Title: The X-ray emitting coronae in AGNs are outflowing  

　　Speaker: JunXian Wang (USTC) 

　　Time: Thursday, 3:00pm, November 7th 

　　Location: Lecture Hall, 3rd floor 

　　Astract: Supper Massive Black hole accretion systems, i.e., active galactic nuclei (AGNs), emit strong hard X-ray radiation, which are believed produced via inverse Compton scattering by hot and compact plasma near the black holes, named accretion disk corona. The origin and physical properties of the corona, including geometry, kinematics and dynamics, yet remain unknown. Taking [OIV] 25.89 um emission line as an isotropic indicator of the intrinsic luminosity of AGNs, we show that Seyfert 2 galaxies have intrinsically fainter absorption-corrected hard X-ray emission comparing with Seyfert 1 galaxies. This suggests the X-ray emitting corona in radio quiet AGNs is relativistically outflowing with bulk velocity of ~ 0.4 – 0.5 c., producing beamed emission toward small viewing inclinations. This remarkably matches the scenario that the role of corona could be subsumed by the base of weak jets in radio quiet AGNs, as suggested in X-ray binaries, and could naturally explain the puzzling correlation between radio and X-ray emission in radio quiet AGNs