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Probing the accretion disk - jet connection via instabilities in the inner accretion flow. From microquasars to quasars

Published online by Cambridge University Press:  24 February 2011

Agnieszka Janiuk ,
Bożena Czerny ,
Monika Mościbrodzka  and
Aneta Siemiginowska
Agnieszka Janiuk
Affiliation:
Center for Theoretical Physics, PAN, Al. Lotnikow 32/46, 02-668 Warsaw, Poland email: agnieszka.janiuk@gmail.com
Bożena Czerny
Affiliation:
N. Copernicus Astronomical Center, Bartycka 18, 00-716 Warsaw, Poland
Monika Mościbrodzka
Affiliation:
Department of Physics, University of Illinois, 1110 West Green Street, Urbana, IL 61801, USA
Aneta Siemiginowska
Affiliation:
Harvard Smithsonian Center for Astrophysics, 60 Garden St, Cambridge, MA 02138, USA
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Abstract

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We present various instability mechanisms in the accreting black hole systems which might indicate at the connection between the accretion disk and jet. The jets observed in microquasars can have a peristent or blobby morphology. Correlated with the accretion luminosity, this might provide a link to the cyclic outbursts of the disk. Such duty-cycle type of behaviour on short timescales results from the thermal instability caused by the radiation pressure domination. The same type of instability may explain the cyclic radioactivity of the supermassive black hole systems. The somewhat longer timescales are characteristic for the instability caused by the partial hydrogen ionization. The distortions of the jet direction and complex morphology of the sources can be caused by precession of the disk-jet axis.

Keywords

physical data and processes: accretionX-rays:binariesgalaxies: active
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 6 , Symposium S275: Jets at all Scales , September 2010 , pp. 94 - 95
Copyright
Copyright © International Astronomical Union 2011

References

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