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La dinámica caótica del giro estelar en sistemas binarios y la producción de Júpiter calientes desalineados
Natalia I Storch1, Kassandra R Anderson1, Dong Lai2
1Center for Space Research, Department of Astronomy, Cornell University, Ithaca, NY 14853, USA.
Science (New York, N.Y.)
|September 13, 2014
Resumen
Los Júpiter calientes a menudo tienen órbitas desalineadas debido a las oscilaciones de Kozai-Lidov y las fuerzas de marea. Las interacciones gravitacionales con las estrellas obladas pueden causar una caótica evolución de la rotación estelar, influyendo en la desalineación final de la rotación y la órbita.
Área de la Ciencia:
- La ciencia exoplanetaria es la ciencia de los exoplanetas.
- La astrofísica es la astrofísica.
- La mecánica celeste es una mecánica celeste.
Sus antecedentes:
- Muchos sistemas exoplanetarios con Júpiter calientes exhiben una desalineación significativa entre los ejes orbitales planetarios y los ejes de giro estelar.
- El mecanismo de Kozai-Lidov, que implica oscilaciones en la excentricidad orbital y la inclinación inducida por un compañero binario, es una teoría líder para la formación de Júpiter caliente.
- La disipación de las mareas también juega un papel crucial en la configuración de estos sistemas.
Objetivo del estudio:
- Investigar el impacto de las interacciones gravitacionales entre planetas y estrellas anfitrionas obladas en la evolución del eje de giro estelar.
- Explorar el papel de la dinámica caótica en la desalineación de la órbita de giro de los sistemas exoplanetarios.
- Comprender cómo estas interacciones contribuyen a la formación de Júpiter calientes.
Principales métodos:
- Simulaciones de la dinámica gravitacional que incorporan las interacciones planeta-estrella y la flatitud estelar.
- Análisis del comportamiento caótico en la evolución del eje de giro estelar durante los ciclos de Kozai.
- Exploración espacial de parámetros que varían la masa del planeta y el período de rotación estelar.
Principales resultados:
- Las interacciones gravitacionales pueden inducir la evolución caótica del eje de giro estelar durante los ciclos de Kozai.
- El sistema exhibe dinámicas complejas con regiones de comportamiento periódico dentro de un mar caótico, dependiendo de los parámetros del sistema.
- La disipación de las mareas, combinada con la evolución caótica del giro, deja una huella discernible en los ángulos finales de desalineación de la órbita de giro.
Conclusiones:
- La interacción gravitacional entre los planetas y las estrellas obladas es un factor importante en la dinámica de espín-órbita estelar.
- La evolución caótica del espín, influenciada por los parámetros del sistema, puede explicar los desajustes de órbita observados en los sistemas de Júpiter caliente.
- Este mecanismo proporciona una vía para comprender la prevalencia de Júpiter calientes desalineados.
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