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PreprintCC BY 4.0arXiv

First and Comprehensive Study of V0757 Pup : γ−Doradus Pulsator in Detached Eclipsing Binary

  • Bakuh Danang Setyo Budi
  • Bryant Randolph
  • Rafa Nanda Akilah
  • Evan Irawan Akbar
  • Hakim Luthfi Malasan
  • Puji Irawati
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Abstract

Pulsating stars in detached eclipsing binary (EA) systems are known for providing many important physical informations which constrain both stellar structure and evolution theories. To date, fewer than 50 γ Doradus (GDOR) stars have been found in eclipsing binary systems, making them important targets to study \textit{g}-mode pulsation inside the stars. We present a comprehensive physical and pulsational analysis of V0757 Pup (TIC 6939791), a detached eclipsing binary system observed by the TESS mission (Sectors 7, 34, 61, and 88) and followed up with ground-based spectroscopy from the Thai National Telescope. By combining light curve modeling with radial velocities derived from medium-resolution spectra, we determined the fundamental stellar and atmospheric parameters with high precision. The system consists of an F2V primary (M1=1.305±0.026M⊙, R1=1.643±0.020R⊙) and a G1V secondary (M2=0.934±0.030M⊙, R2=0.941±0.079R⊙). We performed a detailed frequency analysis of the residual light curves, identifying two dominant independent pulsation frequencies at f∼0.79 c/d and $0.98$ c/d. These frequencies, along with the derived pulsation constant (Q∼0.6 d), confirm the primary component as a γ Doradus pulsator. An analysis of Eclipse Timing Variations (ETV) reveals non detection of third body companions with current available dataset, strengthen by the result of \textit{Gaia} astrometric analysis. Evolutionary modeling indicates the system is ∼2.2 Gyr old, with the primary expected to fill its Roche lobe in ∼1 Gyr. Additionally, we calculate a distance of d≈350 pc based on orbital and SED modeling, which is in excellent agreement with the \textit{Gaia} DR3 parallax distance.

Versions

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Cite

BibTeXRIS
BibTeX
@misc{budi2026first,
  title = {{First and Comprehensive Study of V0757 Pup : $γ-$Doradus Pulsator in Detached Eclipsing Binary}},
  author = {Bakuh Danang Setyo Budi and Bryant Randolph and Rafa Nanda Akilah and Evan Irawan Akbar and Hakim Luthfi Malasan and Puji Irawati},
  howpublished = {arXiv},
  year = {2026},
  month = aug,
  doi = {10.48550/arxiv.2608.11896},
  eprint = {2608.11896},
  archivePrefix = {arXiv},
  url = {https://arxiv.org/abs/2608.11896},
  note = {CC BY 4.0},
}
RIS
TY  - UNPB
TI  - First and Comprehensive Study of V0757 Pup : γ−Doradus Pulsator in Detached Eclipsing Binary
AU  - Bakuh Danang Setyo Budi
AU  - Bryant Randolph
AU  - Rafa Nanda Akilah
AU  - Evan Irawan Akbar
AU  - Hakim Luthfi Malasan
AU  - Puji Irawati
PY  - 2026
DA  - 2026/08/12
PB  - arXiv
DO  - 10.48550/arxiv.2608.11896
UR  - https://arxiv.org/abs/2608.11896
AB  - Pulsating stars in detached eclipsing binary (EA) systems are known for providing many important physical informations which constrain both stellar structure and evolution theories. To date, fewer than 50 γ Doradus (GDOR) stars have been found in eclipsing binary systems, making them important targets to study \textit{g}-mode pulsation inside the stars. We present a comprehensive physical and pulsational analysis of V0757 Pup (TIC 6939791), a detached eclipsing binary system observed by the TESS mission (Sectors 7, 34, 61, and 88) and followed up with ground-based spectroscopy from the Thai National Telescope. By combining light curve modeling with radial velocities derived from medium-resolution spectra, we determined the fundamental stellar and atmospheric parameters with high precision. The system consists of an F2V primary (M_1=1.305±0.026M_⊙, R_1=1.643±0.020R_⊙) and a G1V secondary (M_2=0.934±0.030M_⊙, R_2=0.941±0.079R_⊙). We performed a detailed frequency analysis of the residual light curves, identifying two dominant independent pulsation frequencies at f∼0.79 c/d and $0.98$ c/d. These frequencies, along with the derived pulsation constant (Q∼0.6 d), confirm the primary component as a γ Doradus pulsator. An analysis of Eclipse Timing Variations (ETV) reveals non detection of third body companions with current available dataset, strengthen by the result of \textit{Gaia} astrometric analysis. Evolutionary modeling indicates the system is ∼2.2 Gyr old, with the primary expected to fill its Roche lobe in ∼1 Gyr. Additionally, we calculate a distance of d≈350 pc based on orbital and SED modeling, which is in excellent agreement with the \textit{Gaia} DR3 parallax distance.
ER  -