The Size, Structure, and Variability of Late-Type Stars Measured ...

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vii List of Tables 2.1 ISI Diameter Measurements Made in the Years 1999-2001 . . . . . . . . . . 23 2.2 Diameter Measurements from Various Sources: Supergiants . . . . . . . . . 25 2.3 Diameter Measurements from Various Sources: o Cet . . . . . . . . . . . . . 26 2.4 Diameter Measurements from Various Sources: Other Miras . . . . . . . . . 27 2.5 ISI Angular Diameters, Bolometric Fluxes, and Implied Effective Temperatures 29 3.1 Possible Continuum Sources of Opacity in Stellar Atmospheres . . . . . . . 59 5.1 Increase in Diameter Measured in Various Bandpasses Relative to the P20 Continuum Bandpass . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 107 5.2 Höfner Model Predicted Size Increase from Observed H 2 O Lines in o Cet in Various Bandpasses . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 107
viii Acknowledgements Over the course of my education, a number of people have been instrumental in everything I’ve accomplished. I’d like to thank my parents and family and Sally for their encouragement. I want to thank the faculty at Michigan State University, and in particular Professor Aaron Galonsky for his advisement during my time there. It’s been a privilege to work with the past and current members of the Infrared Spatial Interferometry group at SSL. I’d like to thank Bill Danchi for teaching me a good deal about the ISI, Walt Fitelson for his help making it work, Dave Hale for his company during the observations and his knowledge of the equipment, and Professor Charles Townes for his guidance and willingness to help. In addition, John, Peter, Ed, Jeff, Josh, Sam, Nick, Jerome, Kahina, and Jo Ann have all helped me complete this thesis in some way or another.
Page 1 and 2: The Size, Structure, and Variabilit
Page 3 and 4: 1 Abstract The Size, Structure, and
Page 5 and 6: iv 5 Spectroscopy and ISI Measureme
Page 7: vi 3.15 Density, Temperature, and C
Page 11 and 12: 2 to achieve resolution characteris
Page 13 and 14: 4 sources are not coaligned perfect
Page 15 and 16: 6 Intensity Profile Hankel Transfor
Page 17 and 18: 8 Figure 1.3: Possible Effective Ba
Page 19 and 20: 10 6LJQDO'HWHFWRU 6LJQDO'HWHFWRU /D
Page 21 and 22: 1995A&A...304...69P 12 Figure 1.5:
Page 23 and 24: Figure 1.6: Stellar Evolution of a
Page 25 and 26: 16 such as Mira variables, become u
Page 27 and 28: 18 wavelengths, however, its range
Page 29 and 30: 20 Figure 2.1: ISI Data for o Cet f
Page 31 and 32: 22 Figure 2.3: Uniform Disk, Limb D
Page 33 and 34: 24 2.2 Comparison of ISI Data with
Page 35 and 36: 26 Table 2.3: Diameter Measurements
Page 37 and 38: 28 measurements. χ Cyg and R Leo a
Page 39 and 40: 30 metric flux (from the reference
Page 41 and 42: 32 their surface. Very often, mater
Page 43 and 44: 34 Mira. Finally, variations in tim
Page 45 and 46: 36
Page 47 and 48: 38 Figure 3.2: Intensity Distributi
Page 49 and 50: 40 Figure 3.4: Ratio of the Best-Fi
Page 51 and 52: Figure 3.5: Synthetic Near-Infrared
Page 53 and 54: 44 Angular Diameter (mas) 60 50 40
Page 55 and 56: 46 wavelengths which would cause th
Page 57 and 58: 48 3.4.1 Static Radiative Transfer
Page 59 and 60:
50 Figure 3.8: Ratio of Photospheri
Page 61 and 62:
52 3.4.2 The Effect of Dynamic Phen
Page 63 and 64:
54 Figure 3.10: “Standard” Bowe
Page 65 and 66:
56 extension is reflected at wavele
Page 67 and 68:
58 photosphere. These results suppo
Page 69 and 70:
60 Figure 3.13: Continuum Opacity o
Page 71 and 72:
62 assuming only continuum sources.
Page 73 and 74:
64 Figure 3.16: Normalized Syntheti
Page 75 and 76:
Figure 3.17: Density and Temperatur
Page 77 and 78:
68 Figure 3.19: Apparent Size of H
Page 79 and 80:
70 of Fox and Wood (1985) [31] are
Page 81 and 82:
72 3.5 Explanation of Variations in
Page 83 and 84:
74 Figure 3.21: 2.1 µm Image of 25
Page 85 and 86:
76 at visible wavelengths either by
Page 87 and 88:
78 4.1 Implications of Diameter Mea
Page 89 and 90:
80 11 µm Diameter of o Cet vs. Dat
Page 91 and 92:
82 Figure 4.3: A uniform intensity
Page 93 and 94:
84 phase observed in the continuum
Page 95 and 96:
86 5.1 General Results of 11 µm Sp
Page 97 and 98:
88 depth are the contours plotted a
Page 99 and 100:
90 Figure 5.3: Best Fitting Calcula
Page 101 and 102:
92 of its three parameters. The con
Page 103 and 104:
94 H 2 O on their measured diameter
Page 105 and 106:
96 5.3 Modelling Spectral Features
Page 107 and 108:
98 Figure 5.7: Stellar Intensity Pr
Page 109 and 110:
Figure 5.9: Observed H 2 O Spectral
Page 111 and 112:
Figure 5.10: Höfner Model Predicte
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104 30 km/s causes the spectrum to
Page 115 and 116:
Figure 5.13: o Cet Spectra in Obser
Page 117 and 118:
108 density prediction matches the
Page 119 and 120:
110 Dixon. The infrared angular dia
Page 121 and 122:
112 [29] M. U. Feuchtinger, E. A. D
Page 123 and 124:
114 [50] A. P. Jacob, T. R. Bedding
Page 125 and 126:
116 [70] A. A. Michelson and F. G.
Page 127 and 128:
118 [92] Martin Schwarzschild. Over
Page 129:
120 [114] P. Woitke, D. Krüger, an
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The Size, Structure, and Variability of Late-Type Stars Measured ...

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