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Jupiter's Great Red Spot (GRS) was mapped by the James Webb Space Telescope (JWST)/Mid‐Infrared Instrument (4.9–27.9 μ ${\upmu }$m) in July and August 2022. These observations took place alongside a suite of visual and infrared observations from; Hubble, JWST/NIRCam, Very Large Telescope/VISIR and amateur observers which provided both spatial and temporal context across the jovian disc. The stratospheric temperature structure retrieved using the NEMESIS software revealed a series of hot‐spots above the GRS. These could be the consequence of GRS‐induced wave activity. In the troposphere, the temperature structure was used to derive the thermal wind structure of the GRS vortex. These winds were only consistent with the independently determined wind field by JWST/NIRCam at 240 mbar if the altitude of the Hubble‐derived winds were located around 1,200 mbar, considerably deeper than previously assumed. No enhancement in ammonia was found within the GRS but a link between elevated aerosol and phosphine abundances was observed within this region. North‐south asymmetries were observed in the retrieved temperature, ammonia, phosphine and aerosol structure, consistent with the GRS tilting in the north‐south direction. Finally, a small storm was captured north‐west of the GRS that displayed a considerable excess in retrieved phosphine abundance, suggestive of vigorous convection. Despite this, no ammonia ice was detected in this region. The novelty of JWST required us to develop custom‐made software to resolve challenges in calibration of the data. This involved the derivation of the "FLT‐5" wavelength calibration solution that has subsequently been integrated into the standard calibration pipeline. Plain Language Summary: Regularly observed for over 150 years, Jupiter's Great Red Spot (GRS) is one of the best documented storms in the Solar System. Despite the frequency of observations, crucial questions remain unanswered regarding the internal composition, dynamics and driving mechanism for the storm. Mid‐infrared observations acquired by the James Webb Space Telescope allowed us to peer past the colorful clouds to assess the composition and dynamics of the jovian weather layer. Data from the mid‐infrared instrument was modeled in the 7.30–10.75 μ ${\upmu }$m range to "retrieve" the temperature distribution. Further modeling of these temperatures allowed us to derive the wind speeds throughout the vortex, enabling us to assess the dynamics of the GRS and how the vortex interacts with its surroundings. In addition, a series of hot‐spots were observed above the GRS that could be the result of atmospheric wave activity. The distribution of ammonia was also mapped in this spectral range. Comparison of the distribution of ammonia to the cloud distribution implied that this molecule may condense into the thick layers of cloud above the GRS. Finally phosphine, indicative of upwelling air was mapped and allowed us to identify a small convective storm north‐west of the GRS. Key Points: Jupiter's Great Red Spot (GRS) was observed by James Webb Space Telescope/Mid‐Infrared Instrument in 2022 to study the 3D structure of temperature, aerosols and gaseous speciesA series of stratospheric hot‐spots were discovered to be co‐moving with the GRS in the longitude directionElevated phosphine and a complex distribution of ammonia gas were observed inside the GRS [ABSTRACT FROM AUTHOR]

Jupiter's South Polar Region (SPR) was observed by James Webb Space Telescope/Mid‐Infrared Instrument in December 2022. We used the Medium Resolution Spectrometer mode to provide new information about Jupiter's South Polar stratosphere. The southern auroral region was visible and influenced the atmosphere in several ways: (a) In the interior of the southern auroral oval, we retrieved peak temperatures at two distinct pressure levels near 0.01 and 1 mbar, with warmer temperatures with respect to non‐auroral regions of 12 ± 2 K and 37 ± 4 K respectively. A cold polar vortex is centered at 65°S at 10 mbar. (b) We found that the homopause is elevated to 590−118+25 ${590}_{-118}^{+25}$ km above the 1‐bar pressure level inside the auroral oval compared to 460−50+60 ${460}_{-50}^{+60}$ km at neighboring latitudes and with an upper altitude of 350 km in regions not affected by auroral precipitation. (c) The retrieved abundance of C2H2 shows an increase within the auroral oval, and it exhibits high abundances throughout the polar region. The retrieved abundance of C2H6 increases toward the pole, without being localized in the auroral oval, in contrast with previous analysis (Sinclair et al., 2018, https://doi.org/10.1016/j.icarus.2017.09.016). We determined that the warming at 0.01 mbar and the elevated homopause might be caused by the flux of charged particles depositing their energy in the SPR. The 1‐mbar hotspot may arise from adiabatic heating resulting from auroral‐driven downwelling. The cold region at 10 mbar may be caused by radiative cooling by stratospheric aerosols. The differences in spatial distribution seem to indicate that the hydrocarbons analyzed are affected differently by auroral precipitation. Plain Language Summary: James Webb Space Telescope/Mid‐Infrared instrument observed Jupiter's south polar region in December 2022. The instrument acquired spectroscopic data in the mid‐infrared part of the spectrum, which is sensitive to the temperature of the atmosphere and the chemical abundances. These observations revealed that within the auroral oval there are two regions of high temperatures located at two different altitudes. These are presumably caused by two different phenomena: direct heating from the incoming charged particles in the aurora at a height of 0.01 mbar and adiabatic heating in downdrafts at lower levels. A decrease in temperature was also observed as we approached the South Pole, probably caused by a cold polar vortex associated with stratospheric hazes. We found that the altitude of the homopause (the limit between the well‐mixed part of the atmosphere and the part where molecules are separated according their specific weight) is altered by the auroras, being up to 100 km higher in the auroral region. The atmospheric abundances of acetylene and ethane showed an enrichment of acetylene within the auroral oval, and of ethane at the pole, which may indicate that these molecules are not affected in the same way by the energy input of the aurora. Key Points: The homopause is spatially variable within the polar region and highest within the auroral ovalThe atmosphere inside the Southern Auroral Oval at 1 and 0.01 mbar shows a warming compared with non‐auroral regionsThe C2H2 abundance is enhanced inