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2015 Archive
2010 2011 2012 2013 2014 2015 2016 2017 2018 2019 2020
Author(s): Andrew Nguyen
Presentation: poster
Many stars have constant magnitudes. However, an interesting subset of stars, known as variable stars, can change their apparent brightness. These changes occur for a variety of reasons: eclipsing partners, size changes, and internal energy fluctuations. On November 29, 2014, CCD observations we obtained for the rich star field centered at 22:08:41.22 +54:33:18.3 (2000). We present light curves for four very different variable stars: GSC 03973-01698 (Delta Scuti), VSX J220917.2+543726 (eclipsing binary), Dauban V225 (unknown type), and 4U 2206+54 (high-mass binary). These CCD observations were completed using a 30 cm SCT at an altitude of 2195 m near Sunspot, NM. Periods of 0.065 ± 0.004d and 0.309 ± 0.024d were obtained using the Lomb-Scargle method for GSC 03973-01698 and VSX J220917.2+543726, respectively. Periods were not obtained for the other variables.
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