A rapidly changing jet orientation in the stellar-mass black-hole system V404 Cygni.

Autor: Miller-Jones JCA; International Centre for Radio Astronomy Research-Curtin University, Perth, Western Australia, Australia. james.miller-jones@curtin.edu.au., Tetarenko AJ; Department of Physics, University of Alberta, Edmonton, Alberta, Canada.; East Asian Observatory, Hilo, HI, USA., Sivakoff GR; Department of Physics, University of Alberta, Edmonton, Alberta, Canada., Middleton MJ; School of Physics and Astronomy, University of Southampton, Southampton, UK., Altamirano D; School of Physics and Astronomy, University of Southampton, Southampton, UK., Anderson GE; International Centre for Radio Astronomy Research-Curtin University, Perth, Western Australia, Australia., Belloni TM; Istituto Nazionale di Astrofisica (INAF)-Osservatorio Astronomico di Brera, Merate, Italy., Fender RP; Astrophysics, Department of Physics, University of Oxford, Oxford, UK., Jonker PG; Netherlands Institute for Space Research (SRON), Utrecht, The Netherlands.; Department of Astrophysics/IMAPP, Radboud University, Nijmegen, The Netherlands., Körding EG; Department of Astrophysics/IMAPP, Radboud University, Nijmegen, The Netherlands., Krimm HA; Universities Space Research Association, Columbia, MD, USA.; National Science Foundation, Alexandria, VA, USA., Maitra D; Department of Physics and Astronomy, Wheaton College, Norton, MA, USA., Markoff S; Anton Pannekoek Institute for Astronomy, University of Amsterdam, Amsterdam, The Netherlands.; Gravitation Astroparticle Physics Amsterdam (GRAPPA) Institute, Amsterdam, The Netherlands., Migliari S; European Space Astronomy Centre (ESAC)/European Space Agency (ESA), XMM-Newton Science Operations Centre, Madrid, Spain.; Institute of Cosmos Sciences of the University of Barcelona (ICCUB), Barcelona, Spain., Mooley KP; Astrophysics, Department of Physics, University of Oxford, Oxford, UK.; National Radio Astronomy Observatory (NRAO), Socorro, NM, USA.; Caltech, Pasadena, CA, USA., Rupen MP; Herzberg Astronomy and Astrophysics Research Centre, Penticton, British Columbia, Canada., Russell DM; New York University Abu Dhabi, Abu Dhabi, United Arab Emirates., Russell TD; Anton Pannekoek Institute for Astronomy, University of Amsterdam, Amsterdam, The Netherlands., Sarazin CL; Department of Astronomy, University of Virginia, Charlottesville, VA, USA., Soria R; International Centre for Radio Astronomy Research-Curtin University, Perth, Western Australia, Australia.; School of Astronomy and Space Sciences, University of the Chinese Academy of Sciences, Beijing, China.; Sydney Institute for Astronomy, School of Physics, The University of Sydney, Sydney, New South Wales, Australia., Tudose V; Institute for Space Sciences, Bucharest-Magurele, Romania.
Jazyk: angličtina
Zdroj: Nature [Nature] 2019 May; Vol. 569 (7756), pp. 374-377. Date of Electronic Publication: 2019 Apr 29.
DOI: 10.1038/s41586-019-1152-0
Abstrakt: Powerful relativistic jets are one of the main ways in which accreting black holes provide kinetic feedback to their surroundings. Jets launched from or redirected by the accretion flow that powers them are expected to be affected by the dynamics of the flow, which for accreting stellar-mass black holes has shown evidence for precession 1 due to frame-dragging effects that occur when the black-hole spin axis is misaligned with the orbital plane of its companion star 2 . Recently, theoretical simulations have suggested that the jets can exert an additional torque on the accretion flow 3 , although the interplay between the dynamics of the accretion flow and the launching of the jets is not yet understood. Here we report a rapidly changing jet orientation-on a time scale of minutes to hours-in the black-hole X-ray binary V404 Cygni, detected with very-long-baseline interferometry during the peak of its 2015 outburst. We show that this changing jet orientation can be modelled as the Lense-Thirring precession of a vertically extended slim disk that arises from the super-Eddington accretion rate 4 . Our findings suggest that the dynamics of the precessing inner accretion disk could play a role in either directly launching or redirecting the jets within the inner few hundred gravitational radii. Similar dynamics should be expected in any strongly accreting black hole whose spin is misaligned with the inflowing gas, both affecting the observational characteristics of the jets and distributing the black-hole feedback more uniformly over the surrounding environment 5,6 .
Databáze: MEDLINE
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