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

More documents

Recommendations

Info

117 [81] A. Quirrenbach, D. Mozurkewich, J. T. Armstrong, K. J. Johnston, M. M. Colavita, and M. Shao. Interferometric observations of mira (o ceti). Astronomy and Astrophysics, 259(1):L19–L22, June 1992. [82] A. Quirrenbach, D. Mozurkewich, D. F. Buscher, C. A. Hummel, and J. T. Armstrong. Angular diameter and limb darkening of arcturus. Astonomy and Astrophysics, 312:160–166, 1996. [83] Andreas Quirrenbach. Optical interferometry. Annual Review of Astronomy and Astrophysics, 39:353–401, 2001. [84] Mark J. Reid and Karl M. Menten. Radio photospheres of long-period variable stars. The Astrophysical Journal, 476:327–346, February 1997. [85] A. Richichi, L. Fabbroni, S. Ragland, and M. Scholz. A homogenous temperature calibration for k and m giants with an extension to the coolest stars. Astronomy and Astrophysics, 344:511–520, 1999. [86] S. T. Ridgway, J. A. Benson, H. M. Dyck, L. K. Townsley, and R. A. Hermann. The infrared angular diameter of omicron ceti near maximum light. The Astronomical Journal, 104(6):2224–2228, December 1992. [87] L. S. Rothman, R. R. Gamache, R. H. Tipping, C. P. Rinsland, M. A. H. Smith, D. C. Benner, V. M. Devi, J.-M. Flaud, C. Camy-Peyret, and A. Perrin. The hitran molecular data base - editions of 1991 and 1992. JQSRT, 48(5-6):469–507, 1992. [88] V. Schirrmacher, P. Woitke, and E. Sedlmayr. A radiative instability in post-shockcooling circumstellar gas. Astronomische Gesellschaft Abstract Series, 18:P65S, 2001. [89] M. Scholz and Y. Takeda. Model study of wavelength-dependent limb-darkening and radii of m-type giants and supergiants. Astronomy and Astrophysics, 186:200–212, 1987. [90] M. Scholz and P. R. Wood. The derivation of pulsation velocities from doppler line profiles in m-type mira variables. Astronomy and Astrophysics, 362:1065–1071, 2000. [91] M. Schwarzschild. On the scale of photospheric convection in red giants and supergiants. The Astrophysical Journal, 195:137–144, January 1975.
118 [92] Martin Schwarzschild. Overtone pulsations for the standard model. The Astrophysical Journal, 94:245–252, 1941. [93] M. Shao and M. M. Colavita. Long-baseline optical and infrared stellar interferometry. Annual Review of Astronomy and Astrophysics, 30:457–498, 1992. [94] W. B. Somerville. The continuous absorption coefficient of the negative hydrogen molecular ion. The Astrophysical Journal, 139:192–197, 1964. [95] C. Sterken, E. Broens, and C. Koen. On the period history of χ cygni. Astronomy and Astrophysics, 342:167–172, 1999. [96] Kyung-Won Suh. Optical properties of the silicate dust grains in the envelopes around asymptotic giant branch stars. Mon. Not. R. Astron. Soc., 304:389–405, April 1999. [97] R. R. Thompson, M. J. Creech-Eakman, and R. L. Akeson. Time-dependent asymmetries in the atmosphere of the mira variable r trianguli through infrared interferometry. The Astrophysical Journal, 570:373–378, May 2002. [98] R. R. Thompson, M. J. Creech-Eakman, and G. T. van Belle. Multiepoch interferometric study of mira variables. i. narrowband diameters of rz pegasi and s lacertae. The Astrophysical Journal, 577:447–456, September 2002. [99] T. Tsuji. Water on the early m supergiant stars α orionis and µ cephei. The Astophysical Journal, 538:801–807, August 2000. [100] T. Tsuji. Water in k and m giant stars unveiled by iso. Astronomy and Astrophysics, 376:L1–L4, 2001. [101] Y. Tuchman. Theoretical pulsation models for long period variables. In T. Le Bertre, A. Lebre, and C. Waelkens, editors, Proc. I. A. U. Symposium. 191, Asymptotic Giant Branch Stars, pages 123–131, 1999. [102] P. G. Tuthill, C. A. Haniff, and J. E. Baldwin. Long-term diameter variations in the long-period variable o ceti. Mon. Not. R. Astron. Soc., 277:1541–1546, 1995. [103] P. G. Tuthill, C. A. Haniff, and J. E. Baldwin. Hotspots on late-type supergiants. Mon. Not. R. Astron. Soc., 285:529–539, March 1997.
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 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: 116 [70] A. A. Michelson and F. G.
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?