Mass Distribution and Planet Formation in the Solar Nebula

@article{Desch2007MassDA,
  title={Mass Distribution and Planet Formation in the Solar Nebula},
  author={Steven J. Desch},
  journal={The Astrophysical Journal},
  year={2007},
  volume={671},
  pages={878 - 893}
}
  • S. Desch
  • Published 10 December 2007
  • Physics, Geology
  • The Astrophysical Journal
The surface density profile Σ(r) of the solar nebula protoplanetary disk is a fundamental input to all models of disk processes and evolution. Traditionally it is estimated by spreading out the augmented masses of the planets over the annuli in which the planets orbit today, the so-called minimum-mass solar nebula. Doing so implicitly assumes that the planets completely accreted all planetesimals in their feeding zones, but this assumption has not been tested. Indeed, models of the growth of… 

MINIMUM MASS SOLAR NEBULAE AND PLANETARY MIGRATION

The Minimum Mass Solar Nebula (MMSN) is a protoplanetary disk that contains the minimum amount of solids necessary to build the planets of the solar system. Assuming that the giant planets formed in

EVOLUTION OF THE SOLAR NEBULA AND PLANET GROWTH UNDER THE INFLUENCE OF PHOTOEVAPORATION

The recent development of a new minimum mass solar nebula, under the assumption that the giant planets formed in the compact configuration of the Nice model, has shed new light on planet formation in

A minimum mass nebula for M dwarfs

Recently revealed differences in planets around M dwarf vs. solar-type stars could arise from differences in their primordial disks, and surveys of T Tauri stars find a correlation between stellar

Mass inventory of the giant-planet formation zone in a solar nebula analogue

The initial mass distribution in the solar nebula is a critical input to planet formation models that seek to reproduce today’s Solar System. Traditionally, constraints on the gas mass distribution

Migration of Massive Planets

This thesis studies themigration of massive planets with massMP ≳ . MJupiter. Planetary migration is a process that changes the semi-major axis of the planetary orbit. The gravitational forces of

No universal minimum-mass extrasolar nebula: evidence against in situ accretion of systems of hot super-Earths

It has been proposed that the observed systems of hot super-Earths formed in situ from high-mass disks. By fitting a disk profile to the entire population of Kepler planet candidates, Chiang &

Simultaneous formation of solar system giant planets

Context. In the last few years, the so-called “Nice model” has become increasingly significant for studying the formation and evolution of the solar system. According to this model, the initial

The Dynamic Proto-atmospheres around Low-mass Planets with Eccentric Orbits

Protoplanets are able to accrete primordial atmospheres when embedded in the gaseous protoplanetary disk. The formation and structure of the proto-atmosphere are subject to the planet–disk

Have protoplanetary discs formed planets

It has recently been noted that many discs around T Tauri stars appear to comprise only a few Jupiter masses of gas and dust. Using millimetre surveys of discs within six local star formation
...

References

SHOWING 1-10 OF 59 REFERENCES

Terrestrial Planet Formation in Disks with Varying Surface Density Profiles

The minimum-mass solar nebula (MMSN) model estimates the surface density distribution of the protoplanetary disk by assuming the planets to have formed in situ. However, significant radial migration

Possible Rapid Gas Giant Planet Formation in the Solar Nebula and Other Protoplanetary Disks

  • A. Boss
  • Physics, Geology
    The Astrophysical journal
  • 2000
New three-dimensional, "locally isothermal," hydrodynamical models without velocity damping show that a disk instability can form Jupiter-mass clumps, implying that disk instability could obviate the core accretion mechanism in the solar nebula and elsewhere.

Formation of the Giant Planets

The structure of a gaseous envelope surrounding a protoplanet has been investigated in connection with the formation of the giant planets. Under the assumptions of spherical symmetry and hydrostatic

Formation of the Giant Planets by Concurrent Accretion of Solids and Gas

New numerical simulations of the formation of the giant of the second phase. planets are presented, in which for the first time both the gas and The actual rates at which the giant planets accreted

Formation of Protoplanet Systems and Diversity of Planetary Systems

We investigate the formation of protoplanet systems from planetesimal disks by global (N = 5000 and 10,000 and 0.5 AU < a < 1.5 AU, where N is the number of bodies and a is the distance from a

The Origin of Comets in the Solar Nebula: A Unified Model

Abstract Comets originated as icy planetesimals in the outer Solar System, as shown by dynamical studies and direct observation of objects in the Kuiper disk. Their nuclei have low strength

Planet Formation with Migration

In the core-accretion model, gas-giant planets form solid cores that then accrete gaseous envelopes. Tidal interactions with disk gas cause a core to undergo inward type I migration in 104-105 yr.

Radial Flow of Dust Particles in Accretion Disks

We study the radial migration of dust particles in accreting protostellar disks analogous to the primordial solar nebula. Our main objective is to determine the retention efficiency of dust
...