Characterization of Mesoscale Waves in the Jupiter NEB by Jupiter InfraRed Auroral Mapper on board Juno

Adriani, A.; Moriconi, M. L.; Altieri, F.; Sindoni, G.; Ingersoll, Andrew P.; Grassi, D.; Mura, A.; Atreya, S. K.; Orton, Glenn S.; Lunine, Jonathan I.; Fletcher, Leigh N.; Simon-Miller, A. A.; Melin, Henrik; Tosi, F.; Cicchetti, A.; Noschese, R.; Sordini, R.; Levin, S. M.; Bolton, J. G.; Plainaki, C.; Olivieri, A.

doi:10.3847/1538-3881/aae525

Cited by 6 publications

(3 citation statements)

References 42 publications

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“…The CPCs and PCs revealed by Juno (Adriani et al. 2018a ) challenge our understanding of Jupiter’s polar domain - an octagonal arrangement at the north pole, and a pentagonal (sometimes hexagonal) arrangement at the south pole, whose long-term stability reveals the dynamics of atmospheric turbulence and the ‘beta-drift’ of cyclones (Gavriel and Kaspi 2021 ). The inclined phase of JUICE, with sub-spacecraft latitude reaching up to 33 ∘ , will provide a new glimpse of the polar domain, with its FFRs and polar cyclones, several years after the culmination of the Juno mission.…”

Section: Jupiter Scientific Objectivesmentioning

confidence: 99%

Jupiter Science Enabled by ESA’s Jupiter Icy Moons Explorer

Fletcher,

Cavalié,

Grassi

et al. 2023

Space Sci Rev

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ESA’s Jupiter Icy Moons Explorer (JUICE) will provide a detailed investigation of the Jovian system in the 2030s, combining a suite of state-of-the-art instruments with an orbital tour tailored to maximise observing opportunities. We review the Jupiter science enabled by the JUICE mission, building on the legacy of discoveries from the Galileo, Cassini, and Juno missions, alongside ground- and space-based observatories. We focus on remote sensing of the climate, meteorology, and chemistry of the atmosphere and auroras from the cloud-forming weather layer, through the upper troposphere, into the stratosphere and ionosphere. The Jupiter orbital tour provides a wealth of opportunities for atmospheric and auroral science: global perspectives with its near-equatorial and inclined phases, sampling all phase angles from dayside to nightside, and investigating phenomena evolving on timescales from minutes to months. The remote sensing payload spans far-UV spectroscopy (50-210 nm), visible imaging (340-1080 nm), visible/near-infrared spectroscopy (0.49-5.56 μm), and sub-millimetre sounding (near 530-625 GHz and 1067-1275 GHz). This is coupled to radio, stellar, and solar occultation opportunities to explore the atmosphere at high vertical resolution; and radio and plasma wave measurements of electric discharges in the Jovian atmosphere and auroras. Cross-disciplinary scientific investigations enable JUICE to explore coupling processes in giant planet atmospheres, to show how the atmosphere is connected to (i) the deep circulation and composition of the hydrogen-dominated interior; and (ii) to the currents and charged particle environments of the external magnetosphere. JUICE will provide a comprehensive characterisation of the atmosphere and auroras of this archetypal giant planet.

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Section: Jupiter Scientific Objectivesmentioning

confidence: 99%

Jupiter Science Enabled by ESA’s Jupiter Icy Moons Explorer

Fletcher,

Cavalié,

Grassi

et al. 2023

Space Sci Rev

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“…Understanding and characterizing the variability of Jupiter's belts and zones has been the focus of a large number of studies, with particular interest in tracking and characterizing evolving waves (e.g., Adriani et al., 2018; Fletcher, Melin, et al., 2018; Sánchez‐Lavega et al., 2017; Simon et al., 2015, 2018) and storms (e.g., Hueso et al., 2002; Iñurrigarro et al., 2020; Sánchez‐Lavega et al., 2008, 2017) that trigger some of the most dramatic changes in Jupiter's atmosphere, such as the South Equatorial Belt (SEB, at 7°–17°S planetocentric latitude (all latitudes in this study are planetocentric)) revivals (Fletcher et al., 2011; Fletcher, Orton, Rogers, et al., 2017; Pérez‐Hoyos et al., 2012; Sánchez‐Lavega & Gómez, 1996), the North Temperate Belt (NTB, 21°–28°N latitude) disturbances (Barrado‐Izagirre et al., 2009; Sánchez‐Lavega et al., 2008, 2017), and the North Equatorial Belt (NEB, 7°–17°N) expansions (Fletcher, Orton, Sinclair, et al., 2017; García‐Melendo & Sánchez‐Lavega, 2001; Rogers, 1995; Simon‐Miller et al., 2001). Some of these changes appear to be repeatable and potentially cyclic in nature (e.g., Fletcher, 2017).…”

