Supplementary materials for PhD thesis "A stellar variability survey with STEREO"

<i>This dataset comprises the files contained on a CD-ROM which was attached to the thesis when it was submitted in 2013. It was uploaded to ORDO in 2025 for preservation purposes. For more information, please refer to the thesis </i><i>“</i><i>A stellar variability survey with STEREO"</i><i> </i><i>via ORO</i><i>.</i>This thesis is the result of research done into different types of stellar variability using <i>STEREO</i>/HI-1. There are almost 900,000 stars in the field of view of <i>STEREO</i>/HI-1 and in order to manage the analysis of such numbers, the different types of variability were examined separately. Therefore, the analysis considered eclipsing binaries, chemically peculiar stars (rotational variables), short period variables (mostly pulsational variables) and long period variables (pulsational variables). In doing so, this work covers the main types of regular variability as well as the full range of timescales accessible, from periods of just a couple of hours to over a year, to a wide range of different types of star, from very hot O-type stars to cool M stars, including both young stars and stars that are nearing the end of their lives, also variability of very low amplitude, mere millimagnitudes for some rotational variables, to very large amplitudes, as much as several magnitudes for Miras, and variables have been observed as bright as 3rd magnitude down to the faint limit of 12th magnitude. As wide-ranging as my efforts have been, there is more that can yet be accomplished, from utilising <i>STEREO</i>/HI-2A data to identification and categorisation of new variables and the potential legacy for the photometric database is considerable.<br><br>This research is all my own work, except where specifically stated that is has been done by or in collaboration with others. The publications currently arising from this work are Wraight et al. (2011), which includes much of the work in Chapter 3 and Section 3.1 in particular, Wraight et al. (2012), which includes much of the work in Chapter 4, Wraight et al. (2012b), which includes much of the work in Chapter 6 and Wraight et al. (2012c) which includes much of the work in Section 3.2. A single DVD is included with supporting information.