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The mass of a star is one of its most important properties, and it is nearly impossible to directly measure. The stellar mass is used to determine a stars size, brightness, color, and lifespan. Detached, double-lined eclipsing binaries are the main source of accurate data on stellar masses and radii and provide, together with pulsating stars, detailed information on structure and evolution of normal stars. An eclipsing binary is a set of two stars who have fluctuating brightnesses due to each star passing in front of one another. They give scientists a unique way to determine the mass of the stars by inferring masses through gravitational interactions. Our goal is to find masses, radii, and surface temperatures for selected eclipsing binaries. We used the 16-in Cassegrain telescope at the North Georgia Astronomical Observatory to obtain time-series photometric images and time-series spectra of three eclipsing binary systems (41 Ari, TY-Peg, WZ-Peg) over a 3 month time period. Here, we present our time-series data and estimates of the stellar masses and radii for 41 Ari. Although preliminary, our results will ultimately provide key constraints on the accuracy of stellar structure theory and help pave the way for future eclipsing binary studies at the University of North Georgia.


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  • Subject
    • Physics & Astronomy

  • Institution
    • Dahlonega

  • Event location
    • Nesbitt 3110

  • Event date
    • 23 March 2018

  • Date submitted

    19 July 2022

  • Additional information
    • Acknowledgements:

      Dr. Gregory Feiden