An equatorial oscillation in Saturn’s middle atmosphere

Abstract

The middle atmospheres of planets are driven by a combination of radiative heating and cooling, mean meridional motions, and vertically propagating waves (which originate in the deep troposphere). It is very difficult to model these effects and, therefore, observations are essential to advancing our understanding of atmospheres. The equatorial stratospheres of Earth and Jupiter oscillate quasi-periodically on timescales of about two and four years, respectively, driven by wave-induced momentum transport1,2,3,4,5. On Venus and Titan, waves originating from surface–atmosphere interaction and inertial instability are thought to drive the atmosphere to rotate more rapidly than the surface (superrotation). However, the relevant wave modes have not yet been precisely identified. Here we report infrared observations showing that Saturn has an equatorial oscillation like those found on Earth and Jupiter, as well as a mid-latitude subsidence that may be associated with the equatorial motion. The latitudinal extent of Saturn’s oscillation shows that it obeys the same basic physics as do those on Earth and Jupiter. Future highly resolved observations of the temperature profile together with modelling of these three different atmospheres will allow us determine the wave mode, the wavelength and the wave amplitude that lead to middle atmosphere oscillation.

Main

The stratosphere of Saturn is a region where temperatures increase with altitude, implying a large static stability and important wave activity. The upper stratosphere has a rich hydrocarbon chemistry that is initiated by methane photolysis and produces several species, from acetylene to benzene, which affect temperatures through their radiative properties. Unfortunately, observations performed before the arrival of the NASA Cassini spacecraft were generally limited in vertical coverage to the lower stratosphere (pressures greater than 1 hPa), where the dynamical and chemical timescales were longer than or comparable to a saturnian year6,7,8,9. Observations were also restricted to the summer hemisphere because the winter hemisphere was always hidden behind the optically thick rings. Cassini now gives us access to the full stratospheric range over the whole planet, in particular the upper stratosphere, where the seasonal forcing triggers rapid observable changes.

We acquired limb thermal spectra of Saturn for 2005–2006 using the Composite Infrared Spectrometer (CIRS) aboard Cassini. Limb viewing provides us with a vertical resolution of 1.5 times the scale height (75 km) and probes higher altitudes than nadir sounding10. Figure la displays the pressure–latitude cross-section of the zonal-mean temperature inverted from these CIRS limb spectra. Of particular note is the sharp difference in vertical structure between the northern and southern mid-latitudes and the equatorial region. At extratropical latitudes, the temperature steadily increases with altitude, whereas in the equatorial region it oscillates, with maximum amplitude centred on the equator. Although our temperature retrievals agree with previous measurements11,12 wherever the latter are available, only the vertical resolution and the horizontal coverage on both sides of the equator provided by CIRS limb observations allow us to detect and map the equatorial vertical oscillation. Using the thermal-wind equation (see Supplementary Information), we derived a zonal thermal-wind pressure–latitude cross-section for the stratosphere (Fig. 1b). The vertical structure of the zonal thermal wind at the equator clearly shows alternate bands of eastward and westward vertical shear from the 0.2-hPa altitude down to the 5-hPa altitude.

Figure 1: Saturn’s equatorial oscillation.
figure1

a, This temperature map was retrieved using the hydrogen collision-induced continuum (600 cm-1) between the 20 and 2 hPa pressure levels, and the v4-band of methane (1,300 cm-1) between the 3 and 0.003 hPa pressure levels (see Supplementary Information). The contours indicate temperature in Kelvin. The CIRS observed the planet’s limb each 5° of latitude between 45° S and 45° N (here and in b, negative latitudes lie in the southern hemisphere). The ten detectors were aligned vertically, perpendicular to the planet's limb. Each detector independently probed a given altitude with a vertical resolution of 50–100 km. The temperatures presented in this figure were retrieved from 15.5-cm-1spectra. Vertical profiles of atmospheric temperature were retrieved by means of a constrained inversion with strong low-pass filtering at each limb position. The number of independent longitudes sampled for a given latitude varies between two and four. At the equator the temperature near 10 hPa is 17 K colder than it is at 20° S and 20° N, whereas the equatorial temperature is 20 K warmer near 1 hPa; near 0.1 hPa the equator is again 20 K colder, and at 0.01 hPa the equatorial region is 10 K warmer than it is at adjacent latitudes. b, This map presents the thermal wind field obtained by upward integration of the thermal wind equation on cylinders (see Supplementary Information). The contours indicate measured wind speed minus wind speed at 20 hPa, in metres per second. The dashed parabola delineates the exclusion zone within which the winds cannot be calculated from the thermal wind equation, but are instead interpolated. The error in temperature due to instrument noise is 2 K, and this propagates to an error of 5/(sine of latitude) m s-1 per scale height in the zonal winds.

