An active galactic nucleus (AGN) possess a powerful physical mechanism which is acting at the centre of active galaxies producing high energetic phenomenon in a very hot and compact region called…
Fig.1.3: The Fe K line reflection spectrum between 0.3 to 10keV (Ross and Fabian, 1993).
The line profiles as shown above are an observed frame which is an interpretation from instrumental response. This response could represent multiples of both broad and narrow lines (Fabian et al., 1980; Loar, 1991; Matt et al., 1992). The observation indicates high evidence that the sources show asymmetrical profiles and obeys the Power law relationship.
In order to have a better sight into the asymmetry profile of Iron K emission lines from relativistic accretion disk of Active Galactic Nuclei (AGN), we will employ two types of statistical tests to ASCA observation of Seyfert 1 galaxies data (Nandra et al., 1996 data): distribution and regression analysis in 18-samples of seyfert 1 galaxies. In addition, a close study of the transition of hydrogen like iron which lead to the K emission at 6.4keV where theoretically be done and the result compared to Fe K line emission profiles from the accretion disk of AGN.
The K emission lines in the hydrogen like iron occur in the Balmer series transition when , and the transition factor is 0.76. Then the emitting energy becomes:
Since the atomic number of Fe is 26, then the emitting energy of Fe K line is 6.4keV which is about the peak in Fe K emission in the profiles of most of the Seyfert 1 AGNs. In real materials like iron the Columbic potential is normally affected by the static dielectric constant, of the material. Therefore, we introduce the effective mass into equation 3.1 and rewrite as
3.2 Where m* is the effective mass and m is the ordinary mass. It is observed that to get the real energy from equation 3.2, we simply assuming that m*=m and varying from 0.1-1.0. The purpose of this equation 3.2 is to find out if this result could obey a Power law relationship and to compare our result with the observed line profiles.