How many magnetic red giants can we detect from asymmetries in mixed modes in the Kepler sample?
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Establishing whether or not stellar cores are magnetized is critical for understanding their evolution through the large impact magnetism has on angular momentum transport. Asteroseismology provides a means of doing so by analyzing the symmetry in the frequencies of rotationally split mixed-mode multiplets in a given red giant’s power spectrum. But to use this method, each component of the l=1 mixed mode multiplets must be visible. A mode’s visibility is compromised when its amplitude is so low that it is indistinguishable from noise, or when the frequencies of the various azimuthal orders are so similar that they cannot be identified as a multiplet. Each scenario can occur due to various stellar properties. So far, 23 magnetized red giant cores have been identified in the Kepler sample by these means of analysis. However, it is unknown how many stars went undetected due to a lack of mode visibility. The goal of our work is to calculate the proportion of magnetized red giants on which we can measure dipolar mixed mode asymmetries, and thus evaluate if only identifying 23 is expected. We started by modeling a red giant with MESA and computed its frequencies with GYRE. Next, magsplitpy developed by Das et al. (2020) and Das et al. (2024) was used to calculate the relative amplitudes of the three dipole split modes for a grid of varying inclination, orientation of a dipole magnetic field, rotation rate, and magnetic field strength. A realistic noise level was then set to establish what combinations of these properties result in all the modes being visible. Finally, we apply analytic and/or observational distributions of each parameter to calculate the probability that a red giant has one of these desired combinations of properties. This allows us to conclude how many red giants in the Kepler sample should have visible split magnetic mixed modes and thus could be used to study core magnetism.
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JadenFitzpatrick_TASC9KASC16Poster_20250625_v2.pdf
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