A low mass for Mars from Jupiter’s early gas-driven migration

@article{Walsh2011ALM,
  title={A low mass for Mars from Jupiter’s early gas-driven migration},
  author={Kevin J. Walsh and Alessandro Morbidelli and Sean N. Raymond and David P. O'Brien and Avi M. Mandell},
  journal={Nature},
  year={2011},
  volume={475},
  pages={206-209}
}
Jupiter and Saturn formed in a few million years (ref. 1) from a gas-dominated protoplanetary disk, and were susceptible to gas-driven migration of their orbits on timescales of only ∼100,000 years (ref. 2). Hydrodynamic simulations show that these giant planets can undergo a two-stage, inward-then-outward, migration. The terrestrial planets finished accreting much later, and their characteristics, including Mars' small mass, are best reproduced by starting from a planetesimal disk with an… 

Shaping of the Inner Solar System by the Gas-Driven Migration of Jupiter

Abstract A persistent difficulty in terrestrial planet formation models is creating Mars analogs with the appropriate mass: Mars is typically an order of magnitude too large in simulations. Some

The asteroid belt and Mars' small mass explained by large-scale gas-driven migration of Jupiter

Dynamical simulations of terrestrial planet accretion consistently fail to produce reasonable Mars analogs; planets at Mars' orbital distance are systematically too massive [1]. A recent model,

TERRESTRIAL PLANET FORMATION IN A PROTOPLANETARY DISK WITH A LOCAL MASS DEPLETION: A SUCCESSFUL SCENARIO FOR THE FORMATION OF MARS

Models of terrestrial planet formation for our solar system have been successful in producing planets with masses and orbits similar to those of Venus and Earth. However, these models have generally

Formation of telluric planets and the origin of terrestrial water

Simulations of planet formation have failed to reproduce Mars' small mass (compared with Earth) for 20 years. Here I will present a solution to the Mars problem that invokes large-scale migration of

Conditions for water ice lines and Mars-mass exomoons around accreting super-Jovian planets at 1−20 AU from Sun-like stars

Context. The first detection of a moon around an extrasolar planet (an “exomoon”) might be feasible with NASA’s Kepler or ESA’s upcoming PLATO space telescopes or with the future ground-based

Jupiter's Influence on the Building Blocks of Mars and Earth

Radiometric dating indicates that Mars accreted in the first ~4 Myr of the solar system, coinciding with the formation and possible migration of Jupiter. While nebular gas from the protoplanetary

Terrestrial planet formation constrained by Mars and the structure of the asteroid belt

Reproducing the large Earth/Mars mass ratio requires a strong mass depletion in solids within the protoplanetary disc between 1 and 3 au. The Grand Tack model invokes a specific migration history of

The Hot Jupiter Period–Mass Distribution as a Signature of in situ Formation

More than two decades after the widespread detection of Jovian-class planets on short-period orbits around other stars, their dynamical origins remain imperfectly understood. In the traditional
...

References

SHOWING 1-10 OF 79 REFERENCES

EVIDENCE FROM THE ASTEROID BELT FOR A VIOLENT PAST EVOLUTION OF JUPITER's ORBIT

We use the current orbital structure of large (>50 km) asteroids in the main asteroid belt to constrain the evolution of the giant planets when they migrated from their primordial orbits to their

ORBITAL MIGRATION OF LOW-MASS PLANETS IN EVOLUTIONARY RADIATIVE MODELS: AVOIDING CATASTROPHIC INFALL

Outward migration of low-mass planets has recently been shown to be a possibility in non-barotropic disks. We examine the consequences of this result in evolutionary models of protoplanetary disks.

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

ON THE ORBITAL EVOLUTION OF A GIANT PLANET PAIR EMBEDDED IN A GASEOUS DISK. I. JUPITER–SATURN CONFIGURATION

We carry out a series of high-resolution (1024 × 1024) hydrodynamical simulations to investigate the orbital evolution of Jupiter and Saturn embedded in a gaseous protostellar disk. Our work extends

LONG RANGE OUTWARD MIGRATION OF GIANT PLANETS, WITH APPLICATION TO FOMALHAUT b

Recent observations of exoplanets by direct imaging reveal that giant planets orbit at a few dozens to more than a hundred AU from their central star. The question of the origin of these planets

The effect of an early planetesimal-driven migration of the giant planets on terrestrial planet formation

The migration of the giant planets due to the scattering of planetesimals causes powerful resonances to move through the asteroid belt and the terrestrial planet region. Exactly when and how the

Massive Planet Migration: Theoretical Predictions and Comparison with Observations

We quantify the utility of large radial velocity surveys for constraining theoretical models of type II migration and protoplanetary disk physics. We describe a theoretical model for the expected
...