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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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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.
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Un planeta gigante de órbita ancha en el sistema binario de alta masa b Centauri

Markus Janson1, Raffaele Gratton2, Laetitia Rodet3

  • 1Department of Astronomy, Stockholm University, Stockholm, Sweden. markus.janson@astro.su.se.

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|December 9, 2021
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Los planetas gigantes pueden formarse alrededor de estrellas masivas, desafiando las suposiciones anteriores. Este estudio detectó un planeta en una órbita ancha alrededor de un sistema estelar binario masivo, expandiendo nuestra comprensión de los extremos de la formación de planetas.

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Área de la Ciencia:

  • Ciencias exoplanetarias
  • Astronomía estelar y galáctica
  • Formación y evolución de los planetas

Sus antecedentes:

  • La formación de planetas se observa a través de diversas masas estelares y arquitecturas de sistemas.
  • Estudios anteriores indicaron una disminución en la frecuencia de planetas gigantes alrededor de estrellas que superan las 1,9 masas solares (M), lo que sugiere impedimentos de formación.
  • Los métodos de detección para planetas cercanos son insensibles a los compañeros de órbita ancha.

Objetivo del estudio:

  • Para investigar la formación de planetas en todo el espacio de parámetros de masa estelar, particularmente en las masas más altas.
  • Para probar la hipótesis de que los planetas gigantes son raros o inexistentes alrededor de estrellas significativamente más masivas que el Sol.
  • Para explorar la posibilidad de que existan planetas en órbitas anchas alrededor de estrellas masivas.

Principales métodos:

  • Empleó técnicas de imagen directa para detectar exoplanetas.
  • Observaciones enfocadas en el sistema binario b Centauri de 6 a 10 M.
  • Analizó la relación de masa entre el planeta y la estrella y la separación orbital.

Principales resultados:

  • Confirmó la existencia de un planeta orbitando b Centauri a una distancia extrema de 560 veces la distancia entre el Sol y la Tierra.
  • La proporción de masa del planeta (0,10-0,17%) es comparable a la proporción de Júpiter con el Sol.
  • Este descubrimiento demuestra que los planetas pueden existir en sistemas estelares significativamente más masivos de lo que se extrapolaba anteriormente.

Conclusiones:

  • La formación de este planeta de órbita ancha alrededor de un binario masivo desafía las limitaciones del modelo de acreción del núcleo.
  • Los mecanismos de formación alternativos, como la inestabilidad gravitacional o la migración desde una ubicación de formación diferente, son plausibles.
  • Este hallazgo expande el espacio de parámetros conocido para la formación de planetas, particularmente alrededor de estrellas masivas.