Speaker
Mr
Ronnakrit Rattanamala
(PhD Program in Astronomy, Department of Physics and Materials Science, Faculty of Science, Chiang Mai University, Chiang Mai, 50200, Thailand)
Description
ABSTRACT
The study of the period change of V619 Peg was conducted. V619 Peg is an A-subtype of W UMa contact binary. The data was monitored with the 0.7m telescope at NARIT’s Spring Brook Observatory, Australia, in 2019-2020. The time of minima were used to compute the O-C diagram in order to find the system orbital period change and the third body. The results show that the system has an increasing in its orbital period. The O-C residual has a sinusoidal trend which might be caused by the third body component. The third body is a red dwarf with mass 0.16-0.20 Solar mass and period about 10-12 years.
Keywords: binaries: close — binaries: eclipsing — stars: individual (V619 Peg)
Primary authors
Mr
Ronnakrit Rattanamala
(PhD Program in Astronomy, Department of Physics and Materials Science, Faculty of Science, Chiang Mai University, Chiang Mai, 50200, Thailand)
Dr
Siramas Komonjinda
(Department of Physics and Materials Science, Faculty of Science, Chiang Mai University, Chiang Mai, 50200, Thailand )
Dr
Supachai Awiphan
(National Astronomical Research Institute of Thailand (Public Organization), 260 Moo 4, Donkaew, Mae Rim, Chiang Mai, 50180, Thailand )
Ms
Pranita Sappankum
(PhD Program in Astronomy, Department of Physics and Materials Science, Faculty of Science, Chiang Mai University, Chiang Mai, 50200, Thailand)
Dr
Anirut Phriksee
(National Astronomical Research Institute of Thailand (Public Organization), 260 Moo 4, Donkaew, Mae Rim, Chiang Mai, 50180, Thailand )
