Mass Distribution and Planet Formation in the Solar Nebula

  title={Mass Distribution and Planet Formation in the Solar Nebula},
  author={Steven J. Desch},
  journal={The Astrophysical Journal},
  • S. Desch
  • Published 2007
  • Physics
  • 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… Expand
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 inExpand
Ice lines, planetesimal composition and solid surface density in the solar nebula
Abstract To date, there is no core accretion simulation that can successfully account for the formation of Uranus or Neptune within the observed 2–3 Myr lifetimes of protoplanetary disks. Since solidExpand
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 stellarExpand
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 distributionExpand
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 ofExpand
Growth model interpretation of planet size distribution.
The radii and orbital periods of 4,000+ confirmed/candidate exoplanets have been precisely measured by the Kepler mission. The radii show a bimodal distribution, with two peaks corresponding toExpand
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 &Expand
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 initialExpand
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 formationExpand
The outcome of protoplanetary dust growth: pebbles, boulders or planetesimals?
Context. The evolution of dust particles in protoplanetary disks determines many observable and structural properties of the disk, such as the spectral energy distribution (SED), appearance of disks,Expand


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 migrationExpand
Possible Rapid Gas Giant Planet Formation in the Solar Nebula and Other Protoplanetary Disks.
  • Boss
  • Physics, Medicine
  • 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. Expand
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 hydrostaticExpand
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 accretedExpand
Planetary migration in a planetesimal disk: why did Neptune stop at 30 AU?
Abstract We study planetary migration in a gas-free disk of planetesimals. In the case of our Solar System we show that Neptune could have had either a damped migration, limited to a few AUs, or aExpand
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 strengthExpand
Calculations of the accretion and evolution of giant planets: The effects of solid cores
The evolution of the giant planets is calculated under the general hypothesis that the solid cores formed first, by accretion of small particles, and that these cores later gravitationally attractedExpand
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.Expand
Evolution of protoplanetary disks: Constraints from DM Tauri and GM Aurigae
We present a one-dimensional model of the formation and viscous evolution of protoplanetary disks. The formation of the early disk is modeled as the result of the gravitational collapse of anExpand
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 dustExpand