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Related Concept Videos

Kepler's First Law of Planetary Motion01:10

Kepler's First Law of Planetary Motion

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In the early 17th century, German astronomer and mathematician Johannes Kepler postulated three laws for the motion of planets in the solar system. He formulated his first two laws based on the observations of his forebears, Nikolaus Copernicus and Tycho Brahe.
Polish astronomer Nikolaus Copernicus put forth a theory that stated a heliocentric model for the solar system. According to this heliocentric theory, all the planets, including Earth, orbit the Sun in circular orbits.
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In the early 17th century, German astronomer and mathematician Johannes Kepler postulated three laws for the motion of planets in the solar system. His first law states that all planets orbit the Sun in an elliptical orbit, with the Sun at one of the ellipse's foci. Therefore, the distance of a planet from the Sun varies throughout its revolution around the Sun.
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A thermodynamic system is a set of objects whose thermodynamic properties are of interest. The system is considered to be embedded in its surroundings or the environment. The system and its environment can exchange heat and do work on each other through a boundary that separates them. However, the immediate surroundings of the system interact with it directly and therefore have a much stronger influence on its behavior and properties.
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Phase Transitions: Vaporization and Condensation02:39

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The physical form of a substance changes on changing its temperature. For example, raising the temperature of a liquid causes the liquid to vaporize (convert into vapor). The process is called vaporization—a surface phenomenon. Vaporization occurs when the thermal motion of the molecules overcome the intermolecular forces, and the molecules (at the surface) escape into the gaseous state. When a liquid vaporizes in a closed container, gas molecules cannot escape. As these gas phase...
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Updated: May 1, 2026

Simulation of the Planetary Interior Differentiation Processes in the Laboratory
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Planetary system formation in thermally evolving viscous protoplanetary discs.

Richard P Nelson1, Phil Hellary, Stephen M Fendyke

  • 1Astronomy Unit, Queen Mary, University of London, , Mile End Road, London E1 4NS, UK.

Philosophical Transactions. Series A, Mathematical, Physical, and Engineering Sciences
|March 26, 2014
PubMed
Summary

Simulations successfully form low-mass exoplanets but struggle to create gas giants that migrate close to their stars. Further research is needed to understand giant planet formation and migration dynamics.

Keywords:
extrasolar planetsplanet formationprotoplanetary discs

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Area of Science:

  • Planetary Science
  • Astrophysics
  • Exoplanet Research

Background:

  • Extrasolar planet observations offer insights into planetary formation.
  • Understanding planet formation and migration is crucial for exoplanet studies.

Purpose of the Study:

  • To review current planet formation and migration scenarios.
  • To present and analyze results from simulations combining planetary accretion and gas-disc-driven migration.
  • To contrast simulation outcomes with observational data.

Main Methods:

  • Review of existing planet formation and migration theories.
  • Development and execution of numerical simulations incorporating planetary accretion and gas-disc interactions.
  • Comparison of simulated planetary populations with observed exoplanet data.

Main Results:

  • Simulations effectively reproduce populations of low- and intermediate-mass planets with short orbital periods.
  • Models fail to generate gas giant planets that successfully migrate to orbits near the central star.
  • Discrepancies exist between simulation predictions and observed gas giant planet distributions.

Conclusions:

  • Current models adequately explain the formation of smaller, close-in exoplanets.
  • Significant challenges remain in modeling the formation and migration of gas giant planets.
  • Future research should focus on refining models to account for gas giant survival and inward migration.