Observational evidence for the accretion-disk origin for a radio jet in an active galaxy

Details Observational evidence for the accretion-disk origin for a radio jet in an active galaxy Observational evidence for the accretion-disk origin for a radio jet in an active galaxy

Jun 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002natur.417..625m&link_type=abstract

Nature, Volume 417, Issue 6889, pp. 625-627 (2002).

Physics

135

Scientific paper

Accretion of gas onto black holes is thought to power the relativistic jets of material ejected from active galactic nuclei (AGN) and the `microquasars' located in our Galaxy. In microquasars, superluminal radio-emitting features appear and propagate along the jet shortly after sudden decreases in the X-ray fluxes. This establishes a direct observational link between the black hole and the jet: the X-ray dip is probably caused by the disappearance of a section of the inner accretion disk as it falls past the event horizon, while the remainder of the disk section is ejected into the jet, creating the appearance of a superluminal bright spot. No such connection has hitherto been established for AGN, because of insufficient multi-frequency data. Here we report the results of three years of monitoring the X-ray and radio emission of the galaxy 3C120. As has been observed for microquasars, we find that dips in the X-ray emission are followed by ejections of bright superluminal knots in the radio jet. The mean time between X-ray dips appears to scale roughly with the mass of the black hole, although there are at present only a few data points.

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