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

More documents

Recommendations

Info

Figure 3.15: Density, Temperature, and Calculated 11 µm Opacity as a Function of Radius for Static, Radiation Dominated Supergiant Model Atmosphere 63
64 Figure 3.16: Normalized Synthetic Intensity Profile of Static Radiation Dominated Supergiant Model at Continuum Wavelengths at 1.6 and 11.15 µm. The apparent sizes resulting from a uniform disk fit at each wavelength are 52.71 and 53.36 mas, respectively 11 µm.) Also, the 1.6 µm profile edge is about 1.1% lower than the 11 µm edge. The combination of these two effects, when resulting visibilities are fit to a uniform disk, yields a diameter which is 1.2% greater in size at 11 µm than at 1.6 µm. Both intensity profiles are very nearly a uniform disk, however, due to the relatively steep fall off of density in the model. It should be noted that this in no way implies that a bandpass near 1.6 µm would not be contaminated by spectral lines. In fact, there are very strong H 2 O lines in this region that would cause the intensity profile to appear very different. This should serve only as an illustration of the wavelength dependencies of continuum effects. Because radiation pressure was neglected, the actual extension in α Ori may be somewhat larger; however, gas absorption coefficients near the photosphere are unlikely to be large enough to increase
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 and 8:
vi 3.15 Density, Temperature, and C
Page 9 and 10:
viii Acknowledgements Over the cour
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: 62 assuming only continuum sources.
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
Page 113 and 114: 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
show all

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

You also want an ePaper? Increase the reach of your titles

Delete template?

Save as template?