Logo
ScienceStack
Table of Contents
Fetching ...
Sign In

Characterizing the variability of a sample of massive stars in eclipsing binaries

C. I. Eze, G. Handler, F. Kahraman Aliçavuş, T. Pawar, A. Miszuda

TL;DR

This study tackles the persistent mass-discrepancy problem in massive stars by combining the strengths of asteroseismology and eclipsing-binary analysis. Using a sample of beta Cephei pulsators in eclipsing binaries observed with TESS and multiple spectrographs, it derives orbital elements, atmospheric parameters, and preliminary pulsation properties, providing a foundation for future detailed modeling. The work demonstrates how rotationally split modes and ensemble pulsational characteristics can constrain internal rotation and core mixing, while identifying amplitudes and frequencies linked to pulsation behavior in binary environments. By delivering comprehensive characterization and priors for theoretical modeling, the paper advances the calibration of convective boundary mixing and the interpretation of mass estimates in massive stars.

Abstract

Massive stars exhibit a perplexing mismatch between their inferred masses from different observational techniques, posing a significant challenge to our understanding of stellar evolution and structure. This discrepancy is believed to be caused by the underestimation of the convective core masses. The efficiency of such measurement is usually impaired by a lot of processes at work in the interior of the stars such as convective core overshooting and interior rotation. By integrating the precision of asteroseismology which provides insights into the internal structure and dynamics of stars, with the detailed observational constraints offered by eclipsing binary systems, this study aims to precisely characterize a sample of massive stars in eclipsing binaries to infer their properties and evolutionary state. In this paper, the sample, observed photometrically with TESS and spectroscopically with SALT HRS, CHIRON, HERMES and a spectrograph at Skalnate Pleso Observatory between 2021 and 2024, are analyzed. The orbital elements as well as the basic stellar parameters of the targets in the sample are fitted to derive the geometry of their orbits as well as their absolute parameters. The asteroseismic properties of the targets are also obtained, which unravel their core dynamics and profiles. This is a precursor work that provides detailed characterization of the targets in the sample for future theoretical modeling.

Characterizing the variability of a sample of massive stars in eclipsing binaries

TL;DR

This study tackles the persistent mass-discrepancy problem in massive stars by combining the strengths of asteroseismology and eclipsing-binary analysis. Using a sample of beta Cephei pulsators in eclipsing binaries observed with TESS and multiple spectrographs, it derives orbital elements, atmospheric parameters, and preliminary pulsation properties, providing a foundation for future detailed modeling. The work demonstrates how rotationally split modes and ensemble pulsational characteristics can constrain internal rotation and core mixing, while identifying amplitudes and frequencies linked to pulsation behavior in binary environments. By delivering comprehensive characterization and priors for theoretical modeling, the paper advances the calibration of convective boundary mixing and the interpretation of mass estimates in massive stars.

Abstract

Massive stars exhibit a perplexing mismatch between their inferred masses from different observational techniques, posing a significant challenge to our understanding of stellar evolution and structure. This discrepancy is believed to be caused by the underestimation of the convective core masses. The efficiency of such measurement is usually impaired by a lot of processes at work in the interior of the stars such as convective core overshooting and interior rotation. By integrating the precision of asteroseismology which provides insights into the internal structure and dynamics of stars, with the detailed observational constraints offered by eclipsing binary systems, this study aims to precisely characterize a sample of massive stars in eclipsing binaries to infer their properties and evolutionary state. In this paper, the sample, observed photometrically with TESS and spectroscopically with SALT HRS, CHIRON, HERMES and a spectrograph at Skalnate Pleso Observatory between 2021 and 2024, are analyzed. The orbital elements as well as the basic stellar parameters of the targets in the sample are fitted to derive the geometry of their orbits as well as their absolute parameters. The asteroseismic properties of the targets are also obtained, which unravel their core dynamics and profiles. This is a precursor work that provides detailed characterization of the targets in the sample for future theoretical modeling.

Paper Structure

This paper contains 5 sections, 3 figures, 2 tables.

Table of Contents

  1. Introduction
  2. Spectroscopic Analysis
  3. Pulsation Analysis
  4. Ensemble Pulsational Characteristics
  5. Conclusion

Figures (3)

  • Figure 1: The fit to the RV curve of V1166 Cen.
  • Figure 2: Fourier spectra of V1166 Cen with the neighborhood of the dominant pulsation zoomed into (left panel) and échelle diagram of V1166 Cen (right panel).
  • Figure 3: Frequency-amplitude relation for $\beta$ Cep p modes (left panel) and Period-pulsation amplitude relation for our sample of $\beta$ Cep pulsators in eclipsing binaries (right panel).