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

More documents

Recommendations

Info

109 Bibliography [1] M. D. Albrow, J.-P. Beaulieu, J. A. R. Caldwell, M. Dominik, J. Greenhill, K. Hill, S. Kane, R. Martin, J. Menzies, R. M. Naber, J.-W. Pel, K. Pollard, P. D. Sackett, K. C. Sahu, P. Vermaak, R. Watson, A. Williams, and M. S. Sahu. Limb darkening of a k giant in the galactic bulge: Planet photometry of macho 97-blg-28. The Astrophysical Journal, 522:1011–1021, September 1999. [2] D. R. Alexander and J. W. Ferguson. Low-temperature rosseland opacities. The Astrophysical Journal, 437:879–891, 1994. [3] France Allard, Peter H. Hauschildt, and David Schwenke. Tio and h 2 o absorption lines in cool stellar atmospheres. The Astrophysical Journal, 540:1005–1015, September 2000. [4] R. Alvarez, A. Jorissen, B. Plez, D. Gillet, and A. Fokin. Envelope tomography of long-period variable stars. Astronomy and Astrophysics, 362:655–665, 2000. [5] J. P. Aufdenberg, A. Quirrenbach, P. H. Hauschildt, and E. Baron. Diameters of cool giant stars at 712 nm and 754 nm: Theory vs. observations. AAS, 199:#92.07, 2001. [6] Jason P. Aufdenberg and Peter H. Hauschildt. Testing spherical, expanding, lineblanketed model atmospheres of giant stars with interferometry. Proc. SPIE, 4838, 2002. not yet published. [7] T. E. Beach, L. A. Willson, and G. H. Bowen. The effects of pulsation-extended atmospheres on the apparent diameters of mira variables. The Astrophysical Journal, 329:241–252, June 1988. [8] J. A. Benson, H. M. Dyck, W. L. Mason, R. R. Howell, S. T. Ridgway, and D. J.
110 Dixon. The infrared angular diameter of alpha herculis measured with a michelson interferometer. The Astronomical Journal, 102:2091–2097, December 1991. [9] M. S. Bessell, J. M. Brett, M. Scholz, and P. R. Wood. The effects of photospheric extension upon the spectra of m-type mira variables. Astronomy and Astrophysics, 213:209–225, 1989. [10] M. S. Bessell, M. Scholz, and P. R. Wood. Phase and cycle dependence of the photospheric structure and observable properties of mira variables. Astronomy and Astrophysics, 307:481–499, 1996. [11] M. S. Bessell, M. Scholz, and P. R. Wood. Phase and cycle dependence of the photospheric structure and observable properties of mira variables. Astronomy and Astrophysics, 307:481–499, 1996. [12] M. Bester, W. C. Danchi, D. Hale, C. H. Townes, C. G. Degiacomi, D. Mékarnia, and T. R. Geballe. Measurement at 11 micron wavelengths of the diameters of α orionis and α scorpio, and changes in effective temperature of α orionis and very recent dust emmission. The Astrophysical Journal, 463:336–343, May 1996. [13] P. R. Bevington. Data Reduction and Error Analysis for the Physical Sciences, chapter Ch. 11-5. McGraw-Hill, 1969. [14] M. Born and E. Wolf. Principles of Optics. Electromagnetic Theory of Propogation, Interference, and Diffraction of Light (7th edition). Cambridge UP, 1999. [15] G. H. Bowen. Dynamical modeling of long-period variable star atmospheres. The Astrophysical Journal, 329:299–317, June 1988. [16] G. H. Bowen. Dynamical phenomena in pulsating star atmospheres. In J. Robert Buchler, editor, Numerical Modeling of Nonlinear Stellar Pulsations Problems and Prospects, pages 155–171. Kluwer Academic Publishers, March 1989. [17] G. H. Bowen. Dynamical modelling of cool supergiant atmospheres. In Instabilities in Evolved Super- and Hypergiants, pages 104–110. North-Holland, 1992. [18] D. Burns, J. E. Baldwin, R. C. Boysen, C. A. Haniff, P. R. Lawson, C. D. Mackay, J. Rogers, T. R. Scott, P. J. Warner, D. M. A. Wilson, and J. S. Young. The sur-
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 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
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: 108 density prediction matches the
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 ...

Create successful ePaper yourself

Delete template?

Save as template?