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  Sgr A* near-infrared flares from reconnection events in a magnetically arrested disc

Dexter, J., Tchekhovskoy, A., Jiménez-Rosales, A., Ressler, S. M., Bauböck, M., Dallilar, Y., et al. (2020). Sgr A* near-infrared flares from reconnection events in a magnetically arrested disc. Monthly Notices of the Royal Astronomical Society, 497(1), 4999-5007. doi:10.1093/mnras/staa2288.

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Dexter, J.1, Author              
Tchekhovskoy, A., Author
Jiménez-Rosales, A.1, Author              
Ressler, S. M., Author
Bauböck, M.1, Author              
Dallilar, Y.1, Author              
de Zeeuw, P. T.1, Author              
Eisenhauer, F.1, Author              
Fellenberg, S. von1, Author              
Gao, F.1, Author              
Genzel, R.1, Author              
Gillessen, S.1, Author              
Habibi, M.1, Author              
Ott, T.1, Author              
Stadler, J.1, Author              
Straub, O.1, Author              
Widmann, F.1, Author              
Affiliations:
1Infrared and Submillimeter Astronomy, MPI for Extraterrestrial Physics, Max Planck Society, ou_159889              

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 Abstract: Large-amplitude Sgr A* near-infrared (NIR) flares result from energy injection into electrons near the black hole event horizon. Astrometry data show continuous rotation of the emission region during bright flares, and corresponding rotation of the linear polarization angle. One broad class of physical flare models invokes magnetic reconnection. Here, we show that such a scenario can arise in a general relativistic magnetohydrodynamic simulation of a magnetically arrested disc. Saturation of magnetic flux triggers eruption events, where magnetically dominated plasma is expelled from near the horizon and forms a rotating, spiral structure. Dissipation occurs via reconnection at the interface of the magnetically dominated plasma and surrounding fluid. This dissipation is associated with large increases in NIR emission in models of Sgr A*, with durations and amplitudes consistent with the observed flares. Such events occur at roughly the time-scale to re-accumulate the magnetic flux from the inner accretion disc, ≃10 h for Sgr A*. We study NIR observables from one sample event to show that the emission morphology tracks the boundary of the magnetically dominated region. As the region rotates around the black hole, the NIR centroid and linear polarization angle both undergo continuous rotation, similar to the behaviour seen in Sgr A* flares.

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 Dates: 2020-08-11
 Publication Status: Published online
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 Rev. Type: Peer
 Identifiers: DOI: 10.1093/mnras/staa2288
Other: LOCALID: 3284840
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Title: Monthly Notices of the Royal Astronomical Society
  Other : Mon. Not. R. Astron. Soc.
Source Genre: Journal
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Publ. Info: Oxford : Oxford University Press
Pages: - Volume / Issue: 497 (1) Sequence Number: - Start / End Page: 4999 - 5007 Identifier: ISSN: 1365-8711
CoNE: https://pure.mpg.de/cone/journals/resource/1000000000024150