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The Evolution of the Large-scale ISM: Bubbles and Non-Equilibrium Ionization

The Evolution of the Large-scale ISM: Bubbles and Non-Equilibrium Ionization. M. de Avillez, D. Breitschwerdt Reporter: Sun Wei Nov 11, 2010. Introduction: CIE vs. NEI. CIE: frequent assumption good approximation in hot environments violating detailed balance

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The Evolution of the Large-scale ISM: Bubbles and Non-Equilibrium Ionization

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  1. The Evolution of the Large-scale ISM: Bubbles andNon-Equilibrium Ionization M. de Avillez, D. Breitschwerdt Reporter: Sun Wei Nov 11, 2010

  2. Introduction: CIE vs. NEI • CIE: • frequent assumption • good approximation in hot environments • violating detailed balance • Can never be maintained in evolving plasma • NEI: • Thermodynamic path dependent • Time-dependent

  3. Cooling processes • Electron impact ionization • Excitation-autoionization • Radiation & dielectronic recombination • Charge-exchange recombination & ionization • Continuum & line emissions

  4. Cooling processes (Ref) • Arnaud & Rothenflug 1985 • Arnaud & Raymond 1992 • Mazzotta et al. 1998 • Mazzitelli & Mattioli 2002 • Mattioliet al. 2006, 2007 • Radiation & dielectronic recombination • Verner & Ferland 1996 (RR rate) • Gu 2003 (DR rate) • Bryans 2006 • Badnell 2003, 2006 (RR & DR data tables) • amdpp.phys.strath.ac.uk/tamoc/RR/ or …/DR/

  5. NEI equations

  6. Plasma Modeling: EPEC • Abundance: 10 elements and solar abundance (Asplund et al. 2009) • Initial Condition: isochoric full ionized gas cooling from 1e9 K

  7. Ionization Fraction

  8. Cooling Function

  9. CIE vs. NEI

  10. Combination Lag

  11. Disk-halo interaction simulation: bubbles and superbubbles

  12. Conclusion • Cooling Function: • Time-dependent • Initial condition dependent • History dependent • Expanding vs. static: occurrence X-ray emission • Delayed Recombination: mismatch of recombination and dynamical time scales

  13. Thanks!

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