Active galactic nuclei (AGNs) derive their power from accretion onto supermassive black holes located in the centers of galaxies. Many phenomena connected with active galaxies derive from physical processes associated with the central engine’s accretion flow, which, depending on the mass accretion rate and possibly other parameters, such as black hole spin, generate outflows and relativistic jets. The energy output from the nucleus, whether it be radiative or kinetic, may have a profound influence on the evolution of the host galaxy and its larger scale environment. Continua a leggere Probing Active Galactic Nuclei with Radio Techniques
The greatest challenge in black hole astrophysics lies in the attempt to unify Galactic, intermediate and supermassive black holes under the same physical scheme to gain a more profound understanding of different classes of objects. In such grand-unification models, the observed behaviours and manifestations of accreting black holes are driven by only a few fundamental parameters, such as mass, accretion rate and spin. The conference tackles the issues related to accretion physics, production of jets/winds/outflows and their time evolution by putting a particular emphasis on the role of the net accretion rate onto black holes of all sizes. We are going to explore to which extent grand-unification schemes of black hole accretion are possible and also where they possibly fail. Participants are encouraged to present theoretical and/or observational results and prospects, across the entire electromagnetic spectrum, and to discuss them in the light of grand-unification paradigms of black hole accretion.
Topics suggested for the conference :
- Accretion / ejection flows around black holes: theory and observational predictions
- Disks, winds and jets at different accretion rates: observations and phenomenology
- XRBs and AGN grand-unification and scaling relations – what do they mean and where do they fail?
- Ultraluminous X-ray sources and intermediate mass black holes – the missing link?
- Time scales and variability in different accretion states
- Spin evolution and black hole mergers
- Feeding and feedback across the mass scale