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A relativistic jetted outburst from a massive black hole fed by a tidally disrupted star

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posted on 21.10.2019 by JS Bloom, D Giannios, BD Metzger, SB Cenko, DA Perley, NR Butler, NR Tanvir, AJ Levan, PTO Brien, LE Strubbe, FD Colle, E Ramirez-Ruiz, WH Lee, S Nayakshin, E Quataert, AR King, A Cucchiara, J Guillochon, GC Bower, AS Fruchter, AN Morgan, AJVD Horst
While gas accretion onto some massive black holes (MBHs) at the centers of galaxies actively powers luminous emission, the vast majority of MBHs are considered dormant. Occasionally, a star passing too near a MBH is torn apart by gravitational forces, leading to a bright panchromatic tidal disruption flare (TDF). While the high-energy transient Swift J164449.3+573451 ("Sw 1644+57") initially displayed none of the theoretically anticipated (nor previously observed) TDF characteristics, we show that the observations (Levan et al. 2011) suggest a sudden accretion event onto a central MBH of mass ~10^6-10^7 solar masses. We find evidence for a mildly relativistic outflow, jet collimation, and a spectrum characterized by synchrotron and inverse Compton processes; this leads to a natural analogy of Sw 1644+57 with a smaller-scale blazar. The phenomenologically novel Sw 1644+57 thus connects the study of TDFs and active galaxies, opening a new vista on disk-jet interactions in BHs and magnetic field generation and transport in accretion systems.
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Funding

We thank R. Romani, C. McKee and L. Blitz for close reads of drafts of this work and for helpful interactions. We are grateful to entire Swift team for work on their remarkable facilities that enabled discovery of this event. Swift, launched in November 2004, is a NASA mission in partnership with the Italian Space Agency and the UK Space Agency. Swift is managed by NASA Goddard. Penn State University controls science and flight operations from the Mission Operations Center in University Park, Pennsylvania. Los Alamos National Laboratory provides gamma-ray imaging analysis. JSB and his group were partially supported by grants NASA/NNX10AF93G, NASA/NNX10AI28G, and NSG/AST-100991. DG acknowledges support from the Lyman Spitzer, Jr. Fellowship awarded by the Department of Astrophysical Sciences at Princeton University. BDM is supported by NASA through Einstein Postdoctoral Fellowship grant number PF9-00065 awarded by the Chandra X-ray Center, which is operated by the Smithsonian Astrophysical Observatory for NASA under contract NAS8-03060. SBC wishes to acknowledge generous support from Gary & Cynthia Bengier, the Richard & Rhoda Goldman fund, NASA/Swift grant NNX10AI21G, NASA Fermi grant NNX10A057G, and NSF grant AST-0908886. WHL is supported in part by CONACyT grant 83254. AJvdH was supported by NASA grant NNH07ZDA001-GLAST.

History

Citation

Science, 2011, 333 (6039), pp. 203-206

Author affiliation

/Organisation/COLLEGE OF SCIENCE AND ENGINEERING/Department of Physics and Astronomy

Version

AM (Accepted Manuscript)

Published in

Science

Publisher

American Association for the Advancement of Science

eissn

1095-9203

Copyright date

2011

Available date

21/10/2019

Publisher version

https://science.sciencemag.org/content/333/6039/203

Notes

The primary references for the data presented here were given in the text and may be found in (20) or in the NASA/Swift archive (http://heasarc.nasa.gov/docs/swift/archive/).

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en

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