Occurrence of Earth-Like Bodies in Planetary Systems

  title={Occurrence of Earth-Like Bodies in Planetary Systems},
  author={George W. Wetherill},
  pages={535 - 538}
Present theories of terrestrial planet formation predict the rapid ``runaway formation'' of planetary embryos. The sizes of the embryos increase with heliocentric distance. These embryos then merge to form planets. In earlier Monte Carlo simulations of the merger of these embryos it was assumed that embryos did not form in the asteroid belt, but this assumption may not be valid. Simulations in which runaways were allowed to form in the asteroid belt show that, although the initial distributions… 

Terrestrial planet formation

Defining the role of turbulence in the early nebula is a key to understanding the growth of solids larger than meter size and the initiation of runaway growth of embryos from planetesimals ultimately leads to the Growth of large terrestrial planets via large impacts.

Dynamical Constraints on Mercury’s Collisional Origin

Of the solar system’s four terrestrial planets, the origin of Mercury is perhaps the most mysterious. Modern numerical simulations designed to model the dynamics of terrestrial planet formation

Formation of the terrestrial planets

The early phases of formation in the inner solar system were dominated by collisions and short-range dynamical interactions among planetesimals. But the later phases, which account for most of the

Possible consequences of absence of “jupiters” in planetary systems

  • G. Wetherill
  • Physics, Geology
    Astrophysics and space science
  • 1994
The formation of the gas giant planets Jupiter and Saturn probably required the growth of massive ∼ 15 Earth-mass cores on a time scale shorter than the ∼ 107 time scale for removal of nebular gas, but the probability of similar gas giants occurring in other planetary systems is unclear.

Orbital Migration Of Giant Planets: Using Numerical Integration To Investigate Consequences For Other Bodies

A number of extrasolar planets have been detected in close orbits around nearby stars. It is probable that these planets did not form in these orbits but migrated from their formation locations

Embryo Formation with GPU Acceleration: Reevaluating the Initial Conditions for Terrestrial Accretion

The solar system’s terrestrial planets are thought to have accreted over millions of years out of a sea of smaller embryos and planetesimals. Because it is impossible to know the surface density

Mars’ growth stunted by an early giant planet instability

Origin and evolution of the atmospheres of early Venus, Earth and Mars

We review the origin and evolution of the atmospheres of Earth, Venus and Mars from the time when their accreting bodies were released from the protoplanetary disk a few million years after the



Formation of the Earth

The origin of the earth is discussed in the context of the formation of the sun and the planets, and a standard model for such a formation assuming gravitational instability in a dense interstellar

N-body simulations of planetary formation

We have performed numerical simulations of the last stage of terrestrial planetary formation using an N-body code similar to that of Lecar & Aarseth. An improved treatment of collisions has been


The orbital evolution of asteroidal fragments with diameters ranging from 10 cm to 20 km, injected into the 3:1 Kirkwood gap at 2.50 A.U., has been investigated using Monte Carlo techniques. It is

A numerical simulation of the formation of the terrestrial planets

A numerical simulation of the accumulation of the terrestrial planets was performed, starting with 200 lunar-size planetesimals distributed uniformly in a plane; these were placed in circular orbits

Occurrence of Giant Impacts During the Growth of the Terrestrial Planets

Three-dimensional Monte Carlo simulations of the accumulation of the terrestrial planets in the absence of gas drag produced results that are in general agreement with the number and distribution of

Meteorites may follow a chaotic route to Earth

It is widely believed that meteorites originate in the asteroid belt, but the precise dynamical mechanism whereby material is transported to Earth has eluded discovery. The observational data for the