Pulsations in massive and intermediate-mass binaries of interest
- 1Faculty of Science, Department of Astronomy and Space Sciences, Ege University , 35100 Bornova, İzmir ,
Abstract
We present a comprehensive observational study of seven eclipsing binaries composed of massive and intermediate-mass components. Combining ground-based spectroscopy and space photometry of target stars, we compute precise physical parameters of these systems and investigate pulsational properties of the components. Our findings indicate that primary components of all target systems are slowly pulsating B-type (SPB) stars, while one of the systems includes a secondary component exhibiting δ Sct-type pulsations. Positions of the SPB components in the Hertzsprung–Russell diagram show a wide range in the effective temperature, while some of them are located beyond the hot edge of the instability strip of SPB stars. It appears that discovering a larger number of massive and intermediate-mass eclipsing binaries is required to clarify a definite instability strip for SPB stars. This also raises another question: Is an instability domain essential for SPBs?
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BibTeX
@article{hoyman2026pulsations,
title = {{Pulsations in massive and intermediate-mass binaries of interest}},
author = {B Hoyman and Ö Çakırlı and O Özdarcan},
journal = {Monthly Notices of the Royal Astronomical Society},
year = {2026},
month = oct,
doi = {10.1093/mnras/stag1923},
url = {https://academic.oup.com/mnras/article/doi/10.1093/mnras/stag1923/8898892},
note = {CC BY 4.0},
}
RIS
TY - JOUR
TI - Pulsations in massive and intermediate-mass binaries of interest
AU - B Hoyman
AU - Ö Çakırlı
AU - O Özdarcan
PY - 2026
DA - 2026/10/09
JO - Monthly Notices of the Royal Astronomical Society
DO - 10.1093/mnras/stag1923
UR - https://academic.oup.com/mnras/article/doi/10.1093/mnras/stag1923/8898892
AB - We present a comprehensive observational study of seven eclipsing binaries composed of massive and intermediate-mass components. Combining ground-based spectroscopy and space photometry of target stars, we compute precise physical parameters of these systems and investigate pulsational properties of the components. Our findings indicate that primary components of all target systems are slowly pulsating B-type (SPB) stars, while one of the systems includes a secondary component exhibiting δ Sct-type pulsations. Positions of the SPB components in the Hertzsprung–Russell diagram show a wide range in the effective temperature, while some of them are located beyond the hot edge of the instability strip of SPB stars. It appears that discovering a larger number of massive and intermediate-mass eclipsing binaries is required to clarify a definite instability strip for SPB stars. This also raises another question: Is an instability domain essential for SPBs?
SN - 0035-8711
SN - 1365-2966
ER -