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Áreas de investigación Ciencias físicas Física de la materia condensada Propiedades electrónicas y magnéticas de la materia condensada; superconductividad
Áreas de investigación
Ciencias físicas
Física de la materia condensada
Propiedades electrónicas y magnéticas de la materia condensada; superconductividad
Las entradas rápidas como el combustible adyacente de los discos de acreción de agujeros negros supermasivos en cuásares

Las entradas rápidas como el combustible adyacente de los discos de acreción de agujeros negros supermasivos en cuásares

Hongyan Zhou ^1,2,3, Xiheng Shi ^4,5, Weimin Yuan ^6,7, Lei Hao ⁸, Xiangjun Chen ^5,9, Jian Ge ¹⁰, Tuo Ji ^4,5, Peng Jiang ^4,5, Ge Li ^5,9, Bifang Liu ^6,7, Guilin Liu ^5,9, Wenjuan Liu ^11,12, Honglin Lu ^5,9, Xiang Pan ^4,5, Juntai Shen ⁸, Xinwen Shu ¹³, Luming Sun ^5,9, Qiguo Tian ^4,5, Huiyuan Wang ^5,9, Tinggui Wang ^5,9, Shengmiao Wu ^4,5, Chenwei Yang ^4,5, Shaohua Zhang ^4,5, Zhihao Zhong ^5,9

Hongyan Zhou ^1,2,3, Xiheng Shi ^4,5, Weimin Yuan ^6,7

¹Antarctic Astronomy Research Division, Key Laboratory for Polar Science of the State Oceanic Administration, Polar Research Institute of China, Shanghai, China. zhouhongyan@pric.org.cn.
²School of Astronomy and Space Sciences, University of Science and Technology of China, Hefei, China. zhouhongyan@pric.org.cn.
³Key Laboratory for Research in Galaxies and Cosmology of Chinese Academy of Sciences, Department of Astronomy, University of Science and Technology of China, Hefei, China. zhouhongyan@pric.org.cn.
⁴Antarctic Astronomy Research Division, Key Laboratory for Polar Science of the State Oceanic Administration, Polar Research Institute of China, Shanghai, China.
⁵School of Astronomy and Space Sciences, University of Science and Technology of China, Hefei, China.
⁶National Astronomical Observatories of China, Chinese Academy of Sciences, Beijing, China.
⁷School of Astronomy and Space Science, University of Chinese Academy of Sciences, Beijing, China.
⁸Shanghai Astronomical Observatory, Chinese Academy of Sciences, Shanghai, China.
⁹Key Laboratory for Research in Galaxies and Cosmology of Chinese Academy of Sciences, Department of Astronomy, University of Science and Technology of China, Hefei, China.
¹⁰Department of Astronomy, University of Florida, Bryant Space Science Center, Gainesville, FL, USA.
¹¹Yunnan Observatories, Chinese Academy of Sciences, Kunming, China.
¹²Key Laboratory for the Structure and Evolution of Celestial Objects, Chinese Academy of Sciences, Kunming, China.
¹³Department of Physics, Anhui Normal University, Wuhu, China.

⁰Antarctic Astronomy Research Division, Key Laboratory for Polar Science of the State Oceanic Administration, Polar Research Institute of China, Shanghai, China. zhouhongyan@pric.org.cn.

Nature +

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6 de septiembre de 2019

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6 de septiembre de 2019

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Ver abstracta en PubMed

Resumen

Este resumen es generado por máquina.

Los científicos observaron el flujo de gas en los agujeros negros supermasivos, proporcionando la primera evidencia directa de las entradas que llegan a los discos de acreción de cuásares. Este descubrimiento ayuda a entender cómo estos motores cósmicos crecen e impactan en sus galaxias anfitrionas.

Área De La Ciencia

Astronomía y astrofísica
Fenómenos cósmicos

Sus Antecedentes

Los cuásares son núcleos galácticos extremadamente luminosos impulsados por la acreción de gas en los agujeros negros supermasivos.
La evidencia anterior sugería un flujo de gas hacia los discos de acreción, pero faltaba la observación directa de los flujos entrantes que alcanzaban el disco.

Objetivo Del Estudio

Proporcionar evidencia observacional inequívoca de las entradas de gas que llegan a los discos de acreción en los cuásares.
Para caracterizar la velocidad y la proximidad del gas que cae a los agujeros negros supermasivos.

Principales Métodos

Detección de líneas de absorción amplias desplazadas al rojo de hidrógeno y helio en espectros de cuásares.
Análisis de las velocidades Doppler para inferir el movimiento del gas.
Modelado por fotoionización para determinar las distancias de entrada.

Principales Resultados

Se han observado líneas de absorción desplazadas hacia el rojo que indican velocidades de entrada de gas de hasta 5000 km/s.
Contrató el gas de mayor velocidad dentro de los 10.000 radios gravitacionales del agujero negro.
El modelado de fotoionización sugiere que el flujo de entrada ocurre a aproximadamente 1,000 radios gravitacionales, potencialmente superponiendo el disco de acreción.

Conclusiones

Flujos de entrada de gas observados directamente que llegan a las proximidades de los discos de acreción de cuásares.
Los hallazgos apoyan los modelos de crecimiento de agujeros negros y los mecanismos de retroalimentación de cuásares.
Esto proporciona información crucial sobre el proceso de alimentación de los agujeros negros supermasivos.

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