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- W2006355918 abstract "Combining with our newest CCD times of light minimum of EM Cygni, all 45 available times of light minimum, including 7 data with large scatters, were compiled and an updated |$O-C$| analysis was made. The best-fit for the |$O-C$| diagram of EM Cygni was a quadratic-plus-sinusoidal fit. The secular orbital period decrease rate (|$-$|2.5 |$pm$| 0.3) |$times$| 10|$^{-11} $|s s|$^{-1}$| means that a magnetic braking effect in EM Cygni with a mass-loss rate caused by stellar wind, 2.3 |$times$| 10|$^{-10} M_{odot} $|yr|$^{-1}$|, is needed for explaining the observed orbital period decrease. Moreover, for explaining the significant cyclical period change with a period of |$sim $|17.74 |$pm$| 0.01 yr, shown in the |$O-C$| diagram, magnetic activity cycles and a light travel-time effect were considered in detail. The |$O-C$| diagram of EM Cygni cannot totally rule out the possibility of multi-periodic modulation due to gaps present after 25000 cycles. Based on the hypothesis of a K-type third star in the literature, a light trave-time effect may be a more plausible explanation. However, the low orbital inclination of the third body (|$sim $|7|$^circ!!!.$|4) suggests that the hypothetic K-type third star may be captured by EM Cygni. But, by assuming the spectral contamination from a block of circumbinary material instead of a K-type third star, the third star may be a brown dwarf in the case of a coplanar orbit with a parent binary." @default.
- W2006355918 created "2016-06-24" @default.
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- W2006355918 date "2010-08-25" @default.
- W2006355918 modified "2023-10-10" @default.
- W2006355918 title "Orbital Period Analysis of Eclipsing Z Cam-Type Dwarf Nova EM Cygni: Evidence of Magnetic Braking and a Third Body" @default.
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- W2006355918 doi "https://doi.org/10.1093/pasj/62.4.965" @default.
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