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KOI-126: un triple eclipse jerárquico triple con dos estrellas de baja masa
Joshua A Carter1, Daniel C Fabrycky, Darin Ragozzine
1Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA. jacarter@cfa.harvard.edu
Science (New York, N.Y.)
|January 13, 2011
Resumen
Los datos de Kepler revelaron KOI-126, un sistema estelar triple. Este sistema presenta un sistema binario de baja masa que orbita una tercera estrella, proporcionando un punto de referencia para los modelos estelares.
Área de la Ciencia:
- La astronomía y la astrofísica.
- Física estelar Física estelar es la física estelar.
Sus antecedentes:
- La misión de la nave espacial Kepler es detectar exoplanetas mediante el monitoreo de la luz estelar.
- Los triples jerárquicos estelares son sistemas complejos que requieren una observación detallada.
Objetivo del estudio:
- Para informar de la detección de un sistema triple jerárquico estelar eclipsante, KOI-126, utilizando la fotometría de Kepler.
- Caracterizar los parámetros orbitales y las propiedades estelares del sistema KOI-126.
Principales métodos:
- Análisis de los datos fotométricos de la nave espacial Kepler.
- Identificación de los eventos de eclipse dentro de las curvas de luz.
- Modelado de las curvas de luz para determinar los parámetros orbitales y estelares.
Principales resultados:
- Detección de un sistema estelar jerárquico triple, KOI-126 [A, (B, C) ].
- Caracterización de un binario de baja masa (KOI-126 B y C) con mediciones precisas de masa y radio.
- Determinación del período orbital (1.767 días) y la excentricidad para el binario interno.
- Caracterización de la estrella exterior (KOI-126 A) con mediciones de masa y radio.
- Determinación del período orbital (33,92 días) y la excentricidad (0,304) para la órbita alrededor del binario.
Conclusiones:
- El sistema KOI-126 proporciona un laboratorio único para el estudio de la evolución estelar.
- Los componentes binarios de baja masa sondean el dominio estelar totalmente convectivo, ofreciendo una prueba crítica para los modelos estelares teóricos.
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