Modélisations photochimiques saisonnières des stratosphères de Jupiter et Saturne

One of the goals of this thesis is to interpret the observations of the main hydrocarbons(C2H2 and C2H6) from Cassini (NASA/ESA) on Jupiter and Saturn. The one-dimensional photochemical models are insufficient to explain these spatially resolved observations. I have developed the first two-dimensional (altitude-latitude) seasonal photochemical model for the giant planets, which predicts their chemical composition.Without meridional transport, Saturn’s chemical composition follows the insolation variations. The C2H2 and C2H6 abundances measured by Cassini (Guerlet et al., 2009)are reproduced from the equator up to mid-latitudes, at pressures higher than 0.1mbar.At higher latitudes, the disagreements suggest either a stratospheric circulation cell orthe signature of ion-neutral chemistry. For the first time, I have coupled our seasonal photochemical model with the seasonal radiative model of Greathouse et al. (2008). I predict that the seasonal temperature peak is shifted half a season earlier, with respect to previous models, at high latitudes in the higher stratosphere.Jupiter shows weak seasonal variations of chemical composition, only controlled by its orbital eccentricity. The observed meridional distributions of C2H2 and C2H6 show opposition trends (Nixon et al., 2010). C2H6 observed distribution is reproduced when Isuppose a combination of meridional diffusion and stratospheric circulation, while causingat the same time a stronger agreement with the C2H2 observations. Accounting for theion-neutral chemistry might preferentially affect C2H2 and potentially play a key role on hydrocarbon abundances in Jupiter’s stratosphere.L’un des objectifs de cette thèse est d’interpréter les observations des principaux hydrocarbures(C2H2 et C2H6) effectuées par Cassini (NASA/ESA) sur Jupiter et Saturne. Les modèles photochimiques à une dimension sont insuffisants pour interpréter ces observations spatialement résolues. J’ai développé le premier modèle photochimique saisonnier à deux dimensions (altitude-latitude) des planètes géantes qui calcule leur composition chimique.En l’absence de transport méridional, la composition chimique de Saturne suit les variations d’ensoleillement. Les abondances de C2H2 et C2H6 mesurées par Cassini (Guerletet al., 2009) sont reproduites jusqu’aux latitudes moyennes, à des pressions supérieures à0,1mbar. Les écarts notés dans l’hémisphère sud suggèrent la présence de dynamique ou d’une chimie entre les ions et les espèces neutres. J’ai couplé, pour la première fois, mon modèle photochimique avec le modèle radiatif de Greathouse et al. (2008). Nous prédisons un décalage du pic saisonnier de température, par rapport aux précédents modèles, d’une demi-saison à haute altitude et aux hautes latitudes.Jupiter présente de faibles variations saisonnières de composition chimique, uniquement contrôlées par son excentricité. Les distributions méridionales observées de C2H2 etC2H6 présentent des tendances opposées (Nixon et al., 2010). Mon modèle est en accord avec les observations de C2H6 lorsque j’invoque une combinaison de diffusion méridionale et de circulation stratosphérique, tout en provoquant un plus grand désaccord avec les observations de C2H2. La chimie ionique pourrait principalement affecter C2H2 et jouer un rôle important dans l’atmosphère de Jupiter

0341: AMPK exerts an insulin-sensitizing effect on cardiac glucose uptake by multiple molecular mechanisms including cytoskeleton reorganization

BackgroundInsulin-resistant cardiomyocytes are characterized by a decreased ability of insulin to stimulate glucose uptake. We have previously shown that the activation of AMPK by metformin or phenformin restores insulin-sensitivity in insulin-resistant cardiomyocytes. The aim of our present work is to understand by which molecular mechanisms AMPK exerts its insulin sensitizing effect. In this study we focused on the mTOR/p70S6K pathway and on cytoskeleton reorganization. mTOR/p70S6K, which is known to be inhibited by AMPK, is able to reduce insulin signaling via a negative feedback loop involving serine phosphorylation of IRS-1. On the other hand, cytoskeleton reorganization, which is a known target of AMPK, is responsible for the translocation of the glucose transporter GLUT4 to the plasma membrane.MethodsAdult rat cardiomyocytes were primary cultured and treated with different agents including insulin, AMPK activator (phenformin), mTOR inhibitor rapamycin and/or actin cytoskeleton inhibitor latrunculin B. Glucose uptake was assessed by detritiation of 2-3H-glucose.ResultsFirst, we tested if rapamycin was able to mimic AMPK activators. Similarly to phenformin, rapamycin increased the insulin-dependent phosphorylation of Akt involved in the regulation of glucose uptake. Despite the ability of rapamycin to induce this Akt over-phosphorylation, rapamycin was not able to restore the insulin-dependent stimulation of glucose uptake like phenformin did. On the other hand, latrunculin B abolished the insulin-sensitizing action of phenformin on glucose uptake, in insulin-sensitive as well as in insulinresistant cells.Conclusionsactin cytoskeleton reorganization but not mTOR/p70S6K, is involved in the insulin-sensitizing effect of AMPK on cardiac glucose uptake. The role played by Small G proteins, known to be involved in the regulation of actin cytoskeleton is under investigation

