Variable stars stand out for their rhythmic luminosity changes, which make them essential subjects for astronomical studies. Through Lab 7, I had the opportunity to engage closely with several of these objects, applying data from sources like Gaia and SIMBAD to my own observational data to deepen my understanding of variable stars and their characteristics. In this blog post, I aim to explore some of the more interesting variables that I came across during my research. Altogether I hope this post can help deepen our understanding of celestial objects and the active process of science.
In order to study variable stars and investigate the relationships of these variable stars as a whole, I analyzed historical photometric data sourced from publicly available databases like ASAS and ASAS-SN. This analysis involved extracting detailed light curves to precisely measure periodicity and amplitude variations, enabling a thorough understanding of each star’s pulsation patterns and inherent stellar properties. To compute the light curves for each variable star, I utilized Google Colaboratory, applying periodogram analysis to determine the precise periods of variability for each star, ensuring the analysis was both accurate and efficient.
TT Lyncis is a variable star situated within the boundaries of the Lynx constellation, though it does not align with the constellation’s main outline (https://www.universeguide.com/star/44428/ttlyncis). Located within the Hercules constellation, ROTSE1 J172446.33+435021.7 is a celestial body classified primarily as an RR Lyrae variable (https://www.aavso.org/vsx/index.php?view=detail.top&oid=137752).
Variable Star Analysis Highlights
1. TT Lyn: TT Lyn, a variable star in the constellation Lynx, my findings confirm its classification as an RRAB type RR Lyrae. Positioned at coordinates 09 03 07.79 +44 35 08.1, TT Lyn exhibited a periodicity of 0.5974264 days, closely matching the previously recorded data, thereby affirming its stable pulsation pattern. The light curve analysis indicated a rise time of 18% within its luminosity cycle, with brightness varying between a maximum magnitude of 9.45 and a minimum of 10.14.
Phased Light Curve for TT Lyn
2. ROTSE1 J172446.33+435021.7: ROTSE1 J172446.33+435021.7, a star initially classified as an RRC type RR Lyrae but suggested for reclassification as an eclipsing binary (EB). Positioned in the Hercules constellation, the extensive data review revealed a significant discrepancy in its period; initially recorded at 0.46016699 days, my findings adjusted this to 0.9202451 days, nearly doubling the expected value. This large period difference, along with the observed light curve characteristics, strongly indicates that ROTSE1 J172446.33+435021.7 exhibits behaviour typical of an eclipsing binary rather than a pulsating RR Lyrae, highlighting the need for its reclassification in astronomical catalogs. The maximum and minimum magnitudes observed were 12.22 and 12.5, respectively, with no significant light contamination noted, further supporting the revised classification.
Phased Light Curve for ROTSE1 J172446.33+435021.7
This project not only enriched my understanding of stellar objects but also underscored the importance of meticulous data analysis in astronomy, and the role the public can have in contributing to scientific discoveries. By engaging directly with the raw observational data and matching it against theoretical models, I personally gained insights into the intricate nature of stars as they evolve and interact with their surroundings. For me, this project was a journey into the active process of scientific discovery and evolving nature of science.
Overall, this journey has been an enlightening part of my astronomical studies, showcasing the dynamic and ever-evolving universe (and scientific process) that continues to amaze me. The process has not only contributed to my academic growth but has also deeply enriched my personal appreciation for the field of astronomy.
I hope this post has enriched your understanding of the celestial bodies in our night sky.