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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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.