http://arxiv.org/abs/2301.07097
We develop a numerical method for directly computing the dissipative dynamical tidal response of rapidly rotating, oblate stars and gaseous planets with realistic internal structures. Applying these calculations to neutrally and stably stratified polytropes, we identify the most relevant resonances in models with rotation rates up to nearly the mass-shedding limit. We then compute the dynamical tidal response for Jupiter interior models including both stably stratified and convective regions. These calculations show that resonances involving waves with both gravito-inertial and purely inertial character are capable of explaining a discrepancy between observations and hydrostatic calculations of Jupiter’s response to tidal forcing by Io. This result contrasts with recent work that excluded Jupiter’s rotational flattening, and opens the door to resonances involving a wider range of internal oscillation modes than previously considered.
J. Dewberry
Wed, 18 Jan 23
34/133
Comments: 14 pages, 10 figures, submitted to MNRAS (comments welcome)