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1. Heidelberger Institut für Theoretische Studien, Heidelberg, Germany 2. Zentrum für Astronomie (ZAH/LSW), Heidelberg, Germany [email protected]g Jonas Müller1, 2, Quentin Coppée1, 2, Francisca Espinoza-Rojas1, 2, Saskia Hekker1, 2 (variables) ●We have developed a formalism to calculate asymptotic properties of damped mixed modes (based on Takata 2016b). ●This can be used to generate synthetic power spectra of stellar models. Visibilities of damped mixed modes Visibilities are amplitude ratios weighted by a geometrical factor that depends on the observation methods and the spherical degree : Damping processes operating in the stellar core decrease the multipole mode visibility. ●In observations, visibilities are estimated by integrating segments of the PSD (see shaded regions above). ➢This can lead to observational biases. ●We apply the observational methods to our synthetic PSDs to allow a meaningful comparison of theoretical and observed visibilities. D “Normal” mixed modes Depressed mixed modes Depressed mixed modes Fully suppressed modes Not mixed Core damping can explain the range of observed dipole mode visibilities. The geometrical factor is , in agreement with predictions from Ballot et al. (2011). No core damping Stronger core damping CBA A B C D Dipole mode visibility Observed visibilities are susceptible to stochastic scattering. Theoretical estimates for a 1.5 model. Different masses yield slightly different results. Observed visibilities from Stello et al. (2016a,b). Theoretical predictions have to be compared to averages. Shaded regions correspond to different radial mode linewidths. Magnetic damping in the stellar core according to Müller et al. (2025). Initial main-sequence field strengths range from 1 kG to 100 kG (see colors below).
