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S. Markoff, M. Nowak (MIT, Center for Space Research), H. Falcke (MPIfR & Radio Observatory Westerbork), T. Maccarone (Sterrenkundig Instituut "Anton Pannekoek")
Accreting black holes of both stellar and Galactic scales manage to create jets which carry away a significant fraction of the system energy. How exactly these jets form and are confined is still a matter of great debate. In order to get a better handle on formation scenarios, we need to understand jet geometry, as well as their particle and magnetic field distributions. Sources with sub-Eddington bolometric luminosities are ideal for modeling jets because, as recent results have shown, jets increasingly dominate the power output in this regime. However, the extent to which their actual spectra are jet-dominated is still unclear, and untangling the inflow and outflow contributions is key to understanding their relationship. We present some recent results from modeling of X-ray binary and LLAGN jets, focusing on what can be learned about jet contributions from reflection components, and unusual geometry. We also discuss some constraints on jet models for LLAGN from our own Galactic center supermassive black hole, Sgr A*, which has recently been discovered to flare in the infrared as well as the X-rays. S.M. is supported by an NSF Astronomy & Astrophysics Postdoctoral Fellowship under award AST-0201597.
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Bulletin of the American Astronomical Society, 35#5
© 2003. The American Astronomical Soceity.