Abstract
Many available published times of light minima of the late-type binary system ER Vul have been compiled and analyzed using a new method proposed by Kalimeris et al. (1994). It was shown that the orbital period of the system oscillation with a period of about 30.6 years and an amplitude of 3.2×10-6 days while it undergoes a constant period decrease of about dP /P=7.84× 10-8 day / year. The prospective physical mechanisms that could have modulated the orbital period behaviour (periodic or non-periodic), have been studied. We found that a combination of a magnetic activity cycle mechanism and an enhanced stellar wind could explain satisfactorily the period change.
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Shengbang, Q., Qingyao, L. & Yulan, Y. A Period Study of the Rs CVn-Type Binary ER Vulpeculae. Astrophysics and Space Science 257, 1–10 (1997). https://doi.org/10.1023/A:1000448104322
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DOI: https://doi.org/10.1023/A:1000448104322