Convective storms in closed cyclones in Jupiter: (II) numerical modeling

Iñurrigarro, Peio; Hueso, R.; Sánchez‐Lavega, A.; Legarreta, J.

doi:10.1016/j.icarus.2022.115169

Cited by 6 publications

(2 citation statements)

References 41 publications

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“…Our results, compatible with the range obtained from similar modelling in Visscher et al (2010), indicate marginal agreement with the Juno MWR analysis (Li et al 2020) as discussed above. Cloud models often require one times solar oxygen or higher (Iñurrigarro et al 2022), but can also accommodate subsolar oxygen (Hueso & Sánchez-Lavega 2001). More problematic are the results from lightning data.…”

Section: Discussionmentioning

confidence: 99%

A subsolar oxygen abundance or a radiative region deep in Jupiter revealed by thermochemical modelling

2023

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Jupiter's deep abundances help to constrain the formation history of the planet and the environment of the protoplanetary nebula. Juno recently measured Jupiter's deep oxygen abundance near the equator to be 2.2 +3.9 −2.1 times the protosolar value (2σ uncertainties). Even if the nominal value is supersolar, subsolar abundances cannot be ruled out. Here we use a stateof-the-art one-dimensional thermochemical and diffusion model with updated chemistry to constrain the deep oxygen abundance with upper tropospheric CO observations. We find a value of 0.3 +0.5 −0.2 times the protosolar value. This result suggests that Jupiter could have a carbon-rich envelope that accreted in a region where the protosolar nebula was depleted in water. However, our model can also reproduce a solar/supersolar water abundance if vertical mixing is reduced in a radiative layer where the deep oxygen abundance is obtained. More precise measurements of the deep water abundance are needed to discriminate between these two scenarios and understand Jupiter's internal structure and evolution.

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Section: Discussionmentioning

confidence: 99%

A subsolar oxygen abundance or a radiative region deep in Jupiter revealed by thermochemical modelling

2023

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“…We study whether the GRS could have been generated in a similar way by an energetic moist convective “super‐storm” on Jupiter. We have performed numerical simulations of the response of the Jovian flow at the GRS latitude (∼22° to 24°S) to a localized Gaussian heat injection in EPIC (García‐Melendo et al., 2005; Iñurrigarro et al., 2022) and to a mass injection in the SW (García‐Melendo & Sánchez‐Lavega, 2017; García‐Melendo et al., 2013). Our simulations generate a single oval anticyclone (Figures 3a and 3b, Figures S4–S5 in Supporting Information ) but its length is always smaller than the early GRS (Figures 1c and 1d, Figure 2).…”

Section: Numerical Simulations Resultsmentioning

confidence: 99%

The Origin of Jupiter's Great Red Spot

Sánchez‐Lavega,

García‐Melendo,

Legarreta

et al. 2024

Geophysical Research Letters

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Jupiter's Great Red Spot (GRS) is the largest and longest‐lived known vortex of all solar system planets but its lifetime is debated and its formation mechanism remains hidden. G. D. Cassini discovered in 1665 the presence of a dark oval at the GRS latitude, known as the “Permanent Spot” (PS) that was observed until 1713. We show from historical observations of its size evolution and motions that PS is unlikely to correspond to the current GRS, that was first observed in 1831. Numerical simulations rule out that the GRS formed by the merging of vortices or by a superstorm, but most likely formed from a flow disturbance between the two opposed Jovian zonal jets north and south of it. If so, the early GRS should have had a low tangential velocity so that its rotation velocity has increased over time as it has shrunk.

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The Deep Oxygen Abundance in Solar System Giant Planets, with a New Derivation for Saturn

Cavalié,

Lunine,

Mousis

et al. 2024

Space Sci Rev

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Deep elemental composition is a challenging measurement to achieve in the giant planets of the solar system. Yet, knowledge of the deep composition offers important insights in the internal structure of these planets, their evolutionary history and their formation scenarios. A key element whose deep abundance is difficult to obtain is oxygen, because of its propensity for being in condensed phases such as rocks and ices. In the atmospheres of the giant planets, oxygen is largely stored in water molecules that condense below the observable levels. At atmospheric levels that can be investigated with remote sensing, water abundance can modify the observed meteorology, and meteorological phenomena can distribute water through the atmosphere in complex ways that are not well understood and that encompass deeper portions of the atmosphere. The deep oxygen abundance provides constraints on the connection between atmosphere and interior and on the processes by which other elements were trapped, making its determination an important element to understand giant planets. In this paper, we review the current constraints on the deep oxygen abundance of the giant planets, as derived from observations and thermochemical models.

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Convective storms in closed cyclones in Jupiter: (II) numerical modeling

Cited by 6 publications

References 41 publications

A subsolar oxygen abundance or a radiative region deep in Jupiter revealed by thermochemical modelling

A subsolar oxygen abundance or a radiative region deep in Jupiter revealed by thermochemical modelling

The Origin of Jupiter's Great Red Spot

The Deep Oxygen Abundance in Solar System Giant Planets, with a New Derivation for Saturn

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