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Un sistema binario de estrellas gigantes y agujeros negros de baja masa que no interactúa
Todd A Thompson1,2,3, Christopher S Kochanek4,2, Krzysztof Z Stanek4,2
1Department of Astronomy, The Ohio State University, 140 W. 18th Ave., Columbus, OH 43210, USA. thompson.1847@osu.edu.
Science (New York, N.Y.)
|November 2, 2019
Resumen
Los investigadores descubrieron un compañero invisible masivo de una estrella gigante usando velocidad radial y datos fotométricos. Este agujero negro o sistema de estrellas de neutrones que no interactúa desafía los métodos de detección anteriores para tales binarios.
Área de la Ciencia:
- Astronomía y astrofísica
- Evolución estelar
- Sistemas binarios
Sus antecedentes:
- La emisión de rayos X es el método típico para detectar sistemas binarios de agujeros negros con estrellas compañeras.
- Se predice que los binarios que no interactúan son comunes, pero requieren estrategias de detección alternativas.
- El estudio se centra en la identificación de tales sistemas a través de métodos de observación indirecta.
Objetivo del estudio:
- Para investigar la naturaleza del compañero invisible masivo de la estrella gigante 2MASS J05215658+4359220.
- Demostrar un nuevo método para detectar sistemas binarios que no interactúan.
- Para restringir la masa del compañero invisible.
Principales métodos:
- Combinando las mediciones de velocidad radial con los datos de variabilidad fotométrica.
- Analizando el período orbital y la excentricidad del sistema binario.
- Utilizando parámetros estelares de la estrella gigante visible para inferir las propiedades del compañero.
Principales resultados:
- Se ha confirmado que la brillante estrella gigante 2MASS J05215658+4359220 se encuentra en un sistema binario con una compañera invisible masiva.
- El sistema exhibe un período orbital de aproximadamente 83 días y una excentricidad cercana a cero.
- La masa del compañero invisible se estima entre 5 y 10 masas solares, consistente con un agujero negro de baja masa o una estrella de neutrones masiva.
Conclusiones:
- Los hallazgos sugieren que los binarios de agujeros negros que no interactúan pueden detectarse utilizando la velocidad radial combinada y el análisis de variabilidad fotométrica.
- El compañero detectado podría ser un agujero negro de baja masa o una estrella de neutrones inusualmente masiva, proporcionando nuevos conocimientos sobre la formación de objetos compactos.
- Este estudio pone de relieve la importancia de explorar métodos alternativos para descubrir sistemas binarios que no exhiben emisión de rayos X.
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