Abstract
Inertial waves, which are predominantly driven by the Coriolis force, likely play an important role in solar dynamics, and, additionally, they provide a window into the solar subsurface. The latter allows us to infer properties that are inaccessible to the traditional technique of acoustic wave helioseismology. Thus, a full characterization of these normal modes holds the promise of enabling investigations into solar subsurface dynamics. In this work, we develop a spectral eigenvalue solver to model the spectrum of inertial waves in the Sun. We model the solar convection zone as an anelastic medium, and solve for the normal modes of the momentum and energy equations. We demonstrate that the solver can well reproduce the observed mode frequencies and line widths, not only of sectoral Rossby modes, but also of recently observed high-frequency inertial modes. In addition, we believe that the spectral solver is a useful contribution to the numerical methods of modeling inertial modes on the Sun.
| Original language | English (US) |
|---|---|
| Pages (from-to) | 21 |
| Journal | The Astrophysical Journal Supplement Series |
| Volume | 264 |
| Issue number | 1 |
| DOIs | |
| State | Published - Jan 11 2023 |
| Externally published | Yes |
Bibliographical note
KAUST Repository Item: Exported on 2023-01-18Acknowledged KAUST grant number(s): OSR-CRG2020-4342
Acknowledgements: This material is based upon work supported by Tamkeen under the NYU Abu Dhabi Research Institute grant G1502. We also acknowledge support from the King Abdullah University of Science and Technology (KAUST) Office of Sponsored Research (OSR), under award OSR-CRG2020-4342. This research was carried out on the High-Performance Computing resources at New York University Abu Dhabi.
This publication acknowledges KAUST support, but has no KAUST affiliated authors.
ASJC Scopus subject areas
- Astronomy and Astrophysics
- Space and Planetary Science