Physical and geometrical properties of an Algol type eclipsing binary with a δ Scuti pulsator: HD 221072

GÜROL B., ÖZDEMİR S., Gürsoytrak-Mutlay S. H., Terzioğlu Z.

New Astronomy, cilt.105, 2024 (SCI-Expanded) identifier

  • Yayın Türü: Makale / Tam Makale
  • Cilt numarası: 105
  • Basım Tarihi: 2024
  • Doi Numarası: 10.1016/j.newast.2023.102088
  • Dergi Adı: New Astronomy
  • Derginin Tarandığı İndeksler: Science Citation Index Expanded (SCI-EXPANDED), Scopus, Academic Search Premier, Aerospace Database, Communication Abstracts, INSPEC, Metadex, Civil Engineering Abstracts
  • Anahtar Kelimeler: Binaries, Eclipsing, Fundamental parameters technique, Individual (HD 221072), Photometry stars, Pulsation stars, Stars
  • Ankara Üniversitesi Adresli: Evet

Özet

In this study, we obtained physical and geometrical parameters of an Algol type eclipsing binary hosting a δ Scuti pulsator. Based on the Transiting Exoplanet Survey Satellite (TESS) observations of HD 221072 system published in Sectors 24, 57, and 58, we obtained the photometric solution of the eclipsing binary. The light curve modelling reveals that it is a detached system with masses and radii of the primary and secondary components as M1=1.772±0.003M⊙, M2=1.753±0.003M⊙ and R1=4.157±0.002R⊙, R2=2.369±0.002R⊙, respectively. After removing of the binary model from the TESS data, frequency analysis is applied to the light residuals. The Fourier spectrum shows that it can be divided in two sectors. One of them is located below the f<6d−1 limit and it is purely related with the orbital frequency. Because of the locations of the components on the Hertzsprung–Russell diagram there is a possibility of the secondary component pulsating too. According to the Q pulsation constant obtained for primary and secondary component, we can say that the primary component pulsating with the frequencies larger than f>6d−1 and it is the δ Scuti pulsator in the eclipsing system.