Abstract Hot accretion disk coronae may account for substantial X-ray flux in AGN. We present the results from a novel coronal emission model which builds upon the knowledge we have of solar-stellar coronae. The model considers a population of non-thermal relativistic electrons (injected at the top of an accretion disk magnetic loop) and computes the emission due to the relevant physical mechanisms. The results are compared with the X-ray spectrum of AGN's observed by BeppoSAX. The constraints on model parameters are discussed.
NON THERMAL EMISSION FROM AGN DISK CORONAE / P. PIETRINI; C. TORRICELLI. - STAMPA. - (2003), pp. 129-130. (Intervento presentato al convegno ACTIVE GALACTIC NUCLEI: FROM CENTRAL ENGINE TO HOST GALAXY, MEETING HELD IN MEUDON, FRANCE, JULY 23-27, 2002, EDS.: S. COLLIN, F. COMBES AND I. SHLOSMAN. ASP (ASTRONOMICAL SOCIETY OF THE PACIFIC), CONFERENCE SERIES, VOL. 290, P. 129. tenutosi a Meudon, France nel July 23-27, 2002).
NON THERMAL EMISSION FROM AGN DISK CORONAE
PIETRINI, PAOLA;
2003
Abstract
Abstract Hot accretion disk coronae may account for substantial X-ray flux in AGN. We present the results from a novel coronal emission model which builds upon the knowledge we have of solar-stellar coronae. The model considers a population of non-thermal relativistic electrons (injected at the top of an accretion disk magnetic loop) and computes the emission due to the relevant physical mechanisms. The results are compared with the X-ray spectrum of AGN's observed by BeppoSAX. The constraints on model parameters are discussed.
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