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  Stellar winds pump the heart of the Milky Way

Calderón, D., Cuadra, J., Schartmann, M., Burkert, A., & Russell, C. M. P. (2019). Stellar winds pump the heart of the Milky Way. The Astrophysical Journal Letters, 888(1): L2. doi:10.3847/2041-8213/ab5e81.

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Item Permalink: http://hdl.handle.net/21.11116/0000-0005-DAE1-7 Version Permalink: http://hdl.handle.net/21.11116/0000-0005-DAE2-6
Genre: Journal Article

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 Creators:
Calderón, Diego1, Author              
Cuadra, Jorge, Author
Schartmann, Marc1, Author              
Burkert, Andreas1, Author              
Russell, Christopher M. P., Author
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1Optical and Interpretative Astronomy, MPI for Extraterrestrial Physics, Max Planck Society, ou_159895              

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 Abstract: The central supermassive black hole of the Milky Way, Sgr A*, accretes at a very low rate making it a very underluminous galactic nucleus. Despite the tens of Wolf–Rayet stars present within the inner parsec supplying ~10<sup>−3</sup> M <sub>⊙</sub> yr<sup>−1</sup> instellar winds, only a negligible fraction of this material (<10<sup>−4</sup>) ends up being accreted onto Sgr A*. The recent discovery of cold gas (~10<sup>4</sup> K) in its vicinity raised questions about how such material could settle in the hostile (~10<sup>7</sup> K) environment near Sgr A*. In this work we show that the system of mass-losing stars blowing winds can naturally account for both the hot, inefficient accretion flow, as well as the formation of a cold disk-like structure. We run hydrodynamical simulations using the grid-based code Ramses starting as early in the past as possible to observe the state of the system at the present time. Our results show that the system reaches a quasi-steady state in about ~500 yr with material being captured at a rate of ~10<sup>−6</sup> M <sub>⊙</sub> yr<sup>−1</sup> at scales of ~10<sup>−4</sup> pc, consistent with the observations and previous models. However, on longertimescales (≳3000 yr) the material accumulates close to the black hole in the form of a disk. Considering the duration of the Wolf–Rayet phase (~10<sup>5</sup> yr), we conclude that this scenario has likely already happened, and could be responsible for the more active past of Sgr A*, and/or its current outflow. We argue that the hypothesis of the mass-losing stars being the main regulator of the activity of the black hole deserves further consideration.

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 Dates: 2019-12-27
 Publication Status: Published online
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 Identifiers: DOI: 10.3847/2041-8213/ab5e81
Other: LOCALID: 3213677
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Title: The Astrophysical Journal Letters
  Other : Astrophys. J. Lett.
Source Genre: Journal
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Publ. Info: Chicago, IL : University of Chicago Press for the American Astronomical Society
Pages: - Volume / Issue: 888 (1) Sequence Number: L2 Start / End Page: - Identifier: ISSN: 2041-8205
CoNE: https://pure.mpg.de/cone/journals/resource/954922828215