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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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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.
On the other hand,...
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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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Schwarzschild Radius and Event Horizon01:21

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No object with a finite mass can travel faster than the speed of light in a vacuum. This fact has an interesting consequence in the domain of extremely high gravitational fields.
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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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Although black holes were theoretically postulated in the 1920s, they remained outside the domain of observational astronomy until the 1970s.
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La fría enana marrón Gliese 229 B es un binario cercano

Jerry W Xuan1, A Mérand2, W Thompson3

  • 1Department of Astronomy, California Institute of Technology, Pasadena, CA, USA. wxuan@caltech.edu.

Nature
|October 16, 2024
PubMed
Resumen

Las compañeras enanas marrones de las estrellas, similares a los planetas gigantes, desafían las teorías de formación. Las observaciones revelan que Gliese 229B es en realidad un sistema binario, Gliese 229BaBb, resolviendo discrepancias y planteando nuevas preguntas sobre la formación de enanas marrones binarias.

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Área de la Ciencia:

  • Astronomía y astrofísica
  • Ciencias exoplanetarias
  • Formación de objetos estelares y subestelares

Sus antecedentes:

  • Los compañeros enanas marrones ofrecen información sobre la formación y evolución de los planetas debido a las similitudes con los exoplanetas gigantes.
  • Varias enanas marrones son más masivas de lo previsto por la luminosidad y la edad de la estrella anfitriona, lo que sugiere teorías incompletas o múltiples componentes.

Objetivo del estudio:

  • Para investigar la discrepancia entre las predicciones teóricas y las masas observadas de las compañeras enanas marrones, específicamente Gliese 229B.
  • Resolver el aparente objeto único Gliese 229B en sus componentes constituyentes, si los hay.

Principales métodos:

  • Observaciones de Gliese 229B utilizando el interferómetro GRAVITY.
  • Observaciones independientes con el espectrógrafo CRIRES + en el Very Large Telescope.

Principales resultados:

  • Ambos conjuntos de observación resolvieron Gliese 229B en dos componentes: Gliese 229Ba y Gliese 229Bb.
  • Los componentes tienen masas de 38,1 ± 1,0 y 34,4 ± 1,5 masas de Júpiter (MJup), respectivamente.
  • Se orbitan entre sí con un período de 12,1 días y un semieje mayor de 0,042 UA.

Conclusiones:

  • El descubrimiento del sistema binario de enanas marrones Gliese 229BaBb resuelve el conflicto entre los modelos teóricos y los datos de observación.
  • Este hallazgo plantea nuevas preguntas con respecto a los mecanismos de formación y la prevalencia de sistemas de enanas marrones binarias compactas alrededor de las estrellas.