thesis - IRS, The Infrared Spectrograph

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Cover Image: Planetary Nebula M 57, also known as the Ring Nebula. Image credit: HubbleHeritage Team (AURA/STScI/NASA).Back-cover Image: Planetary Nebula MyCn18, an Hourglass Nebula. Image credit: RaghvendraSahai and John Truger (JPL), the WFPC2 science team and NASA.
Contents1 Introduction 11.1 Evolution of low and intermediate mass stars . . . . . . . . . . . . . . . . 21.1.1 From the cradle to the grave . . . . . . . . . . . . . . . . . . . . . 21.1.2 Nucleosynthesis . . . . . . . . . . . . . . . . . . . . . . . . . . . 31.1.3 Mixing episodes during the evolution . . . . . . . . . . . . . . . . 31.2 Planetary Nebulae . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 41.2.1 PNe and the chemical enrichment of the ISM . . . . . . . . . . . . 41.2.2 Importance of PNe . . . . . . . . . . . . . . . . . . . . . . . . . 51.2.3 Neutral material around PNe . . . . . . . . . . . . . . . . . . . . 51.2.4 PNe in a general context . . . . . . . . . . . . . . . . . . . . . . . 61.3 Physics in PNe . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 71.3.1 The spectrum . . . . . . . . . . . . . . . . . . . . . . . . . . . . 71.3.2 Electron density and temperature, and abundances . . . . . . . . . 81.4 Studying PNe in the infrared . . . . . . . . . . . . . . . . . . . . . . . . . 101.5 In this thesis . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 122 The ISO–SWS Spectrum of Planetary Nebula NGC 7027 132.1 Introduction . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 142.2 ISO observations . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 142.3 Data reduction . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 152.4 Line flux discussion . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 162.5 The visual and the ultraviolet spectrum . . . . . . . . . . . . . . . . . . . 182.6 Analysis . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 212.6.1 Electron density . . . . . . . . . . . . . . . . . . . . . . . . . . . 212.6.2 Electron temperature . . . . . . . . . . . . . . . . . . . . . . . . 222.6.3 Abundances . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 232.7 Discussion . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 262.7.1 Missing stages of ionization . . . . . . . . . . . . . . . . . . . . . 262.7.2 Physical parameters . . . . . . . . . . . . . . . . . . . . . . . . . 272.7.3 Abundances with recombination lines . . . . . . . . . . . . . . . . 272.7.4 Abundances and progenitor . . . . . . . . . . . . . . . . . . . . . 282.8 Conclusions . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 28
Page 1 and 2: RIJKSUNIVERSITEIT GRONINGENPhysics
Page 3: To my parents
Page 7 and 8: CONTENTSvii5 Probing AGB nucleosynt
Page 9 and 10: 1IntroductionPLANETARY NEBULAE are
Page 11 and 12: 1.1. Evolution of low and intermedi
Page 13 and 14: 1.2. Planetary Nebulae 5Flash−Dri
Page 15 and 16: 1.3. Physics in PNe 7their whole li
Page 17 and 18: 1.3. Physics in PNe 95.35 eVO IIIλ
Page 19 and 20: 1.4. Studying PNe in the infrared 1
Page 21 and 22: 2The ISO-SWS Spectrum ofPlanetary N
Page 23 and 24: 2.3. Data reduction 15Table 2.1-. C
Page 25 and 26: 2.4. Line flux discussion 17Table 2
Page 27 and 28: 2.5. The visual and the ultraviolet
Page 29: 2.6. Analysis 21Table 2.5-. Electro
Page 32 and 33: 24 CHAPTER 2: The ISO-SWS Spectrum
Page 39 and 40: 3An ISO and IUE study of PlanetaryN
Page 41 and 42: 3.3. Corrections to line fluxes 33[
Page 43 and 44: 3.4. Line fluxes 35Table 3.1-. Comp
Page 45 and 46: Table 3.3-. IUE intensities, fluxes
Page 47 and 48: 3.5. Physical parameters 393.4.3 Op
Page 49 and 50: 3.5. Physical parameters 41Table 3.
Page 51 and 52: 3.6. Chemical abundances 43Table 3.
Page 53 and 54: 3.6. Chemical abundances 45Table 3.
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3.7. Conclusions 47Acknowledgements
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50 CHAPTER 4: Abundances of Planeta
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5Probing AGB nucleosynthesis viaacc
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5.1. Introduction 71about the synth
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Table 5.2-. Radius, Zanstra tempera
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5.3. Accurate abundances of ISO-obs
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5.3. Accurate abundances of ISO-obs
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5.4. Nucleosynthesis in low- and in
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5.5. Synthetic TP-AGB calculations
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5.6. Comparison between models and
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5.7. Summary and conclusions 103Fig
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5.7. Summary and conclusions 105A s
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6Physical Conditions in PDRs around
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6.2. Observations 109are not promin
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6.4. General parameters of the PNe
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6.4. General parameters of the PNe
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Table 6.3-. Radius, Zanstra tempera
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6.6. Lines fluxes 117Figure 6.2-. S
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6.7. Physical conditions of the PDR
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6.8. PDRs versus Shocks 127Figure 6
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6.10. Atomic, ionized and molecular
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6.10. Atomic, ionized and molecular
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6.11. General discussion 133Table 6
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6.11. General discussion 135Figure
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6.12. Summary and Conclusions 137su
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7Conclusions and future workTHE res
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141• PNe with He/H > 0.14. The st
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143HERSCHEL The launch of this sate
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Nederlandse SamenvattingSTERREN wor
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Nederlandse Samenvatting 147Figuur
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Nederlandse Samenvatting 149PHOTOIO
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Nederlandse Samenvatting 151Figuur
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Nederlandse Samenvatting 153infraro
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English SummarySTARS are born, live
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English Summary 157Figure 2-. Two e
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English Summary 159PHOTOIONIZATIONR
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English Summary 161Figure 5-. Spect
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English Summary 163all) stages of i
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BibliographyAcker A., Marcout J., O
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BIBLIOGRAPHY 167Henry R.B.C., Kwitt
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BIBLIOGRAPHY 169Pottasch S.R., Bern
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List of PublicationsPublications in
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AcknowledgementsI could easily writ
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Acknowledgements 175sense of humor,
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