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Atomic Processes in Gaseous Nebulae

Andri Prozesky MSc. Atomic Processes in Gaseous Nebulae. Outline. Introduction Atomic Processes Modelling Nebulae Why is this New? Why is this Important? Results Future Work. Introduction. Introduction. Atomic Processes - Radiative. Bound-bound processes. Absorption

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Atomic Processes in Gaseous Nebulae

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  1. AndriProzesky MSc Atomic Processes in Gaseous Nebulae

  2. Outline • Introduction • Atomic Processes • Modelling Nebulae • Why is this New? • Why is this Important? • Results • Future Work

  3. Introduction

  4. Introduction

  5. Atomic Processes - Radiative Bound-bound processes • Absorption • Spontaneous emission • Stimulated emission Bound-free processes • Photoionization • Radiative recombination • Stimulated recombination

  6. Atomic Processes - Collisional Bound-bound • Collisional excitation • Collisionalde-excitation Bound-free • Collisional ionization • Three-body recombination

  7. Modelling Nebulae

  8. Modelling Nebulae • Thermodynamic equilibrium Boltzmann distribution:

  9. Modelling Nebulae • Real world • Express occupation numbers ito departure coefficients (bn values) Nn in TE bn = Actual Nn

  10. Modelling Nebulae Te = Ne = 104 K 104 cm-3

  11. Modelling Nebulae • Specific focus – radio recombination lines (RRLs)

  12. Why is this new? • Full quantum mechanical treatment • Newer atomic data • Better computing power

  13. Why is this new? • Calculations to higher n • Stimulated processes included • Applicable to very wide temp range

  14. Why is this important? • New era in radio astronomy with higher sensitivity • Theory behind observations

  15. Why is this important? • Check previous results Bauman, Porter, Ferland & MacAdam (2005) ApJ 628 541

  16. Results Case A Case B

  17. Results Te = Ne = 104 K 104 cm-3

  18. Results Te = Ne = Rneb = 104 K 104 cm-3 20 pc

  19. Future work • Include He and metals • Radiation field • Structure of plasma

  20. Future work • Effects of dust • Radiative transfer

  21. Thank you

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