Exploring internal magnetism in partially suppressed red giant stars

The internal dynamical properties of red giant stars have been explored extensively in recent years as a result of the increase in high precision data availability from the space missions Kepler and TESS (Transiting Exoplanet Survey Satellite), and in this exploration, it has been discovered that some of these stars are not behaving as expected. Red giants are stars that have evolved off of the main sequence after having completed fusing hydrogen into helium in their core. Observational data shows that the cores are rotating significantly slower than models can recreate consistently across evolutionary stages. This discrepancy has prompted investigation into the efficiency of angular momentum transport mechanisms and mixing processes including meridional circulation, shear instability, internal gravity waves, Tayler-Spruit dynamo, fossil magnetic fields etc., to explain this behavior. Analyzing seismic oscillations in stars, via asteroseismology, is a powerful tool as it is the only way in which the deep stellar interior can be probed and subsequently characterized; this is possible as global oscillations modulating the stellar surface are effected by internal processes. For red giants, p-modes (pressure modes; resonating through the entire star) and g-modes (gravity-modes; resonating in the radiative interior) couple to create mixed modes. These mixed modes give access to the otherwise hidden stellar interior as g-modes couple to p-modes, delivering information from the interior to the surface. Internal magnetic signatures have been observationally confirmed in red giant stars via asteroseismology and characterized in two ways. One being that dipole mixed modes with ℓ = 1 will display a global asymmetric frequency shift of its azimuthal components; where the m = 0 and m = ±1 components of the ℓ = 1 dipole mode will be shifted by two different power laws, respectively. And the other being a reduced visibility of dipole mixed mode amplitudes in the power spectra, where stars presenting with this feature are denoted as suppressed. Several studies of the suppressed dipole mixed mode amplitudes have been carried out, but thus far, no dedicated studies of the asymmetric frequency shifts of suppressed red giants have been conducted; one reason being that the asymmetric frequency shifts cannot be characterized when the dipole mixed mode amplitudes are severely reduced in many of the suppressed stars. Sincefullysuppressedstarsdonothavedetectablemixed-modestoevaluate, partiallysuppressed stars, that is, red giant stars presenting with suppressed dipole mixed modes in select parts of their power spectra rather than across the entire spectra, will be the subject of this study as the respective mode amplitudes are still visible at high frequencies. As such, this study will search for asymmetric frequency shifts on the dipole mixed modes of partially suppressed red giant stars; the aim here is to investigate if both mode suppression and magnetic shifting of dipole mixed modes occur simultaneously. Thisstudywillbeconductedbycreatingapipelinetoestimatepriorsofasteroseismicparameters, use the priors to model the power spectra with the stellar modeling code sloscillations_ISTA, and perform a Bayesian fit of the parameters with the simulated data on the star KIC 6975038, a target with partially suppressed dipolar mode amplitudes identified in the literature, to fit its magnetic parameters. I present a novel method to model the stellar power spectra of partially suppressed red giants by application of a sigmoid profile to the ℓ= 1 dipolar mode component of the spectra. With the results of this study I aim at constraining the cause of this partial dipole mode amplitude suppression, allowing for more detailed studies regarding their astrophysical nature. Furthermore, the long term hope for the method used in this study will be to expand the sample of partially suppressed red giants and fit their asteroseismic parameters accordingly.