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Atmospheric mountain wave generation on Venus and its influence on the solid planet’s rotation rate

An Author Correction to this article was published on 15 October 2018

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The Akatsuki spacecraft observed a 10,000-km-long meridional structure at the top of the cloud deck of Venus that appeared stationary with respect to the surface and was interpreted as a gravity wave. Additionally, over four Venus solar days of observations, other such waves were observed to appear in the afternoon over equatorial highland regions. This indicates a direct influence of the solid planet on the whole Venusian atmosphere despite dissimilar rotation rates of 243 and 4 days, respectively. How such gravity waves might be generated on Venus is not understood. Here, we use general circulation model simulations of the Venusian atmosphere to show that the observations are consistent with stationary gravity waves over topographic highs—or mountain waves—that are generated in the afternoon in equatorial regions by the diurnal cycle of near-surface atmospheric stability. We find that these mountain waves substantially contribute to the total atmospheric torque that acts on the planet’s surface. We estimate that mountain waves, along with the thermal tide and baroclinic waves, can produce a change in the rotation rate of the solid body of about 2 minutes per solar day. This interplay between the solid planet and atmosphere may explain some of the difference in rotation rates (equivalent to a change in the length of day of about 7 minutes) measured by spacecraft over the past 40 years.

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Fig. 1: Planetary-scale gravity waves simulated with a GCM.
Fig. 2: Surface conditions.
Fig. 3: Atmospheric torques on the surface and length of day.

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Change history

  • 15 October 2018

    In the version of this Article originally published, a statement regarding past measurements of the length of day and rotation rate of Venus was potentially misleading. The original statement has now been replaced in the online versions of this Article, to acknowledge that neither Magellan nor Venus Express measured an instantaneous rotation rate.


  1. Fukuhara, T. et al. Large stationary gravity wave in the atmosphere of Venus. Nat. Geosci. 10, 85–88 (2017).

    Article  Google Scholar 

  2. Schubert G. in Venus (eds Hunten, D. M. et al.) 681–765 (Univ. Arizona Press, Tuscon, 1983).

  3. Kouyama, T. et al. Topographical and local time dependence of large stationary gravity waves observed at the cloud top of Venus. Geophys. Res. Lett. 44, 12098–12105 (2017).

    Article  Google Scholar 

  4. Lebonnois, S. et al. Superrotation of Venus’ atmosphere analyzed with a full general circulation model. J. Geophys. R. 115, E06006 (2010).

    Google Scholar 

  5. Lebonnois, S., Sugimoto, N. & Gilli, G. Wave analysis in the atmosphere of Venus below 100-km altitude, simulated by the LMD Venus GCM. Icarus 278, 38–51 (2016).

    Article  Google Scholar 

  6. McFarlane, N. A. The effect of orographically excited gravity wave drag on the general circulation of the lower stratosphere and troposphere. J. Atmos. Sci. 44, 1775–1800 (1987).

    Article  Google Scholar 

  7. Lott, F. & Miller, M. J. A new subgrid-scale orographic drag parametrization: its formulation and testing. Q. J. R. Meteorol. Soc. 123, 101–127 (1997).

    Article  Google Scholar 

  8. Scinocca, J. F. & McFarlane, N. A. The parametrization of drag induced by stratified flow over anisotropic orography. Q. J. R. Meteorol. Soc. 126, 2353–2393 (2000).

    Article  Google Scholar 

  9. Collins, M., Lewis, S. R. & Read, P. L. Gravity wave drag in a global circulation model of the martian atmosphere: Parameterisation and validation. Adv. Space Res. 19, 1245–1254 (1997).

    Article  Google Scholar 

  10. Forget, F. et al. Improved general circulation models of the Martian atmosphere from the surface to above 80 km. J. Geophys. Res. 104, 24155–24175 (1999).

    Article  Google Scholar 

  11. Haus, R., Kappel, D. & Arnold, G. Atmospheric thermal structure and cloud features in the southern hemisphere of Venus as retrieved from VIRTIS/VEX radiation measurements. Icarus 232, 232–248 (2014).

    Article  Google Scholar 

  12. Miranda, P. M. A. & James, I. N. Non-linear three-dimensional effects on gravity-wave drag: splitting flow and breaking waves. Q. J. R. Meteorol. Soc. 118, 1057–1081 (1992).

    Article  Google Scholar 

  13. Lebonnois, S. et al. Angular momentum budget in General Circulation Models of superrotating atmospheres: a critical diagnostic. J. Geophys. Res. 117, 12004 (2012).

    Article  Google Scholar 

  14. Mueller, N. T., Helbert, J., Erard, S., Piccioni, G. & Drossart, P. Rotation period of Venus estimated from Venus Express VIRTIS images and Magellan altimetry. Icarus 217, 474–483 (2012).

    Article  Google Scholar 

  15. Cottereau, L., Rambaux, N., Lebonnois, S. & Souchay, J. The various contributions in Venus rotation rate and LOD. Astron. Astrophys. 531, A45 (2011).

    Article  Google Scholar 

  16. Gold, T. & Soter, S. Atmospheric tides and the resonant rotation of Venus. Icarus 11, 356–366 (1969).

    Article  Google Scholar 

  17. Takagi, M. & Matsuda, Y. Effects of thermal tides on the Venus atmospheric superrotation. J. Geophys. Res. 112, D09112 (2007).

    Article  Google Scholar 

  18. Leconte, J., Wu, H., Menou, K. & Murray, N. Asynchronous rotation of Earth-mass planets in the habitable zone of lower-mass stars. Science 347, 632–635 (2015).

    Article  Google Scholar 

  19. Auclair-Desrotour, P., Laskar, J., Mathis, S. & Correia, A. C. M. The rotation of planets hosting atmospheric tides: from Venus to habitable super-Earths. Astron. Astrophys. 603, A108 (2017).

    Article  Google Scholar 

  20. Correia, A. C. M. & Laskar, J. The four final rotation states of Venus. Nature 411, 767 (2001).

    Article  Google Scholar 

  21. Garate-Lopez, I. & Lebonnois, S. Impacts of the cloud structure’s latitudinal variation on the general circulation of the Venus atmosphere as modeled by the LMD-GCM. EGU Geophys. Res. Abstracts 19, 12972 (2017).

    Google Scholar 

  22. Ford, P. G. & Pettengill, G. H. Venus topography and kilometer-scale slopes. J. Geophys. Res. 97, 13103–13114 (1992).

    Article  Google Scholar 

  23. Smith, R. B. Linear theory of stratified hydrostatic flow past an isolated mountain. Tellus 32, 348–364 (1980).

    Article  Google Scholar 

  24. Phillips, D. S. Analytical surface pressure and drag for linear hydrostatic flow over three-dimensional elliptical mountains. J. Atmos. Sci. 41, 1073–1084 (1984).

    Article  Google Scholar 

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We thank NASA for its financial support (grant NNX16AC84G) and the Akatsuki team for its discussions.

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T.N. performed the simulations, model development and scientific interpretation; G.S. contributed to the scientific interpretation, and S.L. to the model development and simulations.

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Correspondence to T. Navarro.

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The authors declare no competing interests.

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Navarro, T., Schubert, G. & Lebonnois, S. Atmospheric mountain wave generation on Venus and its influence on the solid planet’s rotation rate. Nature Geosci 11, 487–491 (2018).

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