Growth of Jupiter: Formation in disks of gas and solids and evolution to the present epoch

  title={Growth of Jupiter: Formation in disks of gas and solids and evolution to the present epoch},
  author={Gennaro D’Angelo and S. J. Weidenschilling and Jack J. Lissauer and Peter H. Bodenheimer},
7 Citations
Dust Resurgence in Protoplanetary Disks Due to Planetesimal–Planet Interactions
Observational data on the dust content of circumstellar disks show that the median dust content in disks around pre-main-sequence stars in nearby star-forming regions seems to increase from ∼1 to ∼2
Mixing of Condensable Constituents with H–He during the Formation and Evolution of Jupiter
Simulations of Jupiter's formation are presented that incorporate mixing of H–He with denser material entering the planet as solids. Heavy compounds and gas mix substantially when the planet becomes
Thermal Processing of Solids Encountering a Young Jovian Core
Jupiter’s enhancement in nitrogen relative to hydrogen when compared to the Sun has been interpreted as evidence that its early formation occurred beyond the N2 snow line (∼20–40 au). However, the
From Pebbles and Planetesimals to Planets and Dust: The Protoplanetary Disk–Debris Disk Connection
The similar orbital distances and detection rates of debris disks and the prominent rings observed in protoplanetary disks suggest a potential connection between these structures. We explore this
Rapid contraction of giant planets orbiting the 20-million-year-old star V1298 Tau
Current theories of planetary evolution predict that infant giant planets have large radii and very low densities before they slowly contract to reach their final size after about several hundred
Oort cloud Ecology
Jan Hendrik Oort hypothesized the existence of a distant cloud of cometary objects that orbit the Sun based on a spike in the reciprocal orbital separation at 1∕a  ≲  10−4 au−1. The Oort cloud is the
Tracing the Formation History of Giant Planets in Protoplanetary Disks with Carbon, Oxygen, Nitrogen, and Sulfur
The composition of giant planets is imprinted by their migration history and the compositional structure of their hosting disks. Studies in recent literature have investigated how the abundances of C


New Formation Models for the Kepler-36 System
Formation of the planets in the Kepler-36 system is modeled by detailed numerical simulations according to the core-nucleated accretion scenario. The standard model is updated to include the
The formation of Jupiter by hybrid pebble–planetesimal accretion
The standard model for giant planet formation is based on the accretion of solids by a growing planetary embryo, followed by rapid gas accretion once the planet exceeds a so-called critical mass1.
Accretion in the ρ-Ophiuchi pre-main sequence stars
Aims. The aim of this paper is to provide a measurement of the mass accretion rate in a large, complete sample of objects in the core of the star forming region p Oph. Methods. The sample includes
Models of the in Situ Formation of Detected Extrasolar Giant Planets
Abstract We present numerical simulations of the formation of the planetary companions to 47 UMa, ρ CrB, and 51 Peg. They are assumed to have formed in situ according to the basic model that a core
The Absolute Chronology and Thermal Processing of Solids in the Solar Protoplanetary Disk
U-corrected Pb-Pb dating from primitive meteorites indicates that chondrule formation started contemporaneously with CAIs and lasted ~3 million years, suggesting that the formation ofCAIs and chondrules reflects a process intrinsically linked to the secular evolution of accretionary disks.
We study the evolution of planetesimals in evolved gaseous disks that orbit a solar-mass star and harbor a Jupiter-mass planet at a p ≈ 5 ?> AU. The gas dynamics are modeled with a three-dimensional
Stellar Structure and Evolution. Stellar Structure and Evolution: Astronomy and Astrophysics Library, ISBN 978-3-642-30255-8
  • 2013