Enhanced C2_2H2_2 absorption within Jupiter's southern auroral oval from Juno UVS observations

Reflected sunlight observations from the Ultraviolet Spectrograph (UVS) on the Juno spacecraft were used to study the distribution of acetylene (C$_2$H$_2$) at Jupiter's south pole. We find that the shape of the C$_2$H$_2$ absorption feature varies significantly across the polar region, and this can be used to infer spatial variability in the C$_2$H$_2$ abundance. There is a localized region of enhanced C$_2$H$_2$ absorption which coincides with the location of Jupiter's southern polar aurora; the C$_2$H$_2$ abundance poleward of the auroral oval is a factor of 3 higher than adjacent quiescent, non-auroral longitudes. This builds on previous infrared studies which found enhanced C$_2$H$_2$ abundances within the northern auroral oval. This suggests that Jupiter's upper-atmosphere chemistry is being strongly influenced by the influx of charged auroral particles and demonstrates the necessity of developing ion-neutral photochemical models of Jupiter's polar regions.Comment: Accepted in JGR: Planet

The complex behavior of the satellite footprints at Jupiter: the result of universal processes?

At Jupiter, some auroral emissions are directly related to the electromagnetic interaction between the moons Io, Europa and Ganymede on one hand and the rapidly rotating magnetospheric plasma on the other hand. Out of the three, the Io footprint is the brightest and the most studied. Present in each hemisphere, it is made of at least three different spots and an extended trailing tail. The variability of the brightness of the spots as well as their relative location has been tentatively explained with a combination of Alfvén waves’ partial reflections on density gradients and bi-directional electron acceleration at high latitude. Should this scenario be correct, then the other footprints should also show the same behavior. Here we show that all footprints are, at least occasionally, made of several spots and they all display a tail. We also show that these spots share many characteristics with those of the Io footprint (i.e. some significant variability on timescales of 2-3 minutes). Additionally, we present some Monte-Carlo simulations indicating that the tails are also due to Alfvén waves electron acceleration rather than quasi-static electron acceleration. Even if some details still need clarification, these observations strengthen the scenario proposed for the Io footprint and thus indicate that these processes are universal. In addition, we will present some early results from Juno-UVS concerning the location and morphology of the footprints during the first low-altitude observations of the polar aurorae. These observations, carried out in previously unexplored longitude ranges, should either confirm or contradict our understanding of the footprints

Possible Transient Luminous Events observed in Jupiter's upper atmosphere

11 transient bright flashes were detected in Jupiter's atmosphere using the UVS instrument on the Juno spacecraft. These bright flashes are only observed in a single spin of the spacecraft and their brightness decays exponentially with time, with a duration of ~1.4 ms. The spectra are dominated by H2 Lyman band emission and based on the level of atmospheric absorption, we estimate a source altitude of 260 km above the 1-bar level. Based on these characteristics, we suggest that these are observations of Transient Luminous Events (TLEs) in Jupiter's upper atmosphere. In particular, we suggest that these are elves, sprites or sprite halos, three types of TLEs that occur in the Earth's upper atmosphere in response to tropospheric lightning strikes. This is supported by visible light imaging, which shows cloud features typical of lightning source regions at the locations of several of the bright flashes. TLEs have previously only been observed on Earth, although theoretical and experimental work has predicted that they should also be present on Jupiter.Comment: Accepted in JGR: Planets. 28 pages, 8 figure

Spatial Variations in the Altitude of the CH4 Homopause at Jupiter's Mid-to-high Latitudes, as Constrained from IRTF-TEXES Spectra

Peer reviewedPublisher PD

The Io, Europa and Ganymede auroral footprints at Jupiter in the ultraviolet: positions and equatorial lead angles

