SIMULATED CURRENT-DRIVEN INSTABILITIES IN AGN JETS Sean M. O’Neill JILA/University of Colorado In collaboration with: Kris Beckwith (JILA/Tech-X Corporation), Mitch Begelman (JILA/APS), Krzysztof Nalewajko (JILA), Greg Salvesen (JILA/APS) Based on O’Neill, Beckwith, & Begelman (2012) What Are Current- Driven Instabilities? Why Are Current-Driven Instabilities Relevant? M87/Virgo A/Virgo X-1 Credit: X-ray: H. Marshall (MIT), et al., CXC, NASA Radio: F. Zhou, F. Owen (NRAO), J. Biretta (STScI) Optical: E. Perlman (UMBC), et al., STScI, NASA Connections With AGN Jets dominated by Poynting flux near source but kinetic energy at greater distances (Sikora et al. 2005). Connections With AGN Jets dominated by Poynting flux near source but kinetic energy at greater distances (Sikora et al. 2005). Rapid gamma-ray blazar variability (MAGIC/HESS) suggests either very large Doppler factors or emission from highly compact region (e.g. PKS 2155-304 in Aharonian et al. 2007, Mrk 501 in Albert et al. 2007). Connections With AGN Jets dominated by Poynting flux near source but kinetic energy at greater distances (Sikora et al. 2005). Rapid gamma-ray blazar variability (MAGIC/HESS) suggests either very large Doppler factors or emission from highly compact region (e.g. PKS 2155-304 in Aharonian et al. 2007, Mrk 501 in Albert et al. 2007). How do jet magnetic fields cross shear layer?