This temperature and zonal wind structure resembles those of Earth’s quasi-biennial oscillation (QBO) and Jupiter’s quasi-quadrennial oscillation (QQO), in which temperature anomalies and eastward/westward winds alternate in altitude1,2,3,4,5. As the QBO and QQO vertical structures of alternating temperature anomalies and winds propagate down, the equatorial wind regime at a given height cyclically changes from easterly to westerly. On Earth, the alternating wind regimes repeat at intervals that vary from 22 to 34 months, with an average period of about 28 months1,2. On Jupiter, the equatorial stratospheric temperature exhibits a 4.4-year period and the equatorial zonal winds in the upper troposphere oscillate with a 4.5-year period3,13,14. Long-term ground-based monitoring reveals a period of 14.7 ± 0.9 terrestrial years on Saturn15. The observational similarities between Saturn’s oscillation and the QBO and QQO are the strong equatorial confinement of temperature minima and maxima and associated shear layers, a stronger eastward than westward shear layer, and the bounding of the equatorial oscillation at latitudes 15–20° north and south. Temperatures near these latitudes are relatively high when equatorial temperatures are relatively low, and vice versa.

On Earth and Jupiter, the quasi-periodic oscillations are triggered by the interaction between upwardly propagating waves and the mean zonal flow2,4,16,17,18,19,20. Planetary-scale Kelvin waves contribute to eastward stresses, whereas mixed Rossby-gravity waves contribute to westward stresses. Over time, the zonal-mean wind anomalies descend and are damped by viscous processes at the tropopause, leading to the observed quasi-periodic cycle. Observations of Saturn (either cloud tracking or thermal measurements21,22,23,24) show abundant evidence for the presence of waves of sizes ranging from planetary scale to mesoscale. These waves may be generated by the deep convection that carries the internal heat flux and waves generated by shear instabilities. Hence, Saturn exhibits conditions similar to the terrestrial and jovian environments that are favourable to the establishment of an equatorial oscillation driven by vertically propagating waves. A simple model that considers the equations for the evolution of a longitudinally symmetric atmosphere subject to a mechanical forcing shows that the equatorial oscillation should be confined within a distance L of the equator (see Supplementary Information). A scale analysis of these equations yields the relation L < (aDN/(2Ω))1/2(ω/α)1/4, where a is Saturn’s radius, D is a height scale, N is the buoyancy frequency, Ω is Saturn’s spin rate, α is a constant radiative timescale and ω is the mechanical forcing frequency. This scale analysis for Saturn yields L = 7,400 km (seven degrees of latitude), in satisfactory agreement with our observations.

At extratropical latitudes, the response of a rapidly rotating atmosphere to the forcing due to planetary-scale waves is quite distinct from that in the tropics: the forcing is balanced by the Coriolis force produced by a mean meridional circulation. Indeed, at mid-latitudes, the stratospheric thermal profile that we retrieved differs completely from that in the equatorial region, in that it steadily increases with altitude. Surprisingly, the temperature difference between 45° S and 45° N at pressures between 10 and 1 hPa is larger than that measured for pressures between 0.1 and 0.01 hPa. At 1–10 hPa the temperature difference peaks at 15 K, whereas at 0.01–0.1 hPa it reaches only 6–7 K. The season observed on Saturn was southern midsummer (the solstice took place in October 2002). The observed temperature gradient between the southern and northern hemispheres should be close to its greatest seasonal amplitude8. Because the thermal inertia increases with depth, owing to larger optical depths, the latitudinal gradient was expected to be higher in the upper stratosphere than it is in the lower stratosphere.

