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Structured outflow from a dynamo active accretion disc

Lookup NU author(s): Dr Brigitta von Rekowski, Professor Axel Brandenburg, Dr Wolfgang Dobler, Professor Anvar ShukurovORCiD


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We present an axisymmetric numerical model of a dynamo active accretion disc. If the dynamo-generated magnetic field in the disc is sufficiently strong (close to equipartition with thermal energy), a fast magneto-centrifugally driven outflow develops within a conical shell near the rotation axis, together with a slower pressure driven outflow from the outer parts of the disc as well as around the axis. Our results show that a dynamo active accretion disc can contribute to driving an outflow even without any external magnetic field. The fast outflow in the conical shell is confined by the azimuthal field which is produced by the dynamo in the disc and advected to the disc corona. This part of the outflow has high angular momentum and is cooler and less dense than its surroundings. The conical shell's half-opening angle is typically about 30° near the disc and decreases slightly with height. The slow outflow is hotter and denser.

Publication metadata

Author(s): Von Rekowski B, Brandenburg A, Dobler W, Shukurov A

Publication type: Article

Publication status: Published

Journal: Astronomy and Astrophysics

Year: 2003

Volume: 398

Issue: 3

Pages: 825-844

Print publication date: 01/02/2003

ISSN (print): 0004-6361

ISSN (electronic): 1432-0746

Publisher: EDP Sciences