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Cerrar agujeros negros binarios supermasivos cerrados.

C Martin Gaskell1

  • 1Astronomy Department, University of Texas, Austin, Texas 78712, USA. gaskell@astro.as.utexas.edu.

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|January 8, 2010
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Resumen
Este resumen es generado por máquina.

Los desplazamientos de línea de núcleos galácticos activos (AGN) pueden no indicar binarios de agujeros negros supermasivos (SMBB). La emisión J1536+0441 probablemente se origina en un disco, lo que desafía las teorías de fusión SMBB.

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Área de la Ciencia:

  • La astrofísica es la astrofísica.
  • La astronomía galáctica es la astronomía galáctica.

Sus antecedentes:

  • Se han atribuido amplias líneas de emisión en núcleos galácticos activos (AGN) con cambios significativos de la velocidad sistémica al movimiento orbital binario del agujero negro supermasivo (SMBB).
  • El núcleo galáctico activo J1536+0441 se propuso recientemente como un ejemplo de este fenómeno SMBB.

Objetivo del estudio:

  • Proponer una interpretación alternativa para las características espectrales observadas en el AGN J1536+0441.1.
  • Reevaluar las implicaciones para las teorías de fusión binaria de agujeros negros supermasivos si J1536+0441 no es un SMBB.

Principales métodos:

  • Análisis de datos espectrales ópticos del núcleo galáctico activo J1536+0441.1.
  • Comparación de los desplazamientos de línea observados con las predicciones para la emisión de disco frente al movimiento orbital de SMBBs.

Principales resultados:

  • Se propone que las características espectrales de J1536+0441 se originan en la emisión de la línea de disco, no en el movimiento orbital de SMBB.
  • Falta de evidencia óptica clara para SMBBs cercanos en J1536+0441.1.

Conclusiones:

  • El fenómeno observado en J1536+0441 puede explicarse por la emisión de disco, desafiando la hipótesis SMBB.
  • Si los SMBB no son responsables, sugiere que las fusiones SMBB más rápidas o la acreción interrumpida en binarios cercanos afectan la alimentación del agujero negro.