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Parameters of Selected Central Stars of Planetary Nebulae from Consistent Optical and Uv Spectral Analysis

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Parameters of Selected Central Stars of Planetary Nebulae from Consistent Optical and Uv Spectral Analysis PARAMETERS OF SELECTED CENTRAL STARS OF PLANETARY NEBULAE FROM CONSISTENT OPTICAL AND UV SPECTRAL ANALYSIS Cornelius Bernhard Kaschinski PARAMETERS OF SELECTED CENTRAL STARS OF PLANETARY NEBULAE FROM CONSISTENT OPTICAL AND UV SPECTRAL ANALYSIS Dissertation Ph.D. Thesis an der Ludwig–Maximilians–Universitat¨ (LMU) Munchen¨ at the Ludwig–Maximilians–University (LMU) Munich fur¨ den Grad des for the degree of Doctor rerum naturalium vorgelegt von submitted by Cornelius Bernhard Kaschinski Munchen,¨ 2013 1st Evaluator: Prof. Dr. A. W. A. Pauldrach 2nd Evaluator: Prof. Dr. Barbara Ercolano Date of oral exam: 25.4.2013 Contents Contents vii List of Figures xii List of Tables xiii Zusammenfassung xv Abstract xvii 1 Introduction 1 1.1 Hot Stars . 1 1.1.1 Evolution of hot stars . 1 1.2 Impact of massive stars on the evolution of stellar clusters . 5 1.3 Motivation of this thesis . 5 1.4 Organization of this thesis . 8 2 Radiation-driven winds of hot luminous stars 11 XVII. Parameters of selected central stars of PN from consistent optical and UV spectral analysis and the universality of the mass–luminosity relation 2.1 Introduction . 12 2.2 Methods . 15 2.2.1 Parameter determination using hydrodynamic models and the UV spectrum . 15 2.2.2 Parameter determination using optical H and He lines . 18 2.2.3 Combined analysis . 19 2.3 Implementation of Stark broadening in the model atmosphere code WM-basic . 19 2.4 CSPN observational material . 25 2.5 Consistent optical and UV analysis of the CSPNs NGC 6826 and NGC 2392 . 25 2.5.1 NGC 6826 . 25 2.5.2 NGC 2392 . 34 2.5.3 Comparison of the dynamical parameters of CSPN and O star winds . 35 2.6 Summary and conclusions . 42 viii CONTENTS 3 Radiation-driven winds of hot luminous stars 45 XVIII. Wind clumpiness and the reliability of stellar and wind parameter determinations from optical and UV spectral analyses of selected central stars of planetary nebulae 3.1 Introduction . 46 3.2 Methods for the determination of stellar parameters and the investigation of CSPN winds . 49 3.3 UV and optical data for the set of central stars of planetary nebulae . 51 3.4 An extended UV analysis of a selected sample of CSPNs . 57 3.5 Accounting for clumping . 60 3.6 Model calculations for individual CSPNs . 63 3.6.1 NGC 2392 . 65 3.6.2 IC 4637 . 65 3.6.3 NGC 3242 . 65 3.6.4 IC 4593 . 65 3.6.5 IC 418 . 66 3.6.6 He 2-108 . 67 3.6.7 Tc 1 . 67 3.6.8 He 2-131 . 68 3.6.9 NGC 6826 . 72 3.6.10 Clumping and the He II l 1640 line . 72 3.7 Summary and conclusions . 72 4 Effects of shocks in stellar atmosphere models on the emission line spectrum of surround- ing H II regions 77 4.1 Introduction . 78 4.2 Methods . 79 4.2.1 WM-Basic . 81 4.2.2 MOCASSIN . 82 4.3 Results . 83 4.3.1 Effects of shocks on the stellar spectral energy distribution . 85 4.3.2 Implications for nebular line diagnostics of stellar effective temperature . 85 4.3.3 Implications for line diagnostics of electron temperature and density . 88 4.3.4 The effect of shocks on strong lines in giant H II regions . 91 4.4 Summary and conclusions . 91 5 Spectroscopic Constraints on the Form of the Stellar Cluster Mass Function 93 5.1 Introduction . 94 5.2 Observations . 95 5.2.1 NGC 2997 cluster sample . 95 5.2.2 Spectroscopy . 95 5.3 Comparison with Models . 97 5.3.1 Statistical measures . 99 5.3.2 NGC 2997 results . 99 5.4 Other cluster catalogues . 100 CONTENTS ix 5.5 Conclusions . 101 6 The Role of Environment in Stellar Clustering in Galaxies 105 6.1 Introduction . 105 6.2 Observations . 