To further explore this issue, we calculated the radiative cooling rates using the hydrocarbon vertical profiles inverted from CIRS limb data (Fig. 2). At 0.01 hPa we obtained a similar cooling rate of 0.2 K per day for latitudes 30° S and 30° N (Fig. 3). This similarity in upper stratosphere cooling rates between the summer and winter hemispheres is in sharp contrast with the differences in the daily mean insolation, which combines the effects of Saturn’s obliquity and screening by the thick rings. At the time of our observations, the ratio of the solar insolation at 30° S to that at 30° N is greater than three (daily mean of 5 W m-2 in the southern hemisphere and 1.5 W m-2 in the northern hemisphere6,9). Hence, the observed state of the upper stratosphere requires either that the heating rate is dominated by a season-independent source or that heat is meridionally redistributed.

Figure 2: Vertical–zonal map of ethane abundance.
figure2

This pressure–latitude cross-section of the ethane volume mixing ratio (indicated by the contours) is inverted by fitting the v9-band of ethane (820 cm-1) observed by the CIRS between 1 and 0.01 hPa. The temperature field used in the calculation is presented in Fig. 1. CIRS spectra measuring the temperature and the composition were obtained simultaneously at the same vertical and spectral resolution. Vertical profiles of the ethane volume mixing ratio were retrieved by means of a constrained inversion with strong low-pass filtering (see Supplementary Information).

Figure 3: Radiative cooling rates in the northern and southern hemispheres.
figure3

The radiative cooling rates were calculated at 30° N (black) and 30° S (red) between 2 and 0.003 hPa, by differentiating the net thermal flux integrated over the v4-band of methane, the v9-band of ethane and the v5-band of acetylene. The hydrocarbon abundance was set to the retrieved value presented in Fig. 2.

The meridional–vertical cross-section of the ethane abundance supports the hypothesis that heat is meridionally redistributed (Fig. 2). In the southern hemisphere, the observed equator-to-mid-latitude abundance gradient agrees with the prediction of photochemical models that it should resemble the yearly average insolation rather than the current seasonal insolation9. However, in the northern hemisphere, the local maximum of the abundance in the upper atmosphere centred at 30° N matches neither the yearly average insolation nor the current insolation. This local maximum constitutes a second strong piece of evidence for transport of hydrocarbon-rich air masses from the southern upper stratosphere to the northern hemisphere. We estimated the vertical velocity needed to explain the observed temperature, assuming adiabatic heating (N2HR-1w = J/cp , where H is the atmospheric scale height, w is the vertical wind speed, J is the heating rate, R is the gas constant and c is the specific heat capacity at constant pressure). We did not calculate the solar heating rate, but we assumed that the atmosphere is globally in radiative balance, that is, that the total radiative cooling at 30° south and north is equal to the total solar heating at these two latitudes. With a heating rate three times larger at 30° S than it is at 30° N, this gives heating rates of 0.30 and 0.10 K per day, respectively, leading to a vertical velocity of 1.5 mm s-1.

This extratropical meridional circulation might be influenced by the equatorial oscillation. On Earth, the QBO does modulate the mean meridional circulation. Equatorial temperature minima are associated with local ascent and, by continuity, descent at extratropical latitudes. One interesting aspect of the global QBO is that the extratropical temperature anomalies are seasonally synchronized, occurring primarily during winter in each hemisphere. The reason for this is not fully known, but one possibility is that during northern winter the meridional flow from south to north, with subsidence in the northern hemisphere, will be reinforced by the QBO-induced sinking motion at extratropical latitudes. On Saturn, the latitude-15° temperature anomalies at the 0.1-Pa and 20-Pa pressure levels are indeed warmer in the northern hemisphere than they are in the southern hemisphere. This seasonal asymmetry is another strong similarity in the behaviours of the stratospheres of Saturn and Earth.

References

  1. 1

    Andrews, D. G., Holton, J. R. & Leovy, C. B. Middle Atmosphere Dynamics (Academic, New York, 1987)

  2. 2

    Baldwin, M. P. et al. The quasi-biennial oscillation. Rev. Geophys. 39, 179–230 (2001)

  3. 3

    Leovy, C. B., Friedson, A. J. & Orton, G. S. The quasiquadrennial oscillation of Jupiter’s equatorial stratosphere. Nature 354, 380–382 (1991)

  4. 4

    Friedson, A. J. New observations and modelling of a QBO-like oscillation in Jupiter’s stratosphere. Icarus 137, 34–55 (1999)

  5. 5

    Flasar, F. M. et al. An intense stratospheric jet on Jupiter. Nature 427, 132–135 (2004)

