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Una burbuja inflada por un chorro de 300 parsecs de largo alrededor de un poderoso microquásar en la galaxia NGC 7793
Manfred W Pakull1, Roberto Soria, Christian Motch
1University of Strasbourg, CNRS UMR 7550, Observatoire Astronomique, 11 rue de l'Université, F67000 Strasbourg, France. manfred.pakull@astro.unistra.fr
Nature
|July 9, 2010
Resumen
Descubrimos un microquásar, S26, en NGC 7793 con potentes chorros, similares a SS433 pero más grandes. Sus chorros son 10.000 veces más energéticos que la emisión de su núcleo de rayos X.
Área de la Ciencia:
- * Astrofísica es la astrofísica.
- * Astrofísica de alta energía.
- * Física de los agujeros negros
Sus antecedentes:
- * Los estados de acreción de agujeros negros cerca o por encima de la luminosidad de Eddington son poco conocidos debido a la rareza de la fuente.
- * Las fuentes de rayos X ultraluminosas (ULX) son agujeros negros extranucleares luminosos, que probablemente se acrecientan a velocidades súper-Eddington.
- * Los microquásares con chorros estacionarios son menos luminosos que los ULX, y los ULX generalmente carecen de evidencia de chorros colimados.
Objetivo del estudio:
- * Para investigar la naturaleza de la gran nebulosa S26 en NGC 7793.3.
- * Para determinar si S26 es alimentado por un agujero negro con chorros colimados.
- * Para caracterizar la potencia de salida y la estructura de S26 y compararla con fuentes astrofísicas conocidas.
Principales métodos:
- * Análisis de rayos X y datos ópticos de la nebulosa S26 y su núcleo.
- * Determinación de la potencia mecánica de salida de los chorros.
- * Análisis estructural de S26, comparándolo con las galaxias activas de tipo II de Fanaroff-Riley y los microcuásares.
Principales resultados:
- * S26 es alimentado por un agujero negro que produce un par de chorros colimados.
- * La potencia mecánica de los chorros es aproximadamente unas pocas 10^40 erg s^-1, ~10^4 veces la emisión del núcleo de rayos X.
- * S26 exhibe una estructura Fanaroff-Riley tipo II, incluyendo puntos calientes de rayos X, lóbulos de radio y un capullo de rayos X.
Conclusiones:
- * S26 es un poderoso microquásar, significativamente más grande y más energético que SS433.
- * La mayor parte de la potencia de chorro de S26 se disipa en partículas térmicas dentro de los lóbulos, no en electrones relativistas.
- * Este descubrimiento proporciona nuevos conocimientos sobre los estados de acreción de agujeros negros a tasas súper-Eddington.
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