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Information to Users INFORMATION TO USERS While the most advanced technology has been used to photograph and reproduce this manuscript, the quality of the reproduction is heavily dependent upon the quality of the material submitted. For example: • Manuscript pages may have indistinct print. In such cases, the best available copy has been filmed. ® Manuscripts may not always be complete. In such cases, a note will indicate that it is not possible to obtain missing pages. ® Copyrighted material may have been removed from the manuscript. In such cases, a note will indicate the deletion. Oversize materials (e.g., maps, drawings, and charts) are photographed by sectioning the original, beginning at the upper left-hand corner and continuing from left to right in equal sections with small overlaps. Each oversize page is also filmed as one exposure and is available, for an additional charge, as a standard 35mm slide or as a 17”x 23” black and white photographic print. Most photographs reproduce acceptably on positive microfilm or microfiche but lack the clarity on xerographic copies made from the microfilm. For an additional charge, 35mm slides of 6”x 9” black and white photographic prints are available for any photographs or illustrations that cannot be reproduced satisfactorily by xerography. Order Number 8726612 The astrophysics of nebulae and active galactic nuclear emission-line regions: New methods and applications Cota, Stephen Andrew, Ph.D. The Ohio State University, 1987 U’lVI'I SOON.ZeebRd. Ann Arbor, MI 48106 The Astrophysics of Nebulae and Active Galactic Nuclear Emission-Line Regions: New Methods and Applications DISSERTATION Presented in Partial Fulfillment of die Requirements for the Degree Doctor of Philosophy in the Graduate School of The Ohio State University By Stqihen A. Cota, B. S. ***** The Ohio State University 1987 Reading Committee: Approved By Dr. Gary J. Ferland Dr. Jack A. Baldwin Dr. Eugene R. C^niotti Gary J. Ferland, Advisor Depariment of Astronomy To Sara -1- ACKNOWLEDGEMENTS It is with great pleasure that I thank my advisor. Dr. Gary J. Ferland. for his help and support in the completion of this dissertation. Thanks are due for both his oiginal research suggestions, which led to this dissertation, and for his almost daily guidance. I also want to warmly thank Dr. Eugene R. Capriotti for his constant help and advice. I owe special thanks to Dr. Jack A. Baldwin, Dr. Hagai Netzer, and Dr. Bradley M. Peterson, for reading this dissertation and for their suggestions. Finally, thanks go to Dr. David G. Lawrie, Dr. Gerald H. Newsom, and Dr. Bradley M. Peterson, for support and advice throughout the years. Nearly 5 years of graduate school has only proved that the task of obtaining a Ph.D. ever was, and ever will be, beyond the limits set by my character. Without the faith and support of my family and Mends, 1 never could have finished what 1 set out to do: 1 owe them all an enormous debt -u- VITA March 10,1960 Bom - Toledo, Ohio 1982 Phi Beta Kappa 1982 B. S., The Ohio State University, Columbus, Ohio 1983 Teaching Associate, Dq>artment of Astronomy, The Ohio State University, Columbus, Ohio 1983 - 198S Research Assistant, Departmmit of Astronomy, The Ohio State University, Columbus, Ohio 1984 Summer Research Assistant, National Astronomy Radio Observatory, Socorro, New Mexico 1986 Research Assistant, Department of Astronomy, The Ohio State University, at Lowell Observatory, Flagstaff, Arizona 1986 -1987 Presidential Fellow, The Ohio State University, Columbus, Ohio 1987 Research Assistant, Department of Astronomy, The Ohio State University, Columbus, Ohio PUBLICATIONS "The Double Broad-line Emitting Regions in NGC 5548 as Possible Evidence for a Supermassive Binary", B. M. Peterson, K. T. Kmrista, and S. A. Cota, Astrophysical Joiamal Letters , 312,1,1987. "Spectrophotometry of the Seyfot 1 Galaxy Arakelian 120", B. M. Peterson, and S. A. Cota, Astronomical Journal , 94,7,1987. "The Size of the Broad-Line Region in the Seyfert Galaxy NGC 4151", B. M. Peterson, and S. A. Cota, submitted to the AstropAyacof Journal, 1987. "Hydrogen Emissivity in Realistic Nebulae: The Effects of Velocity Fields and Internal Dust", S. A. Cota, and G. J. Ferland, submitted to ihoAstrophysical Journal, 1987. -u i- TABLE OF CONTENTS DEDICATION i ACKNOWLEDGEMENTS ü VITA iü LIST OF FIGURES iv LIST OF TABLES v CHAPTER PAGE I. INTRODUCTION 1 n . THREE-BODY RECOMBINATION TO THE HIGHLY EXCITED STATES OF ATOMS AND IONS: AN IMPORTANT PROCESS FOR NOVAE SHELLS AND BROAD-LINE EMPTUNG REGIONS OF ACTIVE GALAXIES 5 2.1 Introduction 5 2.2 Calculations 8 (a) Formalism and Assumptions 8 0)) Computational Details 11 2.3 Results 14 (a) Numerical Results 14 (b) Comparison With Previous Work 15 (c) Evaluation of Approximations 17 2.4 Discussion 19 (a) Late-Fhase Novae Shells 19 0>) H n Regions and Planetary Nebulae 20 (c) Emission-Line Regions of Active Galaxies 21 (i) Conventional Density BLRs m iNLRs 22 (ii) High Density BLRs 23 m . A SIMPLE BUT ACCURATE TREATMENT OF THE HYDROGEN ATOM 33 3.1 Introduction 33 3.2 Factors Influencing the Accuracy of Calculations of the HI Recombination Spectrum 36 (a) /-Mixing 36 0>) Atomic Data 38 (c) Truncation of the Hydrogen Atom 40 -IV- 3.3 A Simple Model Hydrogen Atom 43 (a) Model Hydrogen Atmn 44 0)) Averaging of the Rates and Populations 44 (c) Avoaging of the Eneigies and Statistical Weights 47 (d) Temperature Dqtendence of Collision and Radiative Recombination Rates 49 (e) Choice of 6 . and Results SI 3.4 Comparison With Previous Authors 55 (a) Equations for a Photoionized Slab 55 0>) Comparison to Low Density Calculations with die n-M ethod 58 (c) Comparison to High Deisity Calculations 58 (d) Comparisons at Low Temperatures 60 IV. THE RECOMBINATION SPECTRUM OF HELIUM I: THE EFFECTS OF PHOTOIONIZATION OF HYDRCXÎEN BY HE I RESONANCE PHOTONS ON THE SINGLET EMISSIVmES 89 4.1 Introduction 89 4.2 Calculations 91 (a) Helium I Singlet Energies and Transition Rates 92 (b) Line Transfer 94 (c) Temperature Dqiaidence 98 (d) Collisional Population o f 2^f £rmn 2^S 100 4.3 Results 104 4.4 Discussion 107 (a) Photoionization Models 107 (i) AGN Model 109 (« ) H / / Regions 110 (h i ) Planetary Nebulae 111 (b) Predicted Singlet Spectrum 111 (c) NGC 7027 113 V. HYDROGEN EMISSIYITY IN REALISTIC NEBULAE: THE EFFECTS OF VELOCITY FIELDS AND INTERNAL DUST 131 5.1 Introduction 131 5.2 Calculations 133 (a) The Hydrogen Atom 133 (i) The High-Density Undt 134 (« ) Low^ensity Limit 134 (b) Velocity Structure and Optical Depths 136 (c) Dust to Gas Ratio 137 (d) Radiative Transfer 139 -V- (e) Results 141 5.3 Applications 143 (a) The Orion Nebula 143 Çâ) Giant H n Regions 145 (c) Planetary Nebulae 147 (d) Nova Envelopes 148 5.4 Discussion 149 VI. THE NATURE OF THE IONIZING CONTINUUM IN SGR A WEST 156 6.1 Introduction 156 6.2 Obsmred Properties of Sgr A West 159 (a) Photoionization Models 159 (b) Geometry of Sgr A West 160 ({) Distribution m d Kinematics of the Ionized Gas 161 (ü ) Identification and Nature cf the Central Object 164 (c) Extinction 166 (i) The Near-IR Extinction Curve 166 (ü ) The Far-IR Extinction Curve 168 (ü i) Adopted Extinction 169 (d) Fine Structure Line Spectrum 170 (i) Uncertainties in the line Data 170 ( a ) Adopted Spectrum 172 (a ;) Comparison with Extragalactic Objects 172 (e) The Ionizing Continuum Shape 173 (J) The Hard X-and gamma-Ray Contmua 175 (a ) The Soft X-Ray Continuum 177 (Jii) The IR Continuum 178 (f) The Ionizing Continuum Strength 180 (i) Estimates from [Ne II] 12 J8 pm Fluxes 180 (ii) Estimates from Brackett line Fluxes 182 (Hi) Estimates from Radio Flux Denrities 183 (iv) Other Estimates 184 (g) Density 185 (i) Evidence for lo w Densities 185 (ii) Evidence for High Densities 186 (h) Abundances 188 6.3 The Broad-Line Region, 1RS 16 191 (a) Geometry 191 (b) The //e / %2.058 pm Line 191 (c) Density 194 6.4 Photoionization Calculations 197 6.5 Results 199 -VI- (a) 35,000 K Stellar Atmo^hœ 200 (b) 30,000 K Stellar Atmosphœ 201 (c) AGN Model 201 (d) 40,000 K Stellar Atmosphere 202 6 .6 Discussion 203 (a) Variants on the AGN Models of Sgr A West 204 (i) Formation of [Ar / / ] 7 jjfli and [Ne //] 12.8 pm in AGN Models 204 (« ) Turbulent Heating 206 (fii) Depletion qf Coolants 206 (iv) Optical Depths in the Fine Structure Lines 207 (v) Radiative Excitation 210 (b) Uncertainties in the Calculations 211 (/) Uncertainties in the Stellar Atmospheres 211 (« ) Incomplete or Inaccurate Atomic Data for Argon 211 (c) PredictitHis 213 (d) The Nature of Sgr A West 214 Vn. CONCLUSION 239 APPENDIX 243 BIBLIOGRAPHY 246 -vu- UST OF TABLES TABLE PAGE 1. Comparison o f N, vs. for Adams and Petrosian and the present work 2S 2. N, for Mh, (After Drake and Ulrich 1981) 61 3. Effective H p Recombination Coefficients and H I Line Ratios for Full and No I -Mixing; Case A 62 4. Effective H p Recombination Coefficients and H I Line Ratios for Full and No I -Mixing; Case B 62 5. Ctmparison of Collision Rates from the literature 63 6 . Real and Avemge Energies and Statistical Weights for Real and Fictitious Levels 64 7. Fits to the Radiative Recombination Coefficients for Level n 65 8 . Radiative Rates for m ^ 6 6 6 9. Avoaged Radiative Rates vs. rtc for Case A 67 10. Averaged Radiative Rates A vs. «g for Case B 67 11. Avaaged Radiative Rates A vs. for Case A 68 12. Avoaged Radiative Rates A vs. Re for Case B 6 8 13.
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