Photoionization Modeling: the K Lines in addition to Edges of Iron Plan Introduction Introduction Introduction

Photoionization Modeling: the K Lines in addition to Edges of Iron Plan Introduction Introduction Introduction

Photoionization Modeling: the K Lines in addition to Edges of Iron Plan Introduction Introduction Introduction

Brown, Patricia, Contributing Writer has reference to this Academic Journal, PHwiki organized this Journal Photoionization Modeling: the K Lines in addition to Edges of Iron P. Palmeri (UMH-Belgium) T. Kallman (GSFC/NASA-USA) C. Mendoza & M. Bautista (IVIC-Venezuela) J. Krolik (JHU-USA) Plan Introduction Atomic Data Photoionized Plasma Modeling Conclusions Introduction Iron K lines are observed in (almost) all X-ray sources First reported in rocket observations of the supernova remnant Cas A

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Introduction Appear in a relatively unconfused region Emitted efficiently over wide range of temperatures in addition to ionization states Relativistically broaden in addition to red-shifted lines observed in galactic black hole c in addition to idates Introduction RXTE EXOSAT ASCA XMM Ch in addition to ra Astro-E2 Compton 1000 km/s 300 km/s The world of X-ray observatory is changing: Atomic Data Motivation: they were scarce in addition to not sufficiently accurate especially as long as the M-shell ions (Fe I-XVII) Methods: st in addition to ard atomic codes, i.e. AUTOSTRUCTURE (Badnell), HFR (Cowan) & BPRM (IP/RmaX Projects)

Atomic Data L-shell ions (Fe XVIII-XXV) CI: {2s,2p}N+[1s]{2s,2p} N+1+up to double excitations to M-shell Semi-empirical corrections: compilation of Shirai et al (2000) M-shell ions (Fe I-XVII) Focus on K-vacancy states produced by removing a 1s electron from the ground configuration No experimental energies Ab initio calculations Few experimental data (wavelengths): Fe X & solid state Core Relaxation Effects Electrons in K-vacancy & valence configurations see radically different potentials different orbitals as long as initial & final states of inner-shell transitions affects level energies, wavelengths & rates !!! -increase radiative rates by ~5-10% -increase KLL rates by ~10% -no systematic effect on KLM rates -decrease KMM rates by ~10% Damping Effect Resonances be as long as e K-edge Spectator channels (Damping channels) Participator channels

Damping Effect: Photoabsorption Fe XVII Fe XXIII With damping Without damping Damping Effect: Electron Impact Without damping With damping Fe XIX 2p4 3P2 [1s]2p5 3Po2 [1s]2p5 3Po1 [1s]2p5 3Po0 Line Energy vs. Ionization Stage Blue=Makishima Black=these studies Line moves to red near Fe IX Complicated K line structure

Edge Energy vs. Ionization Stage In first row ions, ground level is split by various valence configurations Blue=Makishima Black=these studies In 2nd in addition to 3rd row ions, Splitting is smaller, Results differ significantly From previous K/K ratio vs. Ionization Stage K/K ratio is a potential diagnostic of ionization Fluorescence Yield vs. Ion. Stage

Photoionized Plasma Modeling With XSTAR Photoionization of a gas by intense external X-ray source (dominant) Other processes affecting ionization, excitation & temperature are in equilibrium Local conditions (ionization fractions, temperature, opacity) parameterized by =Ionization parameter =4Ionizing flux/gas density Photoionized Plasma Modeling: Atomic Processes Each ion has ~3-30 K-vacancy levels which can be populated by photoionization ~4-100 K lines per ion considered in our treatment Ionization Balance & Temperature 104

Simulated Spectra Conclusions Structure of Iron K shell is more complicated than has been previously appreciated, & care is needed to accurately compute useful quantities There is a shortage of experimental data needed as long as accurate spectral modeling especially in intermediate & low ionization stages Converging series of damped resonances act to smear absorption edges Emission lines contain structure which has diagnostic value, even as long as low ionization gas

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