Results 31 to 40 of about 21,167 (278)
Astronomy & Astrophysics, 2023 Planetesimals are born fragile and are subject to destruction by wind erosion as they move through the gas of a protoplanetary disk. In microgravity experiments, we determined the shear stress necessary for erosion of a surface consisting of 1 mm dust pebbles down to 1 Pa ambient pressure. This is directly applicable to protoplanetary disks.
L. Schönau +7 more
openaire +3 more sources
The Astrophysical Journal, 2023 Thanks to “dust-to-planet” simulations (DTPSs), which treat the collisional evolution directly from dust to giant-planet cores in a protoplanetary disk, we showed that giant-planet cores are formed in ≲10 au in several 10 ^5 yr, because porous pebbles ...
Hiroshi Kobayashi, Hidekazu Tanaka
doaj +1 more source
PLANETESIMAL DISK MICROLENSING [PDF]
The Astrophysical Journal, 2009 Motivated by debris disk studies, we investigate the gravitational microlensing of background starlight by a planetesimal disk around a foreground star. We use dynamical survival models to construct a plausible example of a planetesimal disk and study its microlensing properties using established ideas of microlensing by small bodies. When a solar-type
Heng, Kevin, Keeton, Charles R.
openaire +2 more sources
Solution to the debris disc mass problem: planetesimals are born small? [PDF]
, 2020 Debris belts on the periphery of planetary systems, encompassing the region occupied by planetary orbits, are massive analogues of the Solar system's Kuiper belt.
A. Krivov, M. Wyatt
semanticscholar +1 more source
Meteorite evidence for partial differentiation and protracted accretion of planetesimals
Science Advances, 2020 A broad spectrum of fully differentiated, partially melted, and possibly unmelted objects populated the early solar system. Modern meteorite classification schemes assume that no single planetary body could be source of both unmelted (chondritic) and ...
C. Maurel +8 more
semanticscholar +1 more source
The Mass and Size Distribution of Planetesimals Formed by the Streaming Instability. II. The Effect of the Radial Gas Pressure Gradient [PDF]
Astrophysical Journal, 2018 The streaming instability concentrates solid particles in protoplanetary disks, leading to gravitational collapse into planetesimals. Despite its key role in producing particle clumping and determining critical length scales in the instability’s linear ...
Charles P. Abod +5 more
semanticscholar +1 more source
, 1998 A planet orbiting in a disk of planetesimals can experience an instability in which it migrates to smaller orbital radii. Resonant interactions between the planet and planetesimals remove angular momentum from the planetesimals, increasing their ...
Hansen, Brad +3 more
core +3 more sources
Binary Formation in Planetesimal Disks. I. Equal Mass Planetesimals [PDF]
Publications of the Astronomical Society of Japan, 2011 As of April 2010, 48 TNO (trans-Neptunian Object) binaries have been found. This is about 6% of known TNOs. However, in previous theoretical studies of planetary formation in the TNO region, the effect of binary formation has been neglected. TNO binaries can be formed through a variety of mechanisms, such as a three-body process, dynamical friction on ...
Daisaka, Junko K. +2 more
openaire +2 more sources
Pebbles versus planetesimals: the case of Trappist-1 [PDF]
Astronomy & Astrophysics, 2019 We present a study into the formation of planetary systems around low mass stars similar to Trappist-1, through the accretion of either planetesimals or pebbles. The aim is to determine if the currently observed systems around low mass stars could favour
G. Coleman +3 more
semanticscholar +1 more source
Planetesimal collisions in binary systems [PDF]
, 2010 We study the collisional evolution of km-sized planetesimals in tight binary star systems to investigate whether accretion towards protoplanets can proceed despite the strong gravitational perturbations from the secondary star.
Desidera +18 more
core +1 more source