Results 41 to 50 of about 2,834 (210)

On the migration of a system of protoplanets [PDF]

Monthly Notices of the Royal Astronomical Society, 2000
5 Pages, 4 eps-figures, uses MN-Latex style ...
openaire   +2 more sources

Occurrence Rates of Accreting Companions from a New Method for Computing Emission-line Survey Sensitivity: Application to the Hα Giant Accreting Protoplanet Survey

The Astronomical Journal
A key scientific goal of exoplanet surveys is to characterize the underlying population of planets in the local galaxy. In particular, the properties of accreting proto planets can inform the rates and physical processes of planet formation. We develop a
Cailin Plunkett, Katherine B. Follette, Gabriel-Dominique Marleau, Eric L. Nielsen   +3 more
doaj   +1 more source

Tidal Barrier and the Asymptotic Mass of Proto Gas-Giant Planets

, 2007
Extrasolar planets found with radial velocity surveys have masses ranging from several Earth to several Jupiter masses. While mass accretion onto protoplanetary cores in weak-line T-Tauri disks may eventually be quenched by a global depletion of gas ...
D. N. C. Lin, Goldreich P., Ian Dobbs‐Dixon, Kley W., Kley W., Lin D. N. C., Shu Lin Li, Ward W. R.   +7 more
core   +2 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, Benjamin P. Weiss, Namya Baijal, Robert Melikyan, Erik Asphaug, John B. Biersteker, Richard P. Binzel, William F. Bottke, Samuel W. Courville, Linda T. Elkins‐Tanton, David J. Lawrence, José M. G. Merayo, Carol A. Raymond, Mark A. Wieczorek, Maria T. Zuber   +14 more
wiley   +1 more source

Spin of protoplanets generated by pebble accretion: Influences of protoplanet-induced gas flow

Astronomy & Astrophysics, 2023
Context. In the pebble accretion model, protoplanets accrete millimeter-to-centimeter-sized particles (pebbles). When a protoplanet grows, a dense gas envelope forms around it. The envelope affects accretion of pebbles and, in particular, the spin angular momentum transfer at the collision to the planet. Aims.
Takaoka, Kohsuke, Kuwahara, Ayumu, Ida, Shigeru, Kurokawa, Hiroyuki   +3 more
openaire   +2 more sources

Evolution of Terrestrial Planetary Bodies and Implications for Habitability

Reviews of Geophysics, Volume 63, Issue 4, December 2025.
Abstract The terrestrial planetary bodies of our solar system—Mercury, Venus, Earth, and Mars—share a common origin through nebular accretion and early magma ocean differentiation, yet they diverged significantly in geological evolution, tectonic regimes, and habitability.
Peter A. Cawood, Eva E. Stüeken, Priyadarshi Chowdhury, Chris J. Hawkesworth, Jacob A. Mulder   +4 more
wiley   +1 more source

Improved Orbital Constraints and Hα Photometric Monitoring of the Directly Imaged Protoplanet Analog HD 142527 B

The Astronomical Journal, 2022
Companions embedded in the cavities of transitional circumstellar disks have been observed to exhibit excess luminosity at H α , an indication that they are actively accreting.
William O. Balmer, Katherine B. Follette, Laird M. Close, Jared R. Males, Robert J. De Rosa, Jéa I. Adams Redai, Alex Watson, Alycia J. Weinberger, Katie M. Morzinski, Julio Morales, Kimberly Ward-Duong, Laurent Pueyo   +11 more
doaj   +1 more source

Disk Planet Interactions and Early Evolution in Young Planetary Systems

, 2004
We study and review disk protoplanet interactions using local shearing box simulations. These suffer the disadvantage of having potential artefacts arising from periodic boundary conditions but the advantage, when compared to global simulations, of being
A. P. Boss, A. Steinacker, C. Terquem, D. G. Korycansky, D. N. C. Lin, D. N. C. Lin, F. S. Masset, F. S. Masset, G. Bryden, G. D’Angelo, H. Tanaka, J. B. Pollack, J. C. B. Papaloizou, J. C. B. Papaloizou, J. C. B. Papaloizou, J. C. B. Papaloizou, J. F. Hawley, J. F. Hawley, M. Mayor, N. I. Shakura, N. R. Lebovitz, P. Artymowicz, P. Goldreich, P. Goldreich, R. P. Nelson, R. P. Nelson, R.P. Nelson, S. A. Balbus, S. H. Lubow, S. S. Vogt, S. Zucker, U. Ziegler, W. Kley, W. Ward, W. Winters, W. Winters   +35 more
core   +1 more source

The migration of gas giant planets in gravitationally unstable disks [PDF]

, 2015
Planets form in the disks of gas and dust that surround young stars. It is not known whether or not gas giant planets on wide orbits form the same way as Jupiter or form by the fragmentation of gravitationally unstable disks.
Stamatellos, Dimitris
core   +2 more sources

The effect of pressure on dihedral angle between liquid Fe‐S and orthopyroxene: Implication for percolative core formation in planetesimals and planetary embryos

Meteoritics &Planetary Science, Volume 60, Issue 12, Page 2811-2827, December 2025.
Abstract During precursor stages of planet formation, many planetesimals and planetary embryos are considered to have differentiated, forming an iron‐alloy core and silicate mantle. Percolation of liquid iron‐alloy in solid silicates is one of the major possible differentiation processes in these small bodies.
Takumi Miura, Hidenori Terasaki, Hyu Takaki, Kotaro Kobayashi, Geoffrey David Bromiley, Takashi Yoshino   +5 more
wiley   +1 more source