Conveners
Tuesday morning
- Mateusz Ruszkowski (University of Michigan)
Dr
Norbert Werner
(Stanford University)
8/12/14, 9:00 AM
Program
I will present a multi-wavelength study of the nature and origin of the multi-phase medium in giant ellipticals at the centers of low mass groups of galaxies. All systems with extended Halpha emission in our sample contain significant amounts of cold gas, which is co-spatial with the line emitting nebulae and the lowest entropy X-ray emitting plasma. I will show that while the hot atmospheres...
Dr
Massimo Gaspari
(Max Planck Institute for Astrophysics)
8/12/14, 9:25 AM
Program
It is commonly thought that supermassive black holes mainly accrete the hot gas from the surrounding intracluster medium, following the classic Bondi theory. However, in the presence of heating and turbulence due to the AGN feedback, cold clouds and filaments condense out of the hot phase via nonlinear thermal instability, up to 10s kpc radii. Through unprecedented 3D hydrodynamic simulations...
Ms
Yuan Li
(Columbia University)
8/12/14, 9:50 AM
Program
We study the influence of momentum-driven AGN feedback on cool-core clusters using high-resolution adaptive mesh refinement (AMR) simulations. Run-away cooling first happens only in the central 50 pc region while no local instability develops outside the very center of the cluster. The gas is accreted onto the super-massive black hole which powers AGN jets at an increasing rate as the entropy...
Prateek Sharma
(IISc Bangalore)
8/12/14, 11:00 AM
Program
I will summarize the thermal instability model for cold gas in cool core clusters. I will describe some recent results from our simulations with thermal conduction, turbulence, and AGN jets.
Dr
Paul Nulsen
(Harvard-Smithsonian Center for Astrophysics)
8/12/14, 11:25 AM
Program
For a supermassive black hole accreting from a hot, quasi-spherical atmosphere, it is almost inevitable that the fluid approximation fails because particle mean free paths exceed the radius well outside the black hole event horizon. Within this region, the flow needs to be modeled using the Fokker-Planck equation. In the absence of magnetic fields, the flow is analogous to the "loss cone"...
