Asteroseismic analysis of 15 solar-like oscillating evolved stars

ÇELİK ORHAN Z., Yildiz M., Kayhan C.

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY, vol.503, no.3, pp.4529-4536, 2021 (SCI-Expanded) identifier identifier identifier

  • Publication Type: Article / Article
  • Volume: 503 Issue: 3
  • Publication Date: 2021
  • Doi Number: 10.1093/mnras/stab757
  • Journal Indexes: Science Citation Index Expanded (SCI-EXPANDED), Scopus, Academic Search Premier, Aerospace Database, Applied Science & Technology Source, Communication Abstracts, INSPEC, Metadex, zbMATH, DIALNET, Civil Engineering Abstracts
  • Page Numbers: pp.4529-4536
  • Keywords: stars: evolution, stars: fundamental parameters, stars: interiors, stars: oscillations, MINIMUM DELTA-NU, FUNDAMENTAL PROPERTIES, MODEL COMPUTATIONS, SCALING RELATION, KEPLER, FREQUENCIES, TARGETS, CORE
  • Erciyes University Affiliated: Yes


Asteroseismology using space-based telescopes is vital to our understanding of stellar structure and evolution. CoRoT, Kepler, and TESS space telescopes have detected large numbers of solar-like oscillating evolved stars. Solar-like oscillation frequencies have an important role in the determination of fundamental stellar parameters; in the literature, the relations between the two is established by the so-called scaling relations. In this study, we analyse data obtained from the observation of 15 evolved solar-like oscillating stars using the Kepler and ground-based telescopes. The main purpose of the study is to determine very precisely the fundamental parameters of evolved stars by constructing interior models using asteroseismic parameters. We also fit the reference frequencies of models to the observational reference frequencies caused by the Heii ionization zone. The 15 evolved stars are found to have masses and radii within ranges of 0.79-1.47 M-circle dot and 1.60-3.15 R-circle dot, respectively. Their model ages range from 2.19 to 12.75 Gyr. It is revealed that fitting reference frequencies typically increase the accuracy of asteroseismic radius, mass, and age. The typical uncertainties of mass and radius are similar to 3-6 and similar to 1-2 percent, respectively. Accordingly, the differences between the model and literature ages are generally only a few Gyr.