106 6.2.1 The cluster sample . 106 6.3 Comparison with Models . 109 6.4 Conclusions . 109 7 Summary and Conclusions 111 Bibliography 117 Danksagung 129 curriculum vitæ 131 x CONTENTS List of Figures 1.1 Evolution of a solar mass star . 3 2.1 Derived CSPN masses vs. luminosities . 14 2.2 Diagram illustrating the solution of the transfer equation . 17 2.3 Density structure of the D30 test models . 20 2.4 Density structure of the D45 test models . 20 2.5 D30 models testing the implemented Stark broadening in WM-basic . 21 2.6 D45 models testing the implemented Stark broadening in WM-basic . 22 2.7 Effect of different mass loss rates on the line profile of emission lines . 24 2.8 NGC 6826 fitted optical lines based on the optical set of stellar parameters . 26 2.9 NGC 6826 consistent optical and UV lines based on the optical set of stellar parameters 27 2.10 NGC 6826 consistent optical and UV lines based on the UV set of stellar parameters 28 2.11 NGC 6826 consistent optical and UV lines based on the UV set of stellar parameters although using an alternative log g value . 29 2.12 NGC 2392 fitted optical lines based on the optical set of stellar parameters . 30 2.13 NGC 2392 consistent optical and UV lines based on the optical set of stellar parameters 31 2.14 NGC 2392 consistent optical and UV lines based on the UV set of stellar parameters 32 2.15 Radiative acceleration vs. optical depth of NGC 6826 base on the set of UV parameters 35 2.16 Detailed illustration of the radiative acceleration of NGC 6826 vs. z Puppis . 38 2.17 Dynamical parameters of a sample of selected CSPNs . 39 2.18 CSPN and O star mass loss rates vs. G ......................... 41 3.1 Synthetic UV spectra from consistent models for NGC 2392 . 52 3.2 Synthetic UV spectra from consistent models for IC 4593 . 53 3.3 Synthetic UV spectra from consistent models for IC 418 . 54 3.4 Synthetic UV spectra from consistent models for NGC 6826 . 55 3.5 Comparison of Ha line profiles predicted by FASTWIND and WM-basic . 61 3.6 Ha line profile of the S35 clumping test model showing a comparison to a same model with an unscaled mass loss rate . 62 3.7 Observed optical line profiles of NGC 2392 compared to predicted line profiles from four different models . 66 3.8 Observed optical line profiles of IC 4637 compared to predicted line profiles from four different models . 67 3.9 Observed optical line profiles of NGC 3242 compared to predicted line profiles from four different models . 68 xii LIST OF FIGURES 3.10 Observed optical line profiles of IC 4593 compared to predicted line profiles from four different models . 69 3.11 Observed optical line profiles of IC 418 compared to predicted line profiles from four different models . 69 3.12 Observed optical line profiles of He 2-108 compared to predicted line profiles from four different models . 70 3.13 Observed optical line profiles of Tc 1 compared to predicted line profiles from four different models . 70 3.14 Observed optical line profiles of He 2-131 compared to predicted line profiles from four different models . 71 3.15 Observed optical line profiles of NGC 6826 compared to predicted line profiles from four different models . 71 3.16 Comparison of the unclumped to clumped synthetic UV spectrum of NGC 6826 with respect to the compatibility with the observations . 73 3.17 Comparison of the unclumped to clumped synthetic UV spectrum of IC 418 with respect to the compatibility with the observations . 73 4.1 Ionising flux of the 20kK, 30kK, and 40kK models . 82 4.2 hS−Ne parameter derived for the MOCCASIN models . 86 4.3 Graphical solution for the electron temperature line diagnostic equations for the 20kK, 30kK, and 40kK models . 90 5.1 Observed spectra of the 12 observed clusters in NGC 2997 . ..
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