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      Radio emission from the unbound debris of tidal disruption events

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          ABSTRACT

          When a star gets too close to a supermassive black hole, it is torn apart by the tidal forces. Roughly half of the stellar mass becomes unbound and flies away at tremendous velocities – around 10 4 km s −1. In this work, we explore the idea that the shock produced by the interaction of the unbound debris with the ambient medium gives rise to the synchrotron radio emission observed in several tidal disruption event (TDE). We use a moving mesh numerical simulation to study the evolution of the unbound debris and the bow shock around it. We find that as the periapse distance of the star decreases, the outflow becomes faster and wider. A TDE whose periapse distance is a factor of 7 smaller than the tidal radius can account for the radio emission observed in ASASSN-14li. This model also allows us to obtain a more accurate estimate for the gas density around the centre of the host galaxy of ASASSN-14li.

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          Author and article information

          Journal
          Mon Not R Astron Soc
          Mon Not R Astron Soc
          mnras
          Monthly Notices of the Royal Astronomical Society
          Oxford University Press
          0035-8711
          1365-2966
          August 2019
          10 June 2019
          10 June 2020
          : 487
          : 3
          : 4083-4092
          Affiliations
          [1 ]Canadian Institute for Theoretical Astrophysics, 60 St. George St., Toronto, ON M5S 3H8, Canada
          [2 ]Columbia Astrophysics Laboratory, Columbia University, 550 West 120th Street, New York, NY 10027, USA
          [3 ]Racah Institute of Physics, the Hebrew University, 91904 Jerusalem, Israel
          [4 ]Department of Physics and Astronomy, Johns Hopkins University, Baltimore, MD 21228, USA
          Author notes
          Author information
          http://orcid.org/0000-0002-5230-5514
          Article
          PMC6588130 PMC6588130 6588130 stz1567
          10.1093/mnras/stz1567
          6588130
          31258198
          b2483547-3de4-4b41-8644-af7cb2f4948c
          © 2019 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society

          This article is published and distributed under the terms of the Oxford University Press, Standard Journals Publication Model ( https://academic.oup.com/journals/pages/open_access/funder_policies/chorus/standard_publication_model)

          History
          : 06 March 2019
          : 27 May 2019
          : 31 May 2019
          Page count
          Pages: 10
          Funding
          Funded by: National Sleep Foundation 10.13039/100003187
          Award ID: AST-1615084
          Award ID: AST-1715032
          Funded by: National Aeronautics and Space Administration 10.13039/100000104
          Award ID: NNX16AR73G
          Award ID: 80NSSC17K0501
          Funded by: European Research Council 10.13039/501100000781
          Funded by: Simons Foundation 10.13039/100000893
          Award ID: 559794
          Funded by: National Institutes of Health 10.13039/100000002
          Award ID: 1G20RR030893-01
          Categories
          Article

          radiation mechanisms: non-thermal,shock waves
          radiation mechanisms: non-thermal, shock waves

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