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Supergranular-scale solar convection not explained by mixing-length theory

Nature Astronomy volume 8, pages 1088–1101 (2024)Cite this article

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Abstract

Supergranules, which are solar flow features with a lateral scale of 30,000–40,000 km and a lifetime of ~24 h, form a prominent component of the Sun’s convective spectrum. However, their internal flows, which can be probed only by helioseismology, are not well understood. We analyse dopplergrams recorded by the Solar Dynamics Observatory satellite to identify and characterize ~23,000 supergranules. We find that the vertical flows peak at a depth of ~10,000 km, and remain invariant over the full range of lateral supergranular scales, contrary to numerical predictions. We also infer that, within the local seismic resolution (≳5,000 km), downflows are ~40% weaker than upflows, indicating an apparent mass-flux imbalance. This may imply that the descending flows also comprise plumes, which maintain the mass balance but are simply too small to be detected by seismic waves. These results challenge the widely used mixing-length description of solar convection.

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Fig. 1: Surface flow, magnetic field and seismology measurements of the average supergranule.
Fig. 2: Vertical and horizontal flows of the average supergranule.
Fig. 3: Distribution of inflow and outflow sizes and the change in peak depth with horizontal extent.

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Data availability

The HMI data are courtesy of NASA/SDO and the HMI Science Team. The HMI data are available from the Joint Science Operations Center export site http://jsoc.stanford.edu/. Due to the large volume of data, the mode-coupling products and kernels are available from the authors upon request. The numerical simulations are available upon request from M. Rempel.

Code availability

The mode coupling and inversion codes are available at https://github.com/cshanson/modeCoupling.git. Codes for the Slepian functions are available upon request from F. J. Simons.

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Acknowledgements

We thank F. J. Simons for the codes for computing Slepian functions, M. Rempel and R. Cameron for their insights into solar convection, J. W. Lord for the numerical simulations and J. Naranjo for his help with the NYUAD NetDRMS system. This research was carried out with the High Performance Computing resources at NYUAD. The datasets were prepared in the data centre at the Center for Space Science of NYUAD. This research is based upon work supported by Tamkeen under the NYUAD Research Institute (Grant Nos G1502 and CASS to C.S.H, S.H. and K.R.S.). S.H. acknowledges funding from the Department of Atomic Energy, India. K.R.S. and S.H. acknowledge support from the Office of Sponsored Research of King Abdullah University of Science and Technology (Award No. OSR-CRG2020-4342). S.B.D. acknowledges funding from the Elisabeth H. and F. A. Dahlen Award 2022 by the Department of Geosciences, Princeton University. S.B.D. also acknowledges funding from the European Union’s Horizon 2020 research and innovation programme under a Marie Skłodowska-Curie grant (Grant Agreement No. 101034413). Some data products were processed and downloaded from the German Data Center for SDO, which is funded by the German Aerospace Center (DLR Grant No. 500L1701).

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Authors and Affiliations

  1. Center for Astrophysics and Space Science (CASS), NYUAD Research Institute, New York University Abu Dhabi, Abu Dhabi, UAE

    Chris S. Hanson, Shravan Hanasoge & Katepalli R. Sreenivasan

  2. Department of Geosciences, Princeton University, Princeton, NJ, USA

    Srijan Bharati Das

  3. Institute of Science and Technology Austria (IST Austria), Klosterneuburg, Austria

    Srijan Bharati Das

  4. Smithsonian Astrophysical Observatory, Cambridge, MA, USA

    Srijan Bharati Das

  5. Department of Astronomy and Astrophysics, Tata Institute of Fundamental Research, Mumbai, India

    Prasad Mani & Shravan Hanasoge

  6. Sydney Institute for Astronomy, School of Physics, University of Sydney, Sydney, New South Wales, Australia

    Prasad Mani

  7. Department of Physics, New York University, New York, NY, USA

    Katepalli R. Sreenivasan

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Contributions

C.S.H., S.H. and K.R.S. designed the research. C.S.H. developed the software and performed the observational and computational analysis. S.B.D. developed and implemented the mathematical formalism for Slepian functions in this analysis. P.M. tuned the surface measurements and developed the software. All authors discussed the results and contributed to the manuscript.

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Correspondence to Chris S. Hanson.

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Hanson, C.S., Bharati Das, S., Mani, P. et al. Supergranular-scale solar convection not explained by mixing-length theory. Nat Astron 8, 1088–1101 (2024). https://doi.org/10.1038/s41550-024-02304-w

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