Giant planet effects on terrestrial planet formation and system architecture
نویسندگان
چکیده
منابع مشابه
Terrestrial Planet Formation
The standard planetesimal model of terrestrial-planet formation is based on astronomical and cosmochemical observations, and the results of laboratory experiments and numerical simulations. In this model, planets grow in a series of stages beginning with the μm-sized dust grains observed in protoplanetary disks. Dust grains readily stick together to form mm-to-cm-sized aggregates, some of which...
متن کاملTerrestrial planet formation.
Advances in our understanding of terrestrial planet formation have come from a multidisciplinary approach. Studies of the ages and compositions of primitive meteorites with compositions similar to the Sun have helped to constrain the nature of the building blocks of planets. This information helps to guide numerical models for the three stages of planet formation from dust to planetesimals (~10...
متن کاملEarth and Terrestrial Planet Formation
The growth and composition of Earth is a direct consequence of planet formation throughout the Solar System. We discuss the known history of the Solar System, the proposed stages of growth and how the early stages of planet formation may be dominated by pebble growth processes. Pebbles are small bodies whose strong interactions with the nebula gas lead to remarkable new accretion mechanisms for...
متن کاملA reduced efficiency of terrestrial planet formation following giant planet migration
Substantial orbital migration of massive planets may occur in most extrasolar planetary systems. Since migration is likely to occur after a significant fraction of the dust has been locked up into planetesimals, ubiquitous migration could reduce the probability of forming terrestrial planets at radii of the order of 1 au. Using a simple time dependent model for the evolution of gas and solids i...
متن کاملMigration and giant planet formation
X iv :a st ro -p h/ 04 03 57 4v 1 2 4 M ar 2 00 4 We extend the core-accretion model of giant gaseous planets by Pollack et al. ([1996]) to include migration, disc evolution and gap formation. Starting with a core of a fraction of an Earth’s mass located at 8 AU, we end our simulation with the onset of runaway gas accretion when the planet is at 5.5 AU 1 Myr later. This timescale is about a fac...
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ژورنال
عنوان ژورنال: Monthly Notices of the Royal Astronomical Society
سال: 2019
ISSN: 0035-8711,1365-2966
DOI: 10.1093/mnras/stz385