Asteroseismic analysis of the merger product red giant in the γ Persei system
Year: 2026
Type: article
Abstract: γ Persei (γ Per) is a long-period eclipsing binary system (P≈ 14.6 years) containing a red-giant primary, and it is well known for its multi-faceted classification as a visual and spectroscopic binary. Its brightness and binary nature together make it a valuable target for both photometric and spectroscopic studies, particularly in the context of asteroseismology and stellar evolution, as the primary star likely formed through a stellar merger. We determined the seismic parameters ν_̊m max and Δ ν, and the oscillation amplitudes of the primary component, an evolved giant, to estimate its seismic mass, which we compared to its estimated dynamic mass. We used Transiting Exoplanet Survey Satellite data obtained during Sectors 58, 85, and 86. To complement the space-based observations, we incorporated high-resolution radial velocity measurements acquired by the Stellar Observations Network Group during two distinct epochs, 2017 and 2024. We successfully detect solar-like oscillations in γ Per and infer a seismic mass of 3.25 M_⊙, which is slightly below the dynamical mass. We find the photometric oscillation amplitudes to be significantly lower than predicted from scaling relations, but in line with other high-mass red giants. We also find that radial-velocity amplitudes along the Hertzsprung-Russell diagram cannot be fitted uniformly with current scaling relations.
Source: Astronomy and Astrophysics
Language: English
Subfield: Astronomy and Astrophysics
Field: Physics and Astronomy
Domain: Physical Sciences
Open Access status: gold
Estimated APC paid: $1,865
Funder: Magyar Tudományos Akadémia
OpenAlex ID: W7167235434