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Contents | Abstract | Chp 1 | Chp 2 | Chp 3 | Chp 4 | Chp 5 | Chp 6 | Chp 7 | Chp 8 | Chp 9 | Bibliography

Download PhD Thesis Contents Abstract Chapter 1 Chapter 2 Chapter 3 Chapter 4 Chapter 5 Chapter 6 Chapter 7 Chapter 8 Chapter 9 Bibliography

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List of Figures

1.1 Direct Evidence for Be Star Discs
1.2 The proposed Be star model envelope (?)1931ApJ....73...94S
1.3 H

Line profiles of Be stars
1.4 Overall variation of Pleione over ~30 years (?)1995PASJ...47..195H.
1.5 The IR excess observed in

Oph
1.6 Left Panel: A schematic representation of global one armed oscillations in a Be star disc. Right panel: Observed V/R variations in H

1.7 The geometry of the disc model
1.8 Radiation driven wind models for a rapidly rotating B star
1.9 The Bi-stability Jump
2.1 The Liverpool Telescope Filter set Transparencies
2.2 Windows of Transparency in the Atmosphere
4.1 Flow chart of the prototype pipe-line.
4.2 An example of generated R-band airmass curves
4.3 An example of generated I-band airmass curves
4.4 I,R-I diagram for Praesepe.
4.5 R,I-Z diagram for Praesepe.
4.6 I,R-I diagram for photometric cluster members of Praesepe over laid with theoretical isochrones
5.1 The tangential plane concept
5.2 Native co-ordinate system
5.3 Geometry of the Perspective Zenithal Projections
5.4 The Gnomonic Projection
5.5 Flow chart of the off-line PL
5.6 The downhill simplex method
5.7 The tolerance band generated by the PL
5.8 Comparison of reduction methods R-band
5.9 Comparison of reduction methods I-band
5.10 Comparison of reduction methods Z-band
6.1 The Strömgren filter system wavelengths
6.2 The IR excess observed in

Oph
6.3 Considering disc emission
6.4 Considering photospheric emission and disc emission
6.5 A plot of E(b-y)_cs versus EW(H

/Å(left panel) and E(b-y)_cs versus EW(H

)/Å(right panel), derived using using objects earlier than B5.
6.6 A plot of E(b-y)_cs versus EW(H

)/Å(left panel) and E(b-y)_cs versus EW(H

)/Å(right panel), derived using the full-sample.
6.7 A plot of derived M_v against tabulated M_v values
7.1 The Calculation of the

constant
7.2 Interstellar Extinction Versus the Na D₂ 5890Å Line
7.3 Circumstellar Excess Versus the Na D₂ 5890Å Line
7.4 A Plot of E(B-V )_{(H-K)_is} Versus the Sodium EW(Å ) line
7.5 A Plot of (B-V )_is+cs Versus the Na D₂ 5890Å Line EW
7.6 A Plot of E(B-V )_{(H-K)_is} Versus the Optical (B-V )_is+cs Colour
7.7 Circumstellar excess versus H

EW/Å
7.8 Circumstellar excess versus Br

EW/Å
7.9 Circumstellar excess versus Br11 EW/Å
7.10 Circumstellar excess versus Br18 EW/Å
7.11 Circumstellar excess versus HeI 2.058

m EW/Å
7.12 Circumstellar excess versus spectral subtype
7.13 Circumstellar excess versus v olimits@sin(i)
7.14 Circumstellar excess versus

olimits@sin(i)
8.1 An initial plot of E(b-y)_cs versus EW(H

)/Å(left panel) and E(b-y)_cs versus EW(H

)/Å, derived using the ?2001AA...369...99H method.
8.2 The final plot of E(b-y)_cs versus EW(H

)/Å(left panel) and E(b-y)_cs versus EW(H

)/Å, derived using the ?2001AA...369...99H method.
8.3 An initial plot of E(b-y)_cs versus EW(H

)/Å (left panel) and E(b-y)_cs versus EW(H

)/Å (right panel), derived using the ?2001AA...369...99H method, using objects below B5.

A journey of a thousand miles must begin with a single step.
Lao Tzu

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