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

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

Nov 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010hia....15..247d&link_type=abstract

Highlights of Astronomy, Volume 15, p. 247-248

Astronomy and Astrophysics

Astronomy

Accretion Disks, Acceleration Of Particles, Magnetic Fields

Scientific paper

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.

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