A Unifying Model of Mixed Inertial Modes in the Sun

Abstract We present an analytical model that unifies many of the inertial waves that have been recently observed on the surface of the Sun, as well as many other modes that have been theoretically predicted—but have yet to be observed—into a single family of mixed inertial modes . By mixed, we mean...

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Bibliographic Details
Published inAstrophysical journal. Letters Vol. 965; no. 1; p. L8
Main Authors Jain, Rekha, Hindman, Bradley W., Blume, Catherine
Format Journal Article
LanguageEnglish
Published Austin The American Astronomical Society 01.04.2024
IOP Publishing
Subjects
Anelasticity
Astrophysical fluid dynamics
Hydrodynamics
Inertial waves
Internal waves
Mathematical models
Modes
Planetary waves
Radial velocity
Rossby waves
Solar convective zone
Solar interior
Solar surface
Stellar oscillations
Velocity
Wave propagation
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Summary:Abstract We present an analytical model that unifies many of the inertial waves that have been recently observed on the surface of the Sun, as well as many other modes that have been theoretically predicted—but have yet to be observed—into a single family of mixed inertial modes . By mixed, we mean that the prograde- and retrograde-propagating members of this family have different restoring forces and hence different behavior. Thermal Rossby waves exist as prograde-propagating waves, while the high-frequency retrograde (HFR) wave is one example of a member of the retrograde branch. This family of mixed modes has fully 3D motions that satisfy the anelastic form of the continuity condition. As such, the horizontal velocity is both vortical and divergent with the later flow component associated with a dynamically important radial velocity. The modes are differentiated by the number of nodes in latitude, with the lowest latitudinal order corresponding to the traditional thermal Rossby wave of Busse, the first latitudinal overtone to the mixed mode of Bekki et al., and the second overtone to the HFR wave discovered by Hanson et al. There also exist infinitely more modes of higher latitudinal order whose frequencies increase as the order increases. These higher overtones may correspond to many of the inertial modes that have been recently identified by numerical eigenmode solvers.
Bibliography:AAS52476
The Sun and the Heliosphere
ISSN:2041-8205
2041-8213
DOI:10.3847/2041-8213/ad35c6