The Relation between Stellar Pulsation and Emission Line Profiles of HD 144470 Muthia Dewi (a), Aprilia (b*), Irfan Imaduddin (a)
a) Astronomy Study Program, Faculty of Mathematics and Natural Sciences, Institut Teknologi Bandung, Jl. Ganesa 10, Bandung, 40132, Indonesia
b) Astronomy Research Division and Bosscha Observatory, Faculty of Mathematics and Natural Sciences, Institut Teknologi Bandung, Jl. Ganesa 10, Bandung, 40132, Indonesia
*aprilia[at]as.itb.ac.id
Abstract
In this work, we analyse star HD144470 (\(\omega^{1} sco\)), which is a pulsating star that shows emission lines in its spectrum, using photometric and spectroscopic data. The emission line profiles appear at \(\lambda\) 6,506.2 Angstrom (Ce II-line) and \(\lambda\) 6,718.0 Angstrom (Ca I-line). We observe these spectra at Bosscha Observatory, Indonesia, in 2019 and 2020. We use Lomb Scargle Periodogram method to calculate the variability periods in photometric data (9.11-day- 6.65-day and 7.11-day period). Then, we validate it with the appearance of emission lines on the June 29th, 2020 spectrum of the entire spectra. Only the 9.11-day period is proved valid across the spectra. It answers the relation between the period of variability in photometric data and the appearance of the emission line profile of Ce II and Ca I, namely a period of 9.11 days.
Keywords: Pulsation- Emission Line- Period- Oscillation in Stars- Variability
