Buoyancy glitches in the Brunt-Väisälä frequency and evanescent zone contribute to the g-mode phase in red-giant stars beyond the usual ε_g reflection term, prompting a modified formula and new quantification formalism.
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FICO procedure yields average precisions of 2.3% mass, 0.82% radius, 6.9% age and 0.49% mean density for 95 solar-like stars, outperforming direct frequency fitting for stars above 1.15 solar masses or 6050 K.
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Facing the phase: Gravity-mode offset and buoyancy glitches in red--giant branch stars
Buoyancy glitches in the Brunt-Väisälä frequency and evanescent zone contribute to the g-mode phase in red-giant stars beyond the usual ε_g reflection term, prompting a modified formula and new quantification formalism.
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Asteroseismic modelling of main-sequence solar-like stars and Kepler exoplanet host stars with the FICO procedure I. Catalogue of fundamental stellar properties
FICO procedure yields average precisions of 2.3% mass, 0.82% radius, 6.9% age and 0.49% mean density for 95 solar-like stars, outperforming direct frequency fitting for stars above 1.15 solar masses or 6050 K.