [PDF]
, 2009 The core accretion theory of planet formation has at least two fundamental problems explaining the origins of Uranus and Neptune: (1) dynamical times in the trans-Saturnian solar nebula are so long that core growth can take > 15 Myr, and (2) the onset of
Alexander +41 more
core +1 more source
PLANETESIMAL COMPOSITIONS IN EXOPLANET SYSTEMS [PDF]
The Astrophysical Journal, 2012 We have used recent surveys of the composition of exoplanet host stars to investigate the expected composition of condensed material in planetesimals formed beyond the snow line in the circumstellar nebulae of these systems. Of the major solid forming elements, we find that, as for the Sun, the C and O abundances (and particularly the C/O abundance ...
Johnson, T.V. +3 more
openaire +3 more sources