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A 2D model for the excitation of the linearly stable inertial modes of the Sun by turbulent convection

Published online by Cambridge University Press:  23 December 2024

J. Philidet Open the ORCID record for J. Philidet [Opens in a new window]  and
L. Gizon
J. Philidet*
Affiliation:
Max–Planck Institute for Solar System Research, Göttingen, Germany
L. Gizon
Affiliation:
Max–Planck Institute for Solar System Research, Göttingen, Germany
*
email: [email protected]
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Abstract

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The newly discovered inertial modes in the Sun offer the opportunity to probe the solar convective zone down to the tachocline. While linear analysis predicts the frequencies and eigenfunctions of the modes, it gives no information about their excitation or their amplitudes. We present here a theoretical formalism for the stochastic excitation of the solar inertial modes by turbulent convection. The amplitudes predicted by our model are in complete agreement with observations, thus supporting the assumption that they are stochastically excited. Our work also uncovers a qualitative transition in the shape of the inertial mode spectrum, between m ≲ 5 where the modes are clearly resolved in frequency, and m ≳ 5 where the modes overlap. This complicates the interpretation of the high-m data, and suggests that a model for the whole shape of the power spectrum is necessary to exploit the full seismic potential of solar inertial modes.

Keywords

waves – turbulence – Sunoscillations – Suninterior – Sunhelioseismology
Type
Contributed Paper
Information
Proceedings of the International Astronomical Union , Volume 19 , Symposium S365: Dynamics of Solar and Stellar Convection Zones and Atmospheres , December 2023 , pp. 225 - 229
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Copyright
© The Author(s), 2024. Published by Cambridge University Press on behalf of International Astronomical Union

References

Bekki, Y., Cameron, R. H., and Gizon, L.. Theory of solar oscillations in the inertial frequency range: Amplitudes of equatorial modes from a nonlinear rotating convection simulation. arXiv e-prints, art. arXiv:2208.11081, Aug. 2022.Google Scholar
Fournier, D., Gizon, L., and Hyest, L.. Viscous inertial modes on a differentially rotating sphere: Comparison with solar observations., 664:A6, Aug. 2022. doi: 10.1051/0004-6361/202243473.Google Scholar
Gizon, L., Fournier, D., and Albekioni, M.. Effect of latitudinal differential rotation on solar Rossby waves: Critical layers, eigenfunctions, and momentum fluxes in the equatorial β plane., 642:A178, Oct. 2020. doi: 10.1051/0004-6361/202038525.Google Scholar
Gizon, L., Cameron, R. H., Bekki, Y., Birch, A. C., Bogart, R. S., Brun, A. S., Damiani, C., Fournier, D., Hyest, L., Jain, K., Lekshmi, B., Liang, Z.-C., and Proxauf, B.. Solar inertial modes: Observations, identification, and diagnostic promise., 652:L6, Aug. 2021. doi: 10.1051/0004-6361/202141462.Google Scholar
Goldreich, P. and Keeley, D. A.. Solar seismology. II. The stochastic excitation of the solar p-modes by turbulent convection., 212:243–251, Feb. 1977. doi: 10.1086/155043.Google Scholar
Hanson, C. S., Hanasoge, S., and Sreenivasan, K. R.. Discovery of high-frequency retrograde vorticity waves in the Sun. Nature Astronomy, 6:708–714, Mar. 2022. doi: 10.1038/s41550-022-01632-z.CrossRefGoogle Scholar
Liang, Z.-C., Gizon, L., Birch, A. C., and Duvall, T. L.. Time-distance helioseismology of solar Rossby waves., 626:A3, June 2019. doi: 10.1051/0004-6361/201834849.Google Scholar
Lighthill, M. J.. Predictions on the Velocity Field Coming from Acoustic Noise and a Generalized Turbulence in a Layer Overlying a Convectively Unstable Atmospheric Region. In R. N. Thomas, editor, Aerodynamic Phenomena in Stellar Atmospheres, volume 28, page 429, Jan. 1967.CrossRefGoogle Scholar
Löptien, B., Gizon, L., Birch, A. C., Schou, J., Proxauf, B., Duvall, T. L., Bogart, R. S., and Christensen, U. R.. Global-scale equatorial Rossby waves as an essential component of solar internal dynamics. Nature Astronomy, 2:568–573, May 2018. doi: 10.1038/s41550-018-0460-x.CrossRefGoogle Scholar
Papaloizou, J. and Pringle, J. E.. Non-radial oscillations of rotating stars and their relevance to the short-period oscillations of cataclysmic variables., 182:423–442, Feb. 1978. doi: 10.1093/mnras/182.3.423.Google Scholar
Philidet, J. and Gizon, L.. Interaction of solar inertial modes with turbulent convection. A 2D model for the excitation of linearly stable modes., 673:A124, May 2023. doi: 10.1051/0004-6361/202245666.Google Scholar
Samadi, R. and Goupil, M. J.. Excitation of stellar p-modes by turbulent convection. I. Theoretical formulation., 370:136–146, Apr. 2001. doi: 10.1051/0004-6361:20010212.Google Scholar
Triana, S. A., Guerrero, G., Barik, A., and Rekier, J.. Identification of Inertial Modes in the Solar Convection Zone., 934(1):L4, July 2022. doi: 10.3847/2041-8213/ac7dac.Google Scholar