First measurements of Jupiter’s zonal winds with visible imaging spectroscopy

Gonçalves, Ivan; Schmider, F. X.; Gaulme, P.; Morales-Juberías, R.; Guillot, T.; Rivet, J. P.; Appourchaux, T.; Boumier, P.; Jackiewicz, Jason; Sato, Bun’ei; Ida, Shigeru; Ikoma, Masahiro; Mékarnia, D.; Underwood, Thomas A.; Voelz, David G.

doi:10.1016/j.icarus.2018.10.019

Cited by 17 publications

(35 citation statements)

References 73 publications

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“…The THEMIS telescope plans to get an AO system soon, however it will be designed for working on the Sun, which is likely not adapted for observing planetary targets. In the short term, the most promising alternative is the JOVIAL/JIVE project (principal investigator is second author Schmider), which consists of three identical Doppler imaging spectrometers that will be installed in France, New Mexico, and Japan (Gonçalves et al 2016(Gonçalves et al , 2019. The original purpose of the project is to get RV maps of Jupiter and Saturn at short cadence (30 s) to conduct seismic observations of these planets similar to techniques of helioseismology.…”

Section: Discussion and Prospectsmentioning

confidence: 99%

“…The JOVIAL/JIVE instrument is able to provide a complete RV map in only one exposure and does not have any of the issues we encountered in this work in building maps from 1D segments. A paper dedicated to the first Doppler measurements of the wind of Jupiter was recently published by Gonçalves et al (2019). Preliminary observations of Venus were led in spring 2018, and more observations could be done with AO with the C2PU 1 m telescope at the Calern observatory (France) in 2019 or 2020.…”

Section: Discussion and Prospectsmentioning

confidence: 99%

“…As far as we know, it is the first instantaneous optically resolved RV map of any planet of the solar system in the visible domain. The RV image of Jupiter obtained by Gonçalves et al (2019) with the JOVIAL/JIVE instrument are averaged over several complete planetary rotations.…”

Section: Models Of Atmospheric Circulationmentioning

confidence: 99%

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Atmospheric circulation of Venus measured with visible imaging spectroscopy at the THEMIS observatory

Gaulme

Schmider

Widemann

et al. 2019

A&A

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Measuring the atmospheric circulation of Venus at different altitudes is important for understanding its complex dynamics, in particular the mechanisms driving super-rotation. Observationally, Doppler imaging spectroscopy is in principle the most reliable way to measure wind speeds of planetary atmospheres because it directly provides the projected speed of atmospheric particles. However, high-resolution imaging spectroscopy is challenging, especially in the visible domain, and most knowledge about atmospheric dynamics has been obtained with the cloud tracking technique. The objective of the present work is to measure the global properties of the atmospheric dynamics of Venus at the altitude of the uppermost clouds, which is probed by reflected solar lines in the visible domain. Our results are based on high-resolution spectroscopic observations with the long-slit spectrometer of the solar telescope THEMIS. We present the first instantaneous "radial-velocity snapshot" of any planet of the solar system in the visible domain, i.e., a complete radial-velocity map of the planet obtained by stacking data on less than 10 % of its rotation period. From this, we measured the properties of the zonal and meridional winds, which we unambiguously detect. We identify a wind circulation pattern that significantly differs from previous knowledge about Venus. The zonal wind reveals a "hot spot" structure, featuring about 200 m s −1 at sunrise and 70 m s −1 at noon in the equatorial region. Regarding meridional winds, we detect an equator-to-pole meridional flow peaking at 45 m s −1 at mid-latitudes, i.e., about twice as large as what has been reported so far.

