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22 March 2025 |
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Article overview
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Tidally Forced Planetary Waves in the Tachocline of Solar-like Stars | | G.M. Horstmann
; G. Mamatsashvili
; A. Giesecke
; T.V. Zaqarashvili
; F. Stefani
; | | Date: |
1 Aug 2022 | | Abstract: | Can atmospheric waves in planet-hosting solar-like stars substantially
resonate to tidal forcing? Substantially at a level of impacting the space
weather or even of being dynamo-relevant? In particular, low-frequency Rossby
waves, which have been detected in the solar near-surface layers, are
predestined at responding to sunspot cycle-scale perturbations. In this paper,
we seek to address these questions as we formulate a forced wave model for the
tachocline layer, which is widely considered as the birthplace of several
magnetohydrodynamic planetary waves, i.e., Rossby, inertia-gravity
(Poincaré), Kelvin, Alfvén and gravity waves. The tachocline is modeled
as a shallow plasma atmosphere with an effective free surface on top that we
describe within the Cartesian $eta$-plane approximation. As a novelty to
former studies, we equip the governing equations with a conservative tidal
potential and a linear friction law to account for dissipation. We combine the
linearized governing equations to one decoupled wave equation, which
facilitates an easily approachable analysis. Analytical results are presented
and discussed within several interesting free, damped and forced wave limits
for both mid-latitude and equatorially trapped waves. For the idealized case of
a single tide generating body following a circular orbit, we derive an explicit
analytic solution that we apply to our Sun for estimating leading-order
responses to Jupiter. Our analysis reveals that Rossby waves resonating to
low-frequency perturbations can potentially reach considerable velocity
amplitudes in the order of $10^1 - 10^2, {
m cm}, {
m s}^{-1}$, which,
however, strongly rely on the yet unknown total dissipation. | | Source: | arXiv, 2208.00644 | | Services: | Forum | Review | PDF | Favorites | |
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