thesis - IRS, The Infrared Spectrograph

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72 CHAPTER 5: Probing AGB nucleosynthesis via accurate Planetary Nebula abundancesTable 5.1–. Parameters of the PNe. The m V is not corrected for extinction. References to distance, Vmagnitude and extinction are given by superscripts dx, mx, and ex respectively.Name l( ◦ ) b( ◦ ) d (kpc) m V (mag) E B−V C/O He/HNGC 2440 d1,m1,e1 234.8 2.42 1.63 17.49 0.34 > 1 0.119NGC 5315 d2,m2,e2 309.1 -4.40 2.60 14.40 0.37 < 1 0.124NGC 6302 d3,m3,e3 349.5 1.06 1.60 18.90: 0.88 < 1 0.170NGC 6445 d1,e4,e4 8.08 3.90 2.25 19.04 0.72 < 1 0.140NGC 6537 d1,m4,e5 10.10 0.74 1.95 22.40 1.22 ∼ 1 0.149NGC 6543 d4,m1,e6 96.47 29.9 1.00 11.29 0.07 < 1 0.118NGC 6741 d1,m5,e7 34.6 -2.28 1.65 19.26 0.75 1 0.111NGC 7027 d5,m1,e8 84.93 -3.50 0.65 16.53 0.85 > 1 0.106NGC 7662 d3,m1,e7 106.6 -17.6 0.96 ∗ 14.00 0.12 < 1 0.088He 2-111 d1,m3,e5 315.0 -0.37 2.50 20.00: 0.77 < 1 0.185References: d1 Average from Acker et al. (1992); d2 Liu et al. (2001); d3 Terzian (1997);d4 Reed et al. (1999); d5 Bains et al. (2003); m1 Ciardullo et al. (1999); m2 Acker et al.(1992); m3 Assumed m V ; m4 Pottasch (2000); m5 Heap et al. (1989); e1 Bernard Salas et al.(2002, chapter 3); e2 Pottasch et al. (2002); e3 Beintema & Pottasch (1999); e4 van Hoofet al. (2000); e5 Pottasch et al. (2000); e6 Bernard-Salas et al. (2003, chapter 4); e7 Pottaschet al. (2001); e8 Bernard Salas et al. (2001, chapter 2).: Large error.∗ Average distance by Terzian (1997).5.2 Sample of PNe5.2.1 GeneralThe sample used is biased to bright objects, in order to measure many different stages ofionization and accurately derive their abundances. The general parameters of the PNe usedin this study are given in Table 5.1. References for the assumed distances, magnitudes andextinction are given as footnotes in the table.Galactic coordinates show that most of these nebulae belong to the disk (exceptNGC 6543 and NGC 7662) and could be descendants of young progenitors. Distances arevery uncertain and great care was taken to adopt the most reliable ones from the literature.They vary between 0.8 and 2.5 kpc and therefore are close, as would be expected for brightobjects. There are different values in the literature that do not agree within the uncertaintiesthe authors quote. Note that the m V of He 2-111 and NGC 6302 are assumed since their centralstars have never been seen. The extinction is low in most cases except for NGC 6537. Inorder to classify them according to their chemical composition the last two columns of Table5.1 give the C/O and He/H ratios. There are two C-rich PNe, six O-rich PNe and two forwhich it is difficult to assess their nature since the C/O ratio is (although lower than one) veryclose to unity (within the uncertainties). Notice that this sample contains a higher percentageof PNe with a high He/H ratio than many other samples.
Table 5.2–. Radius, Zanstra temperature and luminosity of the observed PNe. F(Hβ) and F(4684Å) are in units of 10 −12erg cm −2 s −1 (not corrected for extinction). The radius is in meter.Name Hydrogen HeliumF(Hβ) † Radius log( L∗L ⊙) log T Z (H) F(4686Å) ∗ Radius log( L∗L ⊙) log T Z (He)NGC 2440 31.6 2.2E+07 2.95 5.25 19.3 2.1E+07 3.08 5.29NGC 5315 38.1 2.7E+08 3.34 4.80 - - - -NGC 6302: 29.5 1.7E+07 3.86 5.52 16.6 1.7E+07 3.88 5.53NGC 6445 7.60 2.4E+07 3.19 5.28 3.40 2.4E+07 3.19 5.28NGC 6537 2.20 5.8E+06 3.50 5.67 3.10 4.6E+06 4.09 5.87NGC 6543 245 3.6E+08 2.96 4.64 14.7 2.8E+08 3.46 4.82NGC 6741 4.40 1.8E+07 2.69 5.22 1.60 1.8E+07 2.69 5.22NGC 7027 75.9 2.7E+07 3.31 5.29 31.1 2.8E+07 3.27 5.28NGC 7662 102 7.8E+07 2.54 4.87 17.4 6.8E+07 2.82 4.97He 2-111: 0.98 2.5E+07 2.37 5.08 0.89 2.0E+07 2.82 5.24: Large error in the radius, temperature and luminosity.† From the same references as the extinction in Table 5.1.∗ From Acker et al. (1992).5.2. Sample of PNe 73
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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
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1.3. Physics in PNe 7their whole li
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1.3. Physics in PNe 95.35 eVO IIIλ
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1.4. Studying PNe in the infrared 1
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2The ISO-SWS Spectrum ofPlanetary N
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2.3. Data reduction 15Table 2.1-. C
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2.4. Line flux discussion 17Table 2
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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: 5.1. Introduction 71about the synth
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
Page 117 and 118: 6.2. Observations 109are not promin
Page 119 and 120: 6.4. General parameters of the PNe
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Page 123 and 124: Table 6.3-. Radius, Zanstra tempera
Page 125 and 126: 6.6. Lines fluxes 117Figure 6.2-. S
Page 127 and 128: 6.7. Physical conditions of the PDR
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6.7. Physical conditions of the PDR
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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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