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Related Concept Videos

Kepler's First Law of Planetary Motion01:10

Kepler's First Law of Planetary Motion

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.
On the other hand,...
Kepler's Second Law of Planetary Motion01:29

Kepler's Second Law of Planetary Motion

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.
While in an elliptical orbit, the total energy of the planet is conserved. Therefore, the planet slows down when it is at apogee and...
Kepler's Third Law of Planetary Motion01:18

Kepler's Third Law of Planetary Motion

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...
Detection of Black Holes01:10

Detection of Black Holes

Although black holes were theoretically postulated in the 1920s, they remained outside the domain of observational astronomy until the 1970s.
Their closest cousins are neutron stars, which are composed almost entirely of neutrons packed against each other, making them extremely dense. A neutron star has the same mass as the Sun but its diameter is only a few kilometers. Therefore, the escape velocity from their surface is close to the speed of light.
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Gravitation Between Spherically Symmetric Masses01:14

Gravitation Between Spherically Symmetric Masses

The gravitational potential energy between two spherically symmetric bodies can be calculated from the masses and the distance between the bodies, assuming that the center of mass is concentrated at the respective centers of the bodies.
Reduced Mass Coordinates: Isolated Two-body Problem01:12

Reduced Mass Coordinates: Isolated Two-body Problem

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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Updated: Jul 20, 2026

Bringing the Visible Universe into Focus with Robo-AO
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Bringing the Visible Universe into Focus with Robo-AO

Published on: February 12, 2013

Discovery of a young planetary-mass binary.

Ray Jayawardhana1, Valentin D Ivanov

  • 1Department of Astronomy and Astrophysics, University of Toronto, Toronto, ON M5S 3H8, Canada. rayjay@astro.utoronto.ca

Science (New York, N.Y.)
|August 5, 2006
PubMed
Summary

Astronomers discovered a wide binary system of two young, planetary-mass brown dwarfs. This ultra-low-mass binary challenges current brown dwarf formation theories.

Area of Science:

  • Astronomy and Astrophysics
  • Exoplanetary Science

Background:

  • Brown dwarfs are substellar objects more massive than planets but less massive than stars.
  • Planetary-mass brown dwarfs are brown dwarfs with masses comparable to giant planets.
  • Studying brown dwarf binaries provides insights into formation mechanisms and system evolution.

Purpose of the Study:

  • To identify and characterize a potential binary system involving a young planetary-mass brown dwarf.
  • To determine the masses, age, and physical association of the components.
  • To test the validity of current brown dwarf formation models.

Main Methods:

  • Utilized observational data to resolve the Oph 162225-240515 system into two distinct objects.
  • Applied stellar/substellar evolution models to estimate masses and age.

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  • Gathered evidence to confirm coevality and physical association.

    • Main Results:

    • Identified a resolved binary system, Oph 162225-240515, composed of two planetary-mass brown dwarfs.
    • Estimated masses of approximately 14 and 7 Jupiter masses for the primary and secondary, respectively.
    • Determined an age of approximately 1 million years and a wide separation of ~240 AU.

    Conclusions:

    • The discovered wide, ultra-low-mass binary challenges popular brown dwarf formation models.
    • This system serves as a crucial test case for theories of substellar object formation.
    • Further investigation is needed to refine formation scenarios.