Verify differential rotation in HD 112485

Verify whether HD 112485 exhibits radial differential rotation through dedicated rotational inversions that independently test the differing effective rotation frequencies inferred from its p- and g-mode multiplets.

Background

The two candidate multiplets in HD 112485 probe different regions of the stellar interior: the higher-frequency dipole p mode is primarily envelope-sensitive, whereas the lower-frequency mode has predominantly g-mode character and is sensitive to the near-core region. Their inferred effective rotation frequencies differ, providing tentative evidence for radial differential rotation. However, the lower-frequency zonal mode is less well reproduced by the forward model, and its preferred rotation rate lies near the upper boundary of the available StORM grid. The models do not include radial rotation profiles, so dedicated inversions are required to establish whether the difference reflects genuine differential rotation.

References

The difference in their inferred effective rotation frequencies, together with their distinct radial sensitivities, therefore provides tentative evidence of differential rotation. Yet, this interpretation requires future verification from actual dedicated rotation inversions for the star because the zonal mode of the lower-frequency multiplet is less well reproduced and its preferred rotation solution lies near the upper limit of the available StORM grid.

— Ensemble pulsational characteristics of eclipsing binaries containing $β$ Cep stars observed by the TESS mission  (2610.01679 - Eze et al., 1 Oct 2026) in Section 7.1, Assessing differential rotation in HD 112485; Section 7.2, Rotational Sensitivity Kernel