Orbital Period Change of the Binary Star System V829 Aql

Article Sidebar

PDF
Published: Mar 24, 2026
DOI: https://doi.org/10.55164/ajstr.v29i4.258435
Keywords:
V829 Aql orbital period change TRO

Main Article Content

Supat Sairattanain
Faculty of Education and Human Development, Sisaket Rajabhat University, Sisaket, 33000, Thailand
Torik Hengpiya
National Astronomical Research Institute of Thailand (Public Organization), Songkhla, 90000, Thailand
Wiraporn Maithong
Faculty of Science and Technology, Chiang Mai Rajabhat University, Chiang Mai, 50300, Thailand

Abstract

A variable star, V829 Aql, is considered one of the binary stars providing invaluable insights into the process of stellar evolution. The purpose of this research study is to calculate the orbital period change of the binary star system V829 Aql using a telescope at the Regional Observatory for the Public, Songkhla, National Astronomical Research Institute of Thailand (Public Organization). Images in the B and V wavelength range will be taken on the night of July 1-2, 2021, from 9:00 p.m. to 5:00 a.m., and subsequently examined. It was discovered that the brightness value pattern adhered to an equation (relationship): the orbital period equals the lowest brightness when it does. The orbital period change is growing, as indicated by the equation O-C = (4.82878 Í 10-13) Epoch2 - (1.5221 Í 10-7) Epoch – 0.01052, which gives a rate of change in orbital period of 1.05 x 10-4 seconds/year. This means that stars continue to separate, which explains the evolution of the TRO theory.

Article Details

Issue
Vol. 29 No. 4 (2026): April
Section
Research Articles
Creative Commons License

This work is licensed under a Creative Commons Attribution-NonCommercial-NoDerivatives 4.0 International License.

References

Diethelm, R. V829 Aquilae is a Pulsating Star with a Variable Light Curve. Commissions 27 and 42 of the IAU Information Bulletin on Variable Stars. 1997, 4530, 1-2.

Diethelm, R. V829 Aquilae Is a Pulsating Star with a Variable Light Curve. Inf. Bull. Var. Stars 1997, 4530, 1–2.

Handler, G.; Pikall, H.; Diethelm, R. The Nature of A829 Aql: A Triple-Mode Radially Pulsating Post-Main-Sequence Delta Scuti Star. Inf. Bull. Var. Stars 1998, 4549, 1–4.

Prša, A. Modeling and Analysis of Eclipsing Binary Stars: The Theory and Design Principles of PHOEBE; IOP Publishing, 2018. https://doi.org/10.1088/978-0-7503-1287-5

SIMBAD Astronomical Database—CDS (Strasbourg). http://simbad.u-strasbg.fr/simbad/ (accessed 2022-10-22).

American Association of Variable Star Observers (AAVSO). Bob Nelson’s Database of Eclipsing Binary O–C Files. https://www.aavso.org/bob-nelsons-o-c-files (accessed 2022-10-22).

Lucy, L. B.; Wilson, R. E. Observational Tests of Theories of Contact Binaries. Astrophys. J. 1979, 231, 502–513. https://doi.org/10.1086/157212

Rahunen, T. The Evolution of Contact Binaries: A New Approach. Astron. Astrophys. 1981, 97(2), 406–409.

Qian, S. Orbital Period Changes of Contact Binary Systems: Direct Evidence for Thermal Relaxation Oscillation Theory. Mon. Not. R. Astron. Soc. 2001, 328, 914–924. https://doi.org/10.1046/j.1365-8711.2001.04921.x

Diffraction Limited. MaxIm DL Software. https://diffractionlimited.com/maxim-dl/ (accessed 2022-10-22).

Romanishin, W. An Introduction to Astronomical Photometry Using CCDs; University of Oklahoma, 2002.

Pancharoen, W.; Maithong, W. The First Study of a Period Change of the V1851 Orion Eclipsing Binary System. ASEAN J. Sci. Technol. Rep. 2021, 24(3), 9–14. https://doi.org/10.55164/ajstr.v24i3.243575