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Analysis reveals decreasing orbital period in the eclipsing binary star V392 Orionis, suggesting significant changes in its light curve.
This study investigates the period change of the eclipsing binary system V392 Orionis (V392 Ori), which is classified as an Algol-type binary star. The research utilized data from the TESS Eclipsing Binary Catalog obtained via the Transiting Exoplanet Survey Satellite (TESS). Light curves were generated through photometric analysis to determine the times of minimum light. The historical and current observational data were used to construct the O–C diagram. The O–C diagram derived from PE and CCD observations exhibits a downward parabolic trend, indicating a decreasing orbital period at a rate of 5.76×10-3 seconds per year.
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Maithong et al. (2025) studied this question.
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