Results 31 to 40 of about 2,834 (210)

MERGING CRITERIA FOR GIANT IMPACTS OF PROTOPLANETS [PDF]

The Astrophysical Journal, 2011
Accepted to ...
Hidenori Genda, Kokubo, E., Ida, S.
openaire   +2 more sources

Formation of Protoplanet Systems [PDF]

Symposium - International Astronomical Union, 2004
We present the latest results of large scale (N = 10000, 0.5AU < a < 1.5AU) N-body simulations of planetary accretion. We confirm the oligarchic growth of protoplanets in the minimum-mass disk and a more massive disk models. Protoplanets with the predicted isolation mass are formed with orbital separation of about 10-15 Hill radius.
Eiichiro Kokubo, Shigeru Ida
openaire   +1 more source

Oscillatory migration of accreting protoplanets driven by a 3D distortion of the gas flow

, 2019
Context. The dynamics of a low-mass protoplanet accreting solids is influenced by the heating torque, which was found to suppress inward migration in protoplanetary disks with constant opacities. Aims.
Chrenko, Ondřej, Lambrechts, Michiel
core   +1 more source

Critical Core Masses for Gas Giant Formation with Grain-Free Envelopes [PDF]

, 2010
We investigate the critical core mass and the envelope growth timescale, assuming grain-free envelopes, to examine how small cores are allowed to form gas giants in the framework of the core accretion model.
Aikawa, Allende Prieto, Allende Prieto, Borysow, Boss, Burrows, Duncan, Fortney, Freedman, Haisch, Hasegawa, Ikoma, Ikoma, Lodders, Masahiro Ikoma, Militzer, Nettelmann, Sasaki, Saumon, Woods, Yasunori Hori   +20 more
core   +1 more source

ECCENTRICITY EVOLUTION THROUGH ACCRETION OF PROTOPLANETS [PDF]

The Astrophysical Journal, 2015
Most of super-Earths detected by the radial velocity (RV) method have significantly smaller eccentricities than the eccentricities corresponding to velocity dispersion equal to their surface escape velocity ("escape eccentricities"). If orbital instability followed by giant impacts among protoplanets that have migrated from outer region is considered ...
Yuji Matsumoto, Makiko Nagasawa, Shigeru Ida   +2 more
openaire   +2 more sources

Disk Evolution Study Through Imaging of Nearby Young Stars (DESTINYS): Dynamical Evidence of a Spiral-Arm-Driving and Gap-Opening Protoplanet from SAO 206462 Spiral Motion

Universe
In the early stages of planetary system formation, young exoplanets gravitationally interact with their surrounding environments and leave observable signatures on protoplanetary disks.
Chen Xie, Chengyan Xie, Bin B. Ren, Myriam Benisty, Christian Ginski, Taotao Fang, Simon Casassus, Jaehan Bae, Stefano Facchini, François Ménard, Rob G. van Holstein   +10 more
doaj   +1 more source

The effects of viscosity on the circumplanetary disks

, 2012
The effects of viscosity on the circumplanetary disks residing in the vicinity of protoplanets are investigated through two-dimensional hydrodynamical simulations with the shearing sheet model.
Bai, Bryden, Canup, D'Angelo, De-Fu Bu, Feng Yuan, Goldreich, Hayashi, Hsien Shang, Ikoma, Ikoma, Kley, Lubow, Machida, Machida, Muto, Quillen, Schubert, Stevenson, Tanigawa, Tanigawa   +20 more
core   +1 more source

Composition of Massive Giant Planets [PDF]

, 2010
The two current models for giant planet formation are core accretion and disk instability. We discuss the core masses and overall planetary enrichment in heavy elements predicted by the two formation models, and show that both models could lead to a ...
Durisen, Jack J. Lissauer, Lissauer, Peter Bodenheimer, Ravit Helled, Safronov   +5 more
core   +1 more source

Distribution of thermodynamic variables inside extra-solar protoplanets formed via disk instability

Egyptian Journal of Remote Sensing and Space Sciences, 2013
In this paper, distribution of thermodynamic variables inside extra-solar protoplanets in their initial stages, formed by gravitational instability, is presented.
G.C. Paul, S.K. Bhattacharjee
doaj   +1 more source

Orbital Migration of Protoplanets in a Marginally Gravitationally Unstable Disk

, 2013
Core accretion and disk instability require giant protoplanets to form in the presence of disk gas. Protoplanet migration models generally assume disk masses low enough that the disk's self-gravity can be neglected.
Boss, Alan P.
core   +1 more source