Section: Introductionmentioning

confidence: 99%

Jupiter's Multi‐Year Cycles of Temperature and Aerosol Variability From Ground‐Based Mid‐Infrared Imaging

Antuñano,

Fletcher,

Orton

et al. 2023

JGR Planets

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We use a long‐term record of ground‐based mid‐infrared (7.9–24.5 μm) observations, captured between 1984 and late 2019 from 3‐m and 8‐m class observatories (mainly NASA's Infrared Telescope Facility, ESO's Very Large Telescope, and the Subaru Telescope), to characterize the long‐term, multi‐decade variability of the thermal and aerosol structure in Jupiter's atmosphere. In this study, spectral cubes assembled from images in multiple filters are inverted to provide estimations of stratospheric and tropospheric temperatures and tropospheric aerosol opacity. We find evidence of non‐seasonal and quasi‐seasonal variations of the stratospheric temperatures at 10 mbar, with a permanent hemispherical asymmetry at mid‐latitudes, where the northern mid‐latitudes are overall warmer than southern mid‐latitudes. A correlation analysis between stratospheric and tropospheric temperature variations reveals a moderate anticorrelation between the 10‐mbar and 330‐mbar temperatures at the equator, revealing that upper‐tropospheric equatorial temperatures are coupled to Jupiter’s Equatorial Stratospheric Oscillation. The North and South Equatorial Belts show temporal variability in their aerosol opacity and tropospheric temperatures that are in approximate antiphase with one another, with moderate negative correlations in the North Equatorial Belt and South Equatorial Belt changes between conjugate latitudes at 10°–16°. This long‐term anticorrelation between belts separated by ∼15° is still not understood. Finally we characterize the lag between thermal and aerosol opacity changes at a number of latitudes, finding that aerosol variations tend to lag after thermal variations by around 6 months at multiple latitudes.

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“…We have used JunoCam's coverage over a wide range of latitudes, coupled with its high spatial resolving power, to examine all of our images for various phenomena in Jupiter's clouds. Small‐scale waves, with wavelengths (distances between wave crests) less than ~300 km, were first detected in 1979 by Voyager (Hunt & Muller, 1979) and have been detected by Galileo (e.g., Bosak & Ingersoll, 2002) and New Horizons (e.g., Reuter et al, 2007) since then, as well as by the near‐infrared JIRAM instrument on Juno (Adriani et al, 2018; Fletcher et al, 2018). Larger waves, with scales of 1,200 km or greater, have since also been detected from the Earth using Hubble Space Telescope (HST) and ground‐based imaging (Simon et al, 2018).…”

Section: Introductionmentioning

confidence: 99%

A Survey of Small‐Scale Waves and Wave‐Like Phenomena in Jupiter's Atmosphere Detected by JunoCam

et al. 2020

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In the first 20 orbits of the Juno spacecraft around Jupiter, we have identified a variety of wave‐like features in images made by its public‐outreach camera, JunoCam. Because of Juno's unprecedented and repeated proximity to Jupiter's cloud tops during its close approaches, JunoCam has detected more wave structures than any previous surveys. Most of the waves appear in long wave packets, oriented east‐west and populated by narrow wave crests. Spacing between crests were measured as small as ~30 km, shorter than any previously measured. Some waves are associated with atmospheric features, but others are not ostensibly associated with any visible cloud phenomena and thus may be generated by dynamical forcing below the visible cloud tops. Some waves also appear to be converging, and others appear to be overlapping, possibly at different atmospheric levels. Another type of wave has a series of fronts that appear to be radiating outward from the center of a cyclone. Most of these waves appear within 5° of latitude from the equator, but we have detected waves covering planetocentric latitudes between 20°S and 45°N. The great majority of the waves appear in regions associated with prograde motions of the mean zonal flow. Juno was unable to measure the velocity of wave features to diagnose the wave types due to its close and rapid flybys. However, both by our own upper limits on wave motions and by analogy with previous measurements, we expect that the waves JunoCam detected near the equator are inertia‐gravity waves.

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Characterization of Mesoscale Waves in the Jupiter NEB by Jupiter InfraRed Auroral Mapper on board Juno

Cited by 6 publications

References 42 publications

Jupiter Science Enabled by ESA’s Jupiter Icy Moons Explorer

Jupiter Science Enabled by ESA’s Jupiter Icy Moons Explorer

Jupiter's Multi‐Year Cycles of Temperature and Aerosol Variability From Ground‐Based Mid‐Infrared Imaging

A Survey of Small‐Scale Waves and Wave‐Like Phenomena in Jupiter's Atmosphere Detected by JunoCam

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