  6. 6

    Barnet, C. D., Beebe, R. F. & Conrath, B. J. A seasonal radiative-dynamic model of Saturn’s troposphere. Icarus 98, 94–107 (1992)

  7. 7

    Bézard, B. & Gautier, D. A seasonal climate model of the atmospheres of the giant planets at the Voyager encounter time. I. Saturn’s stratosphere. Icarus 60, 296–310 (1985)

  8. 8

    Conrath, B. J., Gierasch, P. J. & Leroy, S. S. Temperature and circulation in the stratosphere of the outer planets. Icarus 83, 255–281 (1990)

  9. 9

    Moses, J. I. & Greathouse, T. K. Latitudinal and seasonal models of stratospheric photochemistry on Saturn: Comparision with infrared data from IRTF/TEXES. J. Geophys. Res. 110, 09007 (2005)

  10. 10

    Flasar, F. M. et al. Exploring the Saturn system in the thermal infrared: The Composite Infrared Spectrometer. Space Sci. Rev. 115, 169–297 (2004)

  11. 11

    Flasar, F. M. et al. Temperatures, winds, and composition in the Saturnian system. Science 307, 1247–1251 (2005)

  12. 12

    Greathouse, T. K. et al. Meridional variations of temperature, C2H2 and C2H6 abundances in Saturn’s stratosphere at southern summer solstice. Icarus 177, 18–31 (2005)

  13. 13

    Orton, G. S. et al. Thermal maps of Jupiter: Spatial organization and time dependence of stratospheric temperatures, 1980 to 1990. Science 252, 537–542 (1991)

  14. 14

    Simon-Miller, A. A., Poston, B. W., Orton, G. S. & Fisher, B. Wind variations in Jupiter’s equatorial atmosphere: A QQO counterpart? Icarus 186, 192–203 (2007)

  15. 15

    Orton, G. S. et al. Semi-annual oscillations in Saturn’s low-latitude stratospheric temperatures. Nature doi: 10.1038/nature06897 (this issue)

  16. 16

    Lindzen, R. S. & Holton, J. R. A theory of the quasi-biennial oscillation. J. Atmos. Sci. 25, 1095–1107 (1968)

  17. 17

    Holton, J. R. & Lindzen, R. S. An updated theory for the quasi-biennial cycle of the tropical troposphere. J. Atmos. Sci. 29, 1076–1080 (1972)

  18. 18

    Gray, L. J. & Pyle, J. A. A two-dimensional model of the quasi-biennial oscillation in ozone. J. Atmos. Sci. 46, 203–220 (1989)

  19. 19

    Dunkerton, T. J. Nonlinear propagation of zonal winds in an atmosphere with Newtonian cooling and equatorial wavedriving. J. Atmos. Sci. 48, 236–263 (1991)

  20. 20

    Li, X. & Read, P. L. A mechanical model of the quasi-quadrennial oscillation in Jupiter’s stratosphere. Planet. Space Sci. 48, 637–669 (2000)

  21. 21

    Beebe, R. F., Barnet, C., Sada, P. V. & Murrell, A. S. The onset and growth of the 1990 equatorial disturbance on Saturn. Icarus 95, 163–172 (1992)

  22. 22

    Sanchez-Lavega, A. Observations of Saturn’s Ribbon Wave 14 years after Its discovery. Icarus 158, 272–275 (2002)

  23. 23

    Achterberg, R. K. & Flasar, F. M. Planetary-scale thermal waves in Saturn’s upper troposphere. Icarus 119, 350–369 (1996)

  24. 24

    Schinder, P. J. et al. Vertically propagating waves in the upper atmosphere of Saturn from Cassini radio occultations. (AGU Fall Meeting Abstract No. P23D-06, 2005)

Download references

Author information

Correspondence to T. Fouchet.

Supplementary information

Supplementary Information

The file contains Supplementary Notes, Supplementary Table 1 and Supplementary Figures 1-2 with Legends. (PDF 396 kb)

Rights and permissions

Reprints and Permissions

About this article

Cite this article

Fouchet, T., Guerlet, S., Strobel, D. et al. An equatorial oscillation in Saturn’s middle atmosphere. Nature 453, 200–202 (2008). https://doi.org/10.1038/nature06912

Download citation

Further reading

Comments

By submitting a comment you agree to abide by our Terms and Community Guidelines. If you find something abusive or that does not comply with our terms or guidelines please flag it as inappropriate.