Jupiter's satellite auroral footprints are a consequence of the interaction between the Jovian magnetic field with co-rotating iogenic plasma and the Galilean moons. The disturbances created near the moons propagate as Alfv\'en waves along the magnetic field lines. The position of the moons is therefore "Alfv\'enically" connected to their respective auroral footprint. The angular separation from the instantaneous magnetic footprint can be estimated by the so-called lead angle. That lead angle varies periodically as a function of orbital longitude, since the time for the Alfv\'en waves to reach the Jovian ionosphere varies accordingly. Using spectral images of the Main Alfv\'en Wing auroral spots collected by Juno-UVS during the first forty-three orbits, this work provides the first empirical model of the Io, Europa and Ganymede equatorial lead angles for the northern and southern hemispheres. Alfv\'en travel times between the three innermost Galilean moons to Jupiter's northern and southern hemispheres are estimated from the lead angle measurements. We also demonstrate the accuracy of the mapping from the Juno magnetic field reference model (JRM33) at the completion of the prime mission for M-shells extending to at least 15RJ . Finally, we shows how the added knowledge of the lead angle can improve the interpretation of the moon-induced decametric emissions.Comment: 20 pages, 8 figures, Accepted for publication in Journal of Geophysical Research: Space Physics on 20 April 202

Quantification of diffuse auroral electron precipitation driven by whistler mode waves at Jupiter

While previous studies suggested whistler mode waves as a potential driver of Jupiter's diffuse aurora, their quantitative contribution to generate diffuse aurora remains unclear. We perform an in-depth analysis of an intriguing diffuse auroral electron precipitation event using coordinated observations of precipitating electrons and whistler mode waves from the Juno satellite. A physics-based technique is used to quantify energetic electron precipitation driven by whistler mode waves. We find that the modeled electron precipitation features are consistent with the electron measurements from several keV to several hundred keV over M-shells of 8–18, while additional mechanisms are needed to explain the observed electron precipitation at lower energies (<several keV). Our result provides new quantitative evidence that whistler mode waves are potentially a primary driver of precipitating electrons from several keV to several hundred keV through pitch angle scattering over M ∼ 8–18 and thus generate Jupiter's diffuse aurora.Accepted manuscrip

An intense narrow equatorial jet in Jupiter’s lower stratosphere observed by JWST

The atmosphere of Jupiter has east–west zonal jets that alternate as a function of latitude as tracked by cloud motions at tropospheric levels. Above and below the cold tropopause at ~100 mbar, the equatorial atmosphere is covered by hazes at levels where thermal infrared observations used to characterize the dynamics of the stratosphere lose part of their sensitivity. James Webb Space Telescope observations of Jupiter in July 2022 show these hazes in higher detail than ever before and reveal the presence of an intense (140 m s−1) equatorial jet at 100–200 mbar (70 m s−1 faster than the zonal winds at the cloud level) that is confined to ±3° of the equator and is located below stratospheric thermal oscillations that extend at least from 0.1 to 40 mbar and repeat in multiyear cycles. This suggests that the new jet is a deep part of Jupiter’s Equatorial Stratospheric Oscillation and may therefore vary in strength over time.JWST-ERS-01373, NASA/ESA Hubble Space Telescope programmes no. 16913, 15502 and 16790, PID2019-109467GB-I00 funded by MCIN/AEI/10.13039/501100011033/, Grupos Gobierno Vasco IT1742-22. I.d.; European Research Council Consolidator Grant (under the European Union’s Horizon 2020 research and innovation programme, grant agreement no. 723890), STFC PhD Studentship, NASA grants 80NSSC21K1418 and 80NSSC19K0894

Evidence for inhibition of cholinesterases in insect and mammalian nervous systems by the insect repellent deet

<p>Abstract</p> <p>Background</p> <p>N,N-Diethyl-3-methylbenzamide (deet) remains the gold standard for insect repellents. About 200 million people use it every year and over 8 billion doses have been applied over the past 50 years. Despite the widespread and increased interest in the use of deet in public health programmes, controversies remain concerning both the identification of its target sites at the olfactory system and its mechanism of toxicity in insects, mammals and humans. Here, we investigated the molecular target site for deet and the consequences of its interactions with carbamate insecticides on the cholinergic system.</p> <p>Results</p> <p>By using toxicological, biochemical and electrophysiological techniques, we show that deet is not simply a behaviour-modifying chemical but that it also inhibits cholinesterase activity, in both insect and mammalian neuronal preparations. Deet is commonly used in combination with insecticides and we show that deet has the capacity to strengthen the toxicity of carbamates, a class of insecticides known to block acetylcholinesterase.</p> <p>Conclusion</p> <p>These findings question the safety of deet, particularly in combination with other chemicals, and they highlight the importance of a multidisciplinary approach to the development of safer insect repellents for use in public health.</p