Journal
SCIENCE
Volume 350, Issue 6265, Pages 1242-1245Publisher
AMER ASSOC ADVANCEMENT SCIENCE
DOI: 10.1126/science.aac7087
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Funding
- NSF
- NASA
- Gordon and Betty Moore Foundation
- NSF University Radio Observatories program
- CARMA
- Perimeter Institute for Theoretical Physics
- Natural Sciences and Engineering Research Council of Canada
- Government of Canada through Industry Canada
- Province of Ontario through the Ministry of Research and Innovation
- Sofja Kovalevskaja award from the Alexander von Humboldt Foundation
- Japan Society for the Promotion of Science
- Netherlands Organisation for Scientific Research
- Division Of Astronomical Sciences
- Direct For Mathematical & Physical Scien [1312034, 1207752, 1126433, 1140030, 1337663, 1310896] Funding Source: National Science Foundation
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Near a black hole, differential rotation of a magnetized accretion disk is thought to produce an instability that amplifies weak magnetic fields, driving accretion and outflow. These magnetic fields would naturally give rise to the observed synchrotron emission in galaxy cores and to the formation of relativistic jets, but no observations to date have been able to resolve the expected horizon-scale magnetic-field structure. We report interferometric observations at 1.3-millimeter wavelength that spatially resolve the linearly polarized emission from the Galactic Center supermassive black hole, Sagittarius A*. We have found evidence for partially ordered magnetic fields near the event horizon, on scales of similar to 6 Schwarzschild radii, and we have detected and localized the intrahour variability associated with these fields.
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