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On the role of magnetic reconnection in jet/accretion disk systems

Published online by Cambridge University Press:  21 October 2010

Elisabete M. de Gouveia Dal Pino ,
Pamela Piovezan ,
Luis Kadowaki ,
Grzegorz Kowal  and
Alex Lazarian
Elisabete M. de Gouveia Dal Pino
Affiliation:
IAG, Universidade de São Paulo, Rua do Matão 1226, São Paulo 05508-900, [email protected]
Pamela Piovezan
Affiliation:
IAG, Universidade de São Paulo, Rua do Matão 1226, São Paulo 05508-900, [email protected] Karl-Schwarzschild-Str. 1, Postfach 1317, D-85741 Garching, GermanyMPA, Garching, Germany
Luis Kadowaki
Affiliation:
IAG, Universidade de São Paulo, Rua do Matão 1226, São Paulo 05508-900, [email protected]
Grzegorz Kowal
Affiliation:
IAG, Universidade de São Paulo, Rua do Matão 1226, São Paulo 05508-900, [email protected]
Alex Lazarian
Affiliation:
Astronomy Department, University of Wisconsin, Madison, WI, USA
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Abstract

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The most accepted model for jet production is based on the magneto-centrifugal acceleration out off an accretion disk that surrounds the central source (Blandford & Payne, 1982). This scenario, however, does not explain, e.g., the quasi-periodic ejection phenomena often observed in different astrophysical jet classes. de Gouveia Dal Pino & Lazarian (2005) (hereafter GDPL) have proposed that the large scale superluminal ejections observed in microquasars during radio flare events could be produced by violent magnetic reconnection (MR) episodes. Here, we extend this model to other accretion disk systems, namely: active galactic nuclei (AGNs) and young stellar objects (YSOs), and also discuss its hole on jet heating and particle acceleration.

Keywords

accretion disksacceleration of particlesmagnetic fields
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 5 , Highlights H15: Highlights of Astronomy , November 2009 , pp. 247 - 248
Copyright
Copyright © International Astronomical Union 2010

References

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