The non-linear dependence of flux on black hole mass and accretion rate in core-dominated jets

• Published in: Monthly notices of the Royal Astronomical Society 2003-08, Vol.343 (3), p.L59-L64
• Main Authors: Heinz, S., Sunyaev, R. A.
• Format: Article
• Language: English
• Subjects: galaxies: active; galaxies: jets; galaxies: nuclei; radiation mechanisms: non-thermal; radio continuum: general; X-rays: binaries
• ISSN: 0035-8711; 1365-2966
• DOI: 10.1046/j.1365-8711.2003.06918.x

We derive the non-linear relation between the core flux Fν of accretion-powered jets at a given frequency and the mass M of the central compact object. For scale-invariant jet models, the mathematical structure of the equations describing the synchrotron emission from jets enables us to cancel out the model-dependent complications of jet dynamics, retaining only a simple, model-independent algebraic relation between Fν and M. This approach allows us to derive the Fν–M relation for any accretion disc scenario that provides a set of input boundary conditions for the magnetic field and the relativistic particle pressure in the jet, such as standard and advection-dominated accretion flow (ADAF) disc solutions. Surprisingly, the mass dependence of Fν is very similar in different accretion scenarios. For typical flat-spectrum core-dominated radio jets and standard accretion scenarios, we find Fν∼M17/12. The 7–9 orders of magnitude difference in black hole mass between microquasars and active galactic nuclei (AGN) jets imply that AGN jets must be about 3–4 orders of magnitude more radio-loud than microquasars, i.e. the ratio of radio to bolometric luminosity is much smaller in microquasars than in AGN jets. Because of the generality of these results, measurements of this Fν–M dependence are a powerful probe of jet and accretion physics. We show how our analysis can be extended to derive a similar scaling relation between the accretion rate ṁ and Fν for different accretion disc models. For radiatively inefficient accretion modes, we find that the flat-spectrum emission follows Fν ∝ (M ṁ)17/12.