Two Kepler red-giant eclipsing binaries as lower red-giant branch benchmarks for asteroseismic scaling relations. Dynamical masses and radii from JKTEBOP and PHOEBE-2 modeling
Abstract
Space-based photometry has detected solar-like oscillations in thousands of stars, whose global seismic parameters yield stellar properties via the asteroseismic scaling relations. Because these relations systematically overestimate red-giant masses and radii empirical calibration is required. Double-lined eclipsing binaries hosting oscillating red giants provide precise dynamical masses and radii without external calibration, making them ideal benchmarks. We present KIC 8129189 and KIC 10920813, two Kepler eclipsing binaries containing less-evolved oscillating red giants, as new benchmarks that extend the calibration sample toward smaller radii. We measured radial velocities from high-resolution spectra, extracted global asteroseismic parameters from Kepler light curves, and modeled the binaries with JKTEBOP and PHOEBE-2 using both full light curves and selected eclipse sets, adopting benchmark masses and radii from the envelope of tested model/data configurations. We then fit correction factors fΔν and fνmax to the underlying Δν-density and νmax-surface-gravity relations. We obtain MRG=1.413 ± 0.037 M⊙ and RRG=4.296 ± 0.061 R⊙ for KIC 8129189, and MRG=1.383 ± 0.022 M⊙ and RRG=5.914 ± 0.043 R⊙ for KIC 10920813. The adopted 15-star calibration gives fΔν=0.9777 ± 0.0048 and fνmax=1.024 ± 0.008, corresponding to CM=0.850 ± 0.020 and CR=0.9333 ± 0.0090. Neither correction factor depends significantly on radius, nor does fνmax depend on metallicity; model-based fΔν values are systematically lower than the dynamically derived ones. Both systems agree with the correction from previous benchmarks, showing that continued expansion of the eclipsing-binary sample is essential for testing the scaling relations across evolutionary stage.
Versions
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BibTeX
@misc{hedlund2026kepler,
title = {{Two Kepler red-giant eclipsing binaries as lower red-giant branch benchmarks for asteroseismic scaling relations. Dynamical masses and radii from JKTEBOP and PHOEBE-2 modeling}},
author = {A. Hedlund and P. Gaulme and J. Jackiewicz and T. Appourchaux and E. Guenther},
howpublished = {arXiv},
year = {2026},
month = sep,
doi = {10.48550/arxiv.2609.17737},
eprint = {2609.17737},
archivePrefix = {arXiv},
url = {https://arxiv.org/abs/2609.17737},
note = {CC BY 4.0},
}
RIS
TY - UNPB
TI - Two Kepler red-giant eclipsing binaries as lower red-giant branch benchmarks for asteroseismic scaling relations. Dynamical masses and radii from JKTEBOP and PHOEBE-2 modeling
AU - A. Hedlund
AU - P. Gaulme
AU - J. Jackiewicz
AU - T. Appourchaux
AU - E. Guenther
PY - 2026
DA - 2026/09/17
PB - arXiv
DO - 10.48550/arxiv.2609.17737
UR - https://arxiv.org/abs/2609.17737
AB - Space-based photometry has detected solar-like oscillations in thousands of stars, whose global seismic parameters yield stellar properties via the asteroseismic scaling relations. Because these relations systematically overestimate red-giant masses and radii empirical calibration is required. Double-lined eclipsing binaries hosting oscillating red giants provide precise dynamical masses and radii without external calibration, making them ideal benchmarks. We present KIC 8129189 and KIC 10920813, two Kepler eclipsing binaries containing less-evolved oscillating red giants, as new benchmarks that extend the calibration sample toward smaller radii. We measured radial velocities from high-resolution spectra, extracted global asteroseismic parameters from Kepler light curves, and modeled the binaries with JKTEBOP and PHOEBE-2 using both full light curves and selected eclipse sets, adopting benchmark masses and radii from the envelope of tested model/data configurations. We then fit correction factors f_Δν and f_ν_max to the underlying Δν-density and ν_max-surface-gravity relations. We obtain M_RG=1.413 ± 0.037 M_⊙ and R_RG=4.296 ± 0.061 R_⊙ for KIC 8129189, and M_RG=1.383 ± 0.022 M_⊙ and R_RG=5.914 ± 0.043 R_⊙ for KIC 10920813. The adopted 15-star calibration gives f_Δν=0.9777 ± 0.0048 and f_ν_max=1.024 ± 0.008, corresponding to C_M=0.850 ± 0.020 and C_R=0.9333 ± 0.0090. Neither correction factor depends significantly on radius, nor does f_ν_max depend on metallicity; model-based f_Δν values are systematically lower than the dynamically derived ones. Both systems agree with the correction from previous benchmarks, showing that continued expansion of the eclipsing-binary sample is essential for testing the scaling relations across evolutionary stage.
ER -