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A gas cloud on its way towards the supermassive black hole at the Galactic Centre

机译：通往银河系中心超大质量黑洞的气体云

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摘要

Measurements of stellar orbits1-3 provide compelling evidence4,5 that the compact radio source Sagittarius A* at the Galactic Centre is a black hole four million times the mass of the Sun. With the exception of modest X-ray and infrared flares67, Sgr A* is surprisingly faint, suggesting that the accretion rate and radiation efficiency near the event horizon are currently very low3'8. Here we report the presence of a dense gas cloud approximately three times the mass of Earth that is falling into the accretion zone of Sgr A*. Our observations tightly constrain the cloud's orbit to be highly eccentric, with an innermost radius of approach of only ~3,100 times the event horizon that will be reached in 2013. Over the past three years the cloud has begun to disrupt, probably mainly through tidal shearing arising from the black hole's gravitational force. The cloud's dynamic evolution and radiation in the next few years will probe the properties of the accretion flow and the feeding processes of the supermassive black hole. The kilo-electronvolt X-ray emission of Sgr A* may brighten significantly when the cloud reaches pericentre. There may also be a giant radiation flare several years from now if the cloud breaks up and its fragments feed gas into the central accretion zone.
机译：对恒星轨道1-3的测量提供了令人信服的证据4,5，表明银河中心的紧凑型射手座射手座A *是黑洞，质量是太阳质量的四百万倍。除了适度的X射线和红外耀斑67，Sgr A *令人惊讶地微弱，表明事件视界附近的吸积率和辐射效率目前非常低3'8。在这里，我们报告了一个稠密的气体云的存在，该气体云的质量大约是落入Sgr A *积聚区的地球质量的三倍。我们的观测结果严格地限制了云的轨道高度偏心，其最内层接近半径仅为2013年将达到的事件视界的约3,100倍。在过去的三年中，云已开始破坏，可能主要是通过潮汐剪切作用由黑洞的引力引起的。未来几年中，云的动态演化和辐射将探究超大质量黑洞的吸积流和馈入过程的性质。当云到达中心点时，Sgr A *的千电子伏特X射线发射可能会明显变亮。如果云破裂并且其碎片将气体送入中央吸积区，那么从现在起数年后可能还会出现巨大的辐射耀斑。

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  • 来源
    《Nature》 |2012年第7379期|p.51-54|共4页
  • 作者

    S. Gillessen; R. Genzel; T. K. Fritz; E. Quataert; C. Alig; A. Burkert; J. Cuadra; F. Eisenhauer; O. Pfuhl; K. Dodds-Eden; C. F. Gammie; T. Ott;

  • 作者单位

    Max-Planck-lnstitut fur extraterrestrische Physik (MPE), Giessenbachstrasse 1, D-85748 Garching, Germany;

    Max-Planck-lnstitut fur extraterrestrische Physik (MPE), Giessenbachstrasse 1, D-85748 Garching, Germany,Department, of Physics, Le Conte Hall, University of California, Berkeley, California 94720,USA;

    Max-Planck-lnstitut fur extraterrestrische Physik (MPE), Giessenbachstrasse 1, D-85748 Garching, Germany;

    Department, of Astronomy, University of California, Berkeley, California 94720, USA;

    Universitatssternwarte der Ludwig-Maximilians-Universitat, Scheinerstrasse 1, D-81679 Miinchen, Germany;

    Universitatssternwarte der Ludwig-Maximilians-Universitat, Scheinerstrasse 1, D-81679 Miinchen, Germany ,Max-Planck-lnstitut fur extraterrestrische Physik (MPE), Giessenbachstrasse 1, D-85748 Garching, Germany;

    DepartamentodeAstronomiayAstrofisica,PontificiaUniversidadCat6licade Chile, Vicuna Mackenna 4860,7820436 Macul, Santiago, Chile;

    Max-Planck-lnstitut fur extraterrestrische Physik (MPE), Giessenbachstrasse 1, D-85748 Garching, Germany;

    Max-Planck-lnstitut fur extraterrestrische Physik (MPE), Giessenbachstrasse 1, D-85748 Garching, Germany;

    Max-Planck-lnstitut fur extraterrestrische Physik (MPE), Giessenbachstrasse 1, D-85748 Garching, Germany;

    CenterforTheoretical Astrophysics, Astronomy and Physics Departments, University of Illinois at Urbana-Champaign, 1002 West Green Street, Urbana, Illinois 61801, USA;

    Max-Planck-lnstitut fur extraterrestrische Physik (MPE), Giessenbachstrasse 1, D-85748 Garching, Germany;

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