thesis - IRS, The Infrared Spectrograph

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58 CHAPTER 4: Abundances of Planetary Nebulae BD+30 3639 and NGC 6543Table 4.6–. Ultraviolet (IUE) line fluxes in units of 10 −12 erg cm −2 s −1 for NGC 6543. In Cols. 4and 8 the fluxes have been corrected for interstellar extinction using E B−V = 0.07 and an aperturecorrection factor of 1.3 has been used.λ (nm) Ident. Flux obs Flux corr λ (nm) Ident. Flux obs Flux corrLow ResolutionHigh Resolution124.4 s N V 57.7 140.28 137.1 s O V 2.64 5.99131.0 ? 11.9 27.83 148.3 N IV] 0.05 0.10131.7 b ? 7.30 17.01 148.7 N IV] 0.03 0.07137.6 s O V 29.9 67.66 155.2 s C IV 60.87 133.67140.9 ? 14.6 32.61 166.0 O III] 0.34 0.74155.2 s C IV 56.4 123.85 166.6 O III] 0.98 2.13164.1 s He II 17.4 37.96 174.6 N III] 0.22 0.47166.2 O III] 4.50 9.78 174.8 N III] 0.21 0.45172.1 N IV] 11.0 23.69 174.9 N III] 0.66 1.42174.5 N III] 1.90 4.08 190.6 C III] 8.34 18.19175.9 ? 2.50: 5.36 190.8 C III] 7.66 16.71181.4 [Ne III] 3.40 7.29 229.7 C III 1.41 3.25190.7 C III] 16.9 36.86 232.1 O III 0.07 0.15229.6 C III 4.90 11.30 232.5 C II] 0.71 1.61231.1 C II]+O III 7.10 16.25 232.7 C II] 1.19 2.70232.9 C II] 3.70 8.38 283.7 O IV]? 1.24 2.37241.9 [Ne IV] 2.20 4.74 302.5 O III 0.31 0.58251.0 He II 2.00 4.15 304.7 O III 0.55 1.02267.7 ? 2.30 4.52 313.3 ♮ O III 0.46 0.85279.0 [Ar V]+[Mg V] 2.10 4.04 320.3 s He II 0.28 0.51283.5 C II] 3.00 5.73292.2 † Mg V 0.70 1.32298.7 b [Ne V]? 2.20 4.12318.8 Si II, He I 2.30 4.20320.9 He II 1.50 2.73s Stellar line: ♮ Affected by reseau: b Blended: † May be present.: Noisy.4.5.1 BD+30 3639The optical and ultraviolet data have been taken from Aller & Hyung (1995) and Torres-Peimbert & Peña (1981) respectively. In Table 4.5 the ions used are listed. The dereddenedfluxes have been derived using an extinction of E B−V = 0.34, as derived from the infraredlines (see the previous section). Several lines of the same ion were sometimes used to confirmthe results of the ionic abundances.
4.5. The visual and the ultraviolet spectrum 59Table 4.7–. Optical line fluxes for NGC 6543. In Col. 8 the average fluxes from MP, M, AC and H-eastare given (see Sect. 4.5.2 for details). All the fluxes from Col. 3 to 8 have been corrected for extinctionusing C Hβ =0.2 (as are given in the literature) and are relative to H β . In this paper a lower extinction isfound. The last column lists the average fluxes corrected for extinction using C Hβ =0.1 (E B−V=0.07)and in units of 10 −12 erg cm −2 s −1 .λ Ident. Flux † F lux(nm) MP Midd AC H-East H-North Average372.6 [O II] 15.5 b 23.9 b 21.0 b 8.292 23.53 8.292 24.35372.9 [O II] 3.471 10.15 3.471 10.20386.9 [Ne III] 60.42 51.0 48.35 38.67 53.26 157.4396.8 [Ne III] 35.65 32.0 18.62 16.56 28.76 85.4406.9 [S II] 0.540 2.108 0.54 1.61407.6 [S II] 0.358 0.848 0.385 1.15436.3 [O III] 1.49 1.80 2.2 2.051 1.581 1.89 5.71447.2 He I 6.20 5.30 6.02 6.018 5.158 5.88 17.9468.6 He II 0.050 0.05 0.15471.1 [Ar IV] 1.3 0.935 0.284 1.12 3.45474.0 [Ar IV] 0.910 0.360 0.91 2.81486.1 H I (H β ) 100 100 100 100 100 100 310.9495.9 [O III] 264.1 227.3 218.8 172.2 236.7 740.4500.7 [O III] 774.7 663.0 675.0 704.3 518.5 704.2 2209519.2 [Ar III] 0.055 0.051 0.055 0.17551.8 [Cl III] 0.380 0.478 0.380 1.22553.8 [Cl III] 0.535 0.603 0.535 1.72575.4 [N II] 0.242 0.905 0.242 0.81587.6 He I 23.80 15.6 15.1 20.15 14.10 18.66 60.9610.2 [K IV] 0.042 0.016 0.042 0.14631.2 [S III] 0.74 0.912 1.309 0.826 2.74654.8 [N II] 10.40 5.7 4.884 21.97 6.99 23.3658.3 [N II] 17.30 16.8 16.2 17.27 59.29 16.89 56.4671.6 [S II] 0.85 0.652 3.021 0.751 2.52673.1 [S II] 1.40 1.502 5.722 1.451 4.86713.6 [Ar III] 22.2 14.0 21.18 17.45 19.13 64.8717.1 [Ar IV] 0.026 0.025 0.026 0.09753.0 [Cl IV] 0.144 0.057 0.144 0.49775.1 [Ar III] 3.0 4.674 4.589 3.837 16.10804.6 [Cl IV] 0.300 0.110 0.300 1.05857.9 [Cl II] 0.048 0.127 0.048 0.17953.1 [S III] 19.10 46.46 19.10 68.4† References: MP: Manchado & Pottasch (1989), M: from Middlemass et al. (1989), AC:Aller & Czyzak (1979), H-east and H-north: Hyung et al. (2000).b Blended with the line at 372.9 nm.
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RIJKSUNIVERSITEIT GRONINGENPhysics
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To my parents
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Contents1 Introduction 11.1 Evoluti
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CONTENTSvii5 Probing AGB nucleosynt
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1IntroductionPLANETARY NEBULAE are
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1.1. Evolution of low and intermedi
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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.
Page 55: 3.7. Conclusions 47Acknowledgements
Page 58 and 59: 50 CHAPTER 4: Abundances of Planeta
Page 77 and 78: 5Probing AGB nucleosynthesis viaacc
Page 79 and 80: 5.1. Introduction 71about the synth
Page 81 and 82: Table 5.2-. Radius, Zanstra tempera
Page 83 and 84: 5.3. Accurate abundances of ISO-obs
Page 85 and 86: 5.3. Accurate abundances of ISO-obs
Page 87 and 88: 5.4. Nucleosynthesis in low- and in
Page 89 and 90: 5.5. Synthetic TP-AGB calculations
Page 91 and 92: 5.6. Comparison between models and
Page 111 and 112: 5.7. Summary and conclusions 103Fig
Page 113 and 114: 5.7. Summary and conclusions 105A s
Page 115 and 116: 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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