Abstract
Thanks to the precision of Kepler observations, [3] were able to measure the linewidth and amplitude of individual modes (including mixed modes) in several subgiant power spectra. We perform a forward modelling of a Kepler subgiant based on surface properties and observed frequencies. Non-adiabatic computations including a time- dependent treatment of convection give the lifetimes of radial and non-radial modes. Next, combining the lifetimes and inertias with a stochastic excitation model gives the amplitudes of the modes. We can now directly compare theoretical and observed linewidths and amplitudes of mixed-modes to obtain new constraints on our theoretical models.
Highlights
Thanks to the precision of Kepler observations, [3] were able to measure the linewidth and amplitude of individual modes in several subgiant power spectra
The theoretical amplitudes ratios for p-dominated modes mainly depends on the visibilities of the modes and the error bars are too large to provide additional constraints on the models that could comes from the ratios with g-dominated mixed-modes
The remaining discrepancies may comes from missing physics in the structure model such as the turbulent pressure
Summary
Thanks to the precision of Kepler observations, [3] were able to measure the linewidth and amplitude of individual modes (including mixed modes) in several subgiant power spectra. Equilibrium model: We used the frequencies obtained by [3] (obtained from Quarters 5 to 7 of Kepler data) as well as the spectroscopic constraint from [8] to search the structure model of KIC 6442183. The models are computed with the CESTAM evolutionary code [7] using a LevenbergMarquardt algoritm (OSM) to search for the model parameters that reproduce the spectroscopic and seismic constraints. We fit the spectroscopic constraints and low frequencies modes.
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