thesis - IRS, The Infrared Spectrograph

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56 CHAPTER 4: Abundances of Planetary Nebulae BD+30 3639 and NGC 6543Table 4.3–. Extinction for BD+30 3639. The predicted H β fluxes have been derived using the theoreticalfluxes from Hummer & Storey (1987) (see text for explanation).♯ Units in 10 −12 erg cm −2 s −1 .Ident. Transition λ Flux ♯ Predict. ♯ C Hβ(µm)H βBrα 5 → 4 4.052 25.1 304 0.51Brβ 6 → 4 2.626 13.3 283 0.48Pfα 6 → 5 7.459 7.69 292 0.50Pfγ 8 → 5 3.740 3.33 303 0.51H I 13 → 5 3.039 1.71 311 0.52Table 4.4–. Infrared measured line intensities for NGC 6543. In the last column the dereddened andaperture corrected fluxes (Flux corr ) are given. The E B−V=0.07, and the aperture correction factor is1.3 for ions measured with the smallest ISO SWS aperture (
4.5. The visual and the ultraviolet spectrum 57Table 4.5–. Ultraviolet (IUE) and optical line fluxes in units of 10 −12 erg cm −2 s −1 for BD+30 3639.The optical lines are from Aller & Hyung (1995).λ (nm) Ident. Flux obs Flux corr λ (nm) Ident. Flux obs Flux corr190.9 † C III] 1.76 21.7 551.8 [Cl III] 0.12 0.31232.6 ⋆ C II 19.7 292.5 553.8 [Cl III] 0.37 0.97372.6 [O II] 98.8 417.3 575.4 [N II] 5.15 12.89372.9 [O II] 40.2 169.6 587.6 He I 4.06 9.94406.9 [S II] 6.04 23.6 630.0 [O I] 1.88 4.30407.6 [S II] 1.62 6.31 631.2 [S III] 1.32 3.01447.1 He I 0.77 2.73 636.3 [O I] 0.71 1.61486.1 ♯ H β 93.3 293.9 658.3 [N II] 457.0 1002.9493.3 [O III] 0.06 0.18 671.6 [S II] 5.18 11.12495.9 [O III] 2.09 6.39 673.1 [S II] 11.17 24.0519.9 [N I] 0.24 0.68 858.1 [Cl II] 1.01 1.68520.1 [N I] 0.18 0.51 912.6 [Cl II] 0.27 0.43† From the IUE observations (see Sect. 4.2.2).⋆ Taken from Torres-Peimbert & Peña (1981).♯ From Acker et al. (1992).4.4.2 NGC 6543In Table 4.4 the twenty one lines measured with SWS are tabulated. Upper limits for [Mg IV]at 4.49 µm and [O IV] at 25.9 µm were also derived. Three LWS lines were also used.The strongest lines correspond to [Ne III] and [S IV]. [Si II], although faint, is also clearlydetected.It is not possible to derive the extinction in the same way as for BD+30 3639 becausethe hydrogen lines have been measured with the smallest aperture, which as discussed inSect. 4.3, may miss some nebular flux. The expected H β can be found from the 6 cm radioemission using the following equation:F (H β ) =(4.1)2.82 × 10 9 t 0.53 (1 + He+H+ 3.7 He+++ H) +In this equation the flux density S ν =0.873 Jy at 5 GHz (George et al. 1974), t is theelectron temperature in units of 10 4 K (0.82 for this nebula) and 2.82 × 10 9 is a conversionfactor to give the F (H β ) in erg cm −2 s −1 . The helium abundances used in this calculationare those of Table 4.10. The predicted H β flux is then 307.8 × 10 −12 erg cm −2 s −1 . Themeasured H β flux by Acker et al. (1992) is 245.5 × 10 −12 erg cm −2 s −1 . This leads toC Hβ =0.1 or E B−V =0.07 which we shall use in the remainder of this paper.4.5 The visual and the ultraviolet spectrumOptical and ultraviolet lines have been used to provide more information on ionization stagesof some ions, especially carbon, oxygen and nitrogen.S ν
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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
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.
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
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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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thesis - IRS, The Infrared Spectrograph

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