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Jet launching and field advection in quasi-Keplerian discs

Published online by Cambridge University Press:  24 February 2011

Jonathan Ferreira  and
Pierre Olivier Petrucci
Jonathan Ferreira
Affiliation:
Laboratoire d'Astrophysique de Grenoble, CNRS, Université Joseph Fourier, B.P. 53, F-38041 Grenoble, France
Pierre Olivier Petrucci
Affiliation:
Laboratoire d'Astrophysique de Grenoble, CNRS, Université Joseph Fourier, B.P. 53, F-38041 Grenoble, France
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Abstract

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The fact that self-confined jets are observed around black holes, neutron stars and young forming stars points to a jet launching mechanism independent of the nature of the central object, namely the surrounding accretion disc. The properties of Jet Emitting Discs (JEDs) are briefly reviewed. It is argued that, within an alpha prescription for the turbulence (anomalous viscosity and diffusivity), the steady-state problem has been solved. Conditions for launching jets are very stringent and require a large scale magnetic field Bz close to equipartition with the total (gas and radiation) pressure. The total power feeding the jets decreases with the disc thickness: fat ADAF-like structures with h ~ r cannot drive super-Alfvénic jets. However, there exist also hot, optically thin JED solutions that would be observationally very similar to ADAFs.

Finally, it is argued that variations in the large scale magnetic Bz field is the second parameter required to explain hysteresis cycles seen in LMXBs (the first one would be Ṁa).

Keywords

accretion, accretion disks(magnetohydrodynamics:) MHD(stars:) binaries: generalISM: jets and outflowsgalaxies: jets
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 6 , Symposium S275: Jets at all Scales , September 2010 , pp. 260 - 264
Copyright
Copyright © International Astronomical Union 2011

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