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Section: Discussion and Prospectsmentioning

confidence: 99%

Section: Discussion and Prospectsmentioning

confidence: 99%

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Atmospheric circulation of Venus measured with visible imaging spectroscopy at the THEMIS observatory

Gaulme

Schmider

Widemann

et al. 2019

A&A

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“…For the other giant planets, one must rely on continuous observations of the planetary disk for at least days to detect waves that have amplitudes of at most a few tens of cm/s. Ground based observations at Jupiter with a Doppler imager appear promising -yielding already the direct measurement of zonal winds, with the ability to potentially measure meridional and vertical speeds (Gonçalves et al, 2019). Given the potential of the method, the application to a spacecraft at Uranus or Neptune should be studied.…”

Section: Seismologymentioning

confidence: 99%

Uranus and Neptune are key to understand planets with hydrogen atmospheres

Guillot¹

2024

Preprint

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<div class="page" title="Page 1"> <div class="layoutArea"> <div class="column"> <p>Uranus and Neptune are the last unexplored planets of the Solar System. I show that they hold crucial keys to understand the atmospheric dynamics and structure of planets with hydrogen atmospheres. Their atmospheres are active and storms are believed to be fueled by methane condensation which is both extremely abundant and occurs at low optical depth. This means that mapping temperature and methane abundance as a function of position and depth will inform us on how convection organizes in an atmosphere with no surface and condensates that are heavier than the surrounding air, a general feature of gas giants. Using this information will be essential to constrain the interior structure of Uranus and Neptune themselves, but also of Jupiter, Saturn and numerous exoplanets with hydrogen atmospheres. Owing to the spatial and temporal variability of these atmospheres, an orbiter is required. A probe would provide a reference profile to lift ambiguities inherent to remote observations. It would also measure abundances of noble gases which can be used to reconstruct the history of planet formation in the Solar System. Finally, mapping the planets&#8217; gravity and magnetic fields will be essential to constrain their global composition, structure and evolution.</p> </div> </div> </div>

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“…Upper tropospheric wind velocities are difficult to quantify, however, as there are no visible targets to track. One possible avenue is to use Doppler shifts from spectral lines, similar to Gonçalves et al (2019), who use a spectrometer to obtain Doppler wind speeds measured in the visible spectrum. Their method would be able to sense actual particle velocities, but they note that the limited spectral and spatial resolution degrades the accuracy of the data near regions where the dynamics deviate significantly from the zonal mean, e.g.…”

Section: Drift Rate and Vertical Wind Shearmentioning

confidence: 99%

The aftermath of convective events near Jupiter's fastest prograde jet: implications for clouds, dynamics and vertical wind shear

Sankar,

Klare,

Palotai

2021

Preprint

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The 24 • N jet borders the North Tropical Belt and North Tropical Zone, and is the fastest prograde jet on Jupiter, reaching speeds above 170 m/s. In this region, observations have shown several periodic convective plumes, likely from latent heat release from water condensation, which affect the cloud and zonal wind structure of the jet. We model this region with the Explicit Planetary hybrid-Isentropic Coordinate model using its active microphysics scheme to study the phenomenology of water and ammonia clouds within the jet region. On perturbing the atmosphere, we find that an upper tropospheric wave develops that directly influences the cloud structure within the jet. This wave travels at ∼ 75 m/s in our model, and leads to periodic chevron-shaped features in the ammonia cloud deck. These features travel with the wave speed, and are subsequently much slower than the zonal wind at the cloud deck. The cloud structure, and the slower drift rate, were both observed following the convective outbreak in this region in 2016 and 2020. We find that an upper level circulation is responsible for these cloud features in the aftermath of the convective outbursts. The comparatively slower observed drift rates of these features, relative to the wind speed of the jet, provides constraints on the vertical wind shear above the cloud tops, and we suggest that wind velocities determined from cloud tracking should correspond to a different altitude compared to the 680 hPa pressure level. We also diagnose the convective potential of the atmosphere due to water condensation, and find that it is strongly coupled to the wave.

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First measurements of Jupiter’s zonal winds with visible imaging spectroscopy

Cited by 17 publications

References 73 publications

Atmospheric circulation of Venus measured with visible imaging spectroscopy at the THEMIS observatory

Atmospheric circulation of Venus measured with visible imaging spectroscopy at the THEMIS observatory

Uranus and Neptune are key to understand planets with hydrogen atmospheres

The aftermath of convective events near Jupiter's fastest prograde jet: implications for clouds, dynamics and vertical wind shear

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