In recently years, Star, AGN (Active Galactic Nucleus), BHC (Black Hole Candidate) etc. by Chandra and XMM-Newton satellite with high resolution spectrometer have been observed actively. Especially, Chandra have achieved high resolution in term of X-ray energy to combine grating (HETG and LETG) and high precisely CCD (Charge Coupled Device). Therefore, the X-ray spectral lines from almost stars and AGN are observed not only Lyα of Hydrogen-like Si, Mg, Ne, O, and N ions, but also much more intense lines from helium-like ions and L-shell iron ions.
In this paper, we constructed a collisional-radiative model for L-shell and M-shell iron ions and analyzed X-ray spectra from early type star (OB stars) with Chandra. Our model includes a large number of energy levels from lithium-like to magnesium-like iron ions. We can solve the rate equations assuming the ionization equilibrium. We can also solve the rate equation for non-equilibrium ionization plasmas; to solve the rate equations for only excited states. Atomic data of radiative transition rate, autoionization rate / dielectronic capture, collisional-excitation rate, collisional ionization / three-body recombination rate, and radiative recombination rate are calculated mainly by Hullac code. Furthermore we compare the collisional excitation rate coefficients by Hullac code with other published data for iron ions. Line absorptions by stellar wind around stars are also discussed to consider the radiation transfer of lines.