Magnetic Fields, Relativistic Jets and Accretion Disks: From Observations to Simulations and Back Again

Presented by Sean Matt, CEA Saclay

The last decade has seen a dramatic increase in the computational power available to astrophysicists. As a result, we are now able to execute large scale, three-dimensional numerical simulations based on our best insights into the physics at work in a variety of astrophysical systems and use the outputs from these calculations to provide improved interpretations of observational data. I will describe efforts along these lines in two areas: relativistic jets and accretion disks. For relativistic jets, I will describe how simulations have informed us of the physical ingredients necessary to form a jet (or otherwise); the non-linear relationships between jet composition and evolution and how results from these simulations can be used to gain improved interpretations of observations of these systems. For accretion disks, I will describe how simulations can be used to test assumptions regarding the inner structure of black hole accretion disks; how observed changes in disk variability can be used to gain insights into changes in disk physics and finally, how simulations can be used to predict observational signatures of turbulence in real disks.