Mass transfer and tidally tilted pulsation in the Algol-type system TZ Dra

Kahraman Aliçavuş F., Handler G., Aliçavuş F., De Cat P., Bedding T. R., Lampens P., ...More

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY, vol.510, no.1, pp.1413-1424, 2022 (SCI-Expanded) identifier

  • Publication Type: Article / Article
  • Volume: 510 Issue: 1
  • Publication Date: 2022
  • Doi Number: 10.1093/mnras/stab3515
  • 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.1413-1424
  • Keywords: stars: atmospheres, binaries: eclipsing, stars: fundamental parameters, stars: individual: TZ Dra, stars: variables: delta Scuti, CLOSE BINARY-SYSTEMS, DELTA-SCUTI STARS, ECLIPSING BINARY, PHYSICAL PARAMETERS, COMPONENTS, LIGHT, CATALOG, PERIOD, SCT
  • Çanakkale Onsekiz Mart University Affiliated: Yes


Oscillating eclipsing Algols (oEAs) are remarkable systems that allow us to determine accurate fundamental stellar parameters (mass, radius) and probe the stellar interiors through pulsations. TZDra is an oEA system containing a delta Scuti component. To examine particular characteristics of such close systems including pulsations and mass transfer, we present a detailed photometric and spectroscopic study of TZDra. With the analysis of high-resolution spectra, the orbital parameters were determined by the radial velocity analysis and the atmospheric parameters were derived for the primary component. The binary modelling and the pulsational frequency analysis was carried out using the Transiting Exoplanet Survey Satellite data set. The H alpha line profiles show the signature of mass transfer from the cool to the hot binary component. The conclusion of mass transfer/mass-loss in the system was supported by the analysis of the orbital period changes. As a result, it was found that there is 3.52 x 10(-9) M-circle dot yr(-1) mass-loss from the system most probably through the hotspot and stellar winds. Additionally, most pulsation frequencies originating from the primary component were found to be spaced by harmonics of the orbital frequencies in particular, 12 doublets spaced by 2f(orb) were detected from which we infer that this star is a tidally tilted pulsator. A mean p-mode frequency spacing of approximate to 7.2 d(-1) was found as well.