An X-ray View of Accreting Black Holes

主讲人 (Speaker): 江佳颖

主讲人单位 (Speaker's Institute): 美国韦恩州立大学

邀请人 (Invited by): 谭栢轩

时间 (Time): 星期二, 2018/01/16 - 15:00 to 16:00

地点 (Location): 珠海校区海滨红楼17栋107会议室

摘要 (Abstract):

X-ray emission from accreting black hole systems provide information on the accretion geometry of the innermost region of the black hole. Observational evidence indicates that black hole systems are consisted of an accretion disk around a central black hole with a hot illuminating corona above the disk plane. The reflection of the X-rays emitted from a corona of energetic particles surrounding an accreting black hole from the accretion disk can be used as a probe of physical processes around the central engine. The most prominent feature of the reflection spectrum, Fe K-alpha fluorescent line, can be broadened by special and general relativistic effects. Measuring the broadness of the line gives information of the inner radius of the accretion disk and hence the black hole spin. This talk mainly focuses on modelling the X-ray spectra of low-mass X-ray binaries (LXMBs) and active galactic nuclei (AGN), including systems with complex outflows, using a self-consistent relativistic reflection model.

主讲人简介 (Speaker's CV):

Dr. Chia-Ying Chiang graduated at National Tsing Hua University in 2006 and got her PhD at the University of Cambridge in 2013, on the topic “Modelling the X-ray Spectra of Accreting Black Holes”. She is now a postdoc at the Wayne State University. Her major research topic has been to probe the accretion flows and geometry of relativistic systems spanning from LMXBs to AGN using X-ray spectroscopy and timing analysis. These sources show different complexities, and she found that the reflection model offers a consistent physical scenario in explaining various systems. She has plenty of experience in reducing and analyzing X-ray data from major X-ray space missions (Chandra, XMM-Newton, NuSTAR, Suzaku, Swift, and RXTE).