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Related Concept Videos

Kepler's First Law of Planetary Motion01:10

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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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Kepler's Second Law of Planetary Motion01:29

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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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Kepler's Third Law of Planetary Motion01:18

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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. In 1909, he formulated his first two laws based on the observations of his forebears, Nikolaus Copernicus and Tycho Brahe. However, in 1918, he published his third law of planetary motion, which gives a precise mathematical relationship between a planet's average distance from the Sun and the amount of time it takes to revolve around the Sun. It...
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Eccentricity of an Ellipse01:27

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An ellipse is a fundamental conic section defined by the constant sum of distances from any point on its curve to two fixed points, known as the foci. This geometric property can be physically demonstrated using a pencil, string, and two pins. By anchoring the string at both ends and maintaining it taut with a pencil, one can trace the outline of an ellipse.The shape and extent of the ellipse are determined by its eccentricity, e, defined as the ratio of the distance between the center and a...
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Circular Orbits and Critical Velocity for Satellites01:16

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The Moon orbits around the Earth. In turn, the Earth (and other planets) orbit the Sun. The space directly above our atmosphere is filled with artificial satellites in orbit. One can examine the circular orbit, the simplest kind of orbit, to understand the relationship between the speed and the period of planets and satellites with respect to their positions and the bodies that they orbit.
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Reduced Mass Coordinates: Isolated Two-body Problem01:12

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In classical mechanics, the two-body problem is one of the fundamental problems describing the motion of two interacting bodies under gravity or any other central force. When considering the motion of two bodies, one of the most important concepts is the reduced mass coordinates, a quantity that allows the two-body problem to be solved like a single-body problem. In these circumstances, it is assumed that a single body with reduced mass revolves around another body fixed in a position with an...
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Surface Mapping of Earth-like Exoplanets using Single Point Light Curves
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Exoplanet orbital eccentricities derived from LAMOST-Kepler analysis.

Ji-Wei Xie1, Subo Dong2, Zhaohuan Zhu3

  • 1School of Astronomy and Space Science, Nanjing University, Nanjing 210093, China; Key Laboratory of Modern Astronomy and Astrophysics in Ministry of Education, Nanjing University, Nanjing 210093, China; jwxie@nju.edu.cn dongsubo@pku.edu.cn.

Proceedings of the National Academy of Sciences of the United States of America
|September 28, 2016
PubMed
Summary
This summary is machine-generated.

The solar system

Keywords:
exoplanetsorbital eccentricitiesplanetary dynamicssolar systemtransit

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Area of Science:

  • Astronomy and astrophysics
  • Exoplanetary science

Background:

  • The solar system's circular, coplanar orbits suggest disk formation.
  • Early discovered exoplanets often have eccentric orbits, questioning solar system uniqueness.

Purpose of the Study:

  • To investigate the orbital eccentricity distribution of Kepler exoplanets.
  • To compare Kepler exoplanet systems with our solar system.

Main Methods:

  • Utilized precise host star parameters from LAMOST observations.
  • Analyzed transit duration statistics for a large, homogeneous Kepler planet sample (698 planets).

Main Results:

  • Found an eccentricity dichotomy: single-transiting planets are eccentric (e ≈ 0.3), while multiple-transiting planets are nearly circular (e ≈ 0.03) and coplanar.
  • Kepler multiples and solar system objects share a common relation between eccentricity and mutual inclination.

Conclusions:

  • The solar system's architecture is not unique; many Kepler multiple-planet systems exhibit similar low eccentricities and coplanarity.
  • Disk formation may be a common process for generating ordered planetary systems throughout the galaxy.