The magnetic nature of disk accretion onto black holes

Jon M. Miller (), John Raymond, Andy Fabian, Danny Steeghs, Jeroen Homan, Chris Reynolds, Michiel van der Klis and Rudy Wijnands
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Jon M. Miller: University of Michigan
John Raymond: Harvard-Smithsonian Center for Astrophysics
Andy Fabian: University of Cambridge
Danny Steeghs: Harvard-Smithsonian Center for Astrophysics
Jeroen Homan: Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology
Chris Reynolds: University of Maryland
Michiel van der Klis: Astronomical Institute Anton Pannekoek, University of Amsterdam
Rudy Wijnands: Astronomical Institute Anton Pannekoek, University of Amsterdam

Nature, 2006, vol. 441, issue 7096, 953-955

Abstract: The attraction of black holes We can't see black holes, they are black on a black background. But we can see where they are, thanks to the bright glow emitted by matter as it falls into the black hole. This disk accretion process is central to much of high-energy astrophysics, but observational clues as to its inner workings are rare. Using remarkable spectra obtained from the stellar-mass black-hole binary GRO J1655–40, Miller et al. have now achieved the long-sought goal of setting observational constraints on the nature of disk accretion onto compact objects. The spectra record an X-ray-absorbing wind that must be powered by a magnetic process that can also drive accretion through the disk. This demonstrates that disk accretion onto black holes is a fundamentally magnetic process.

Date: 2006
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DOI: 10.1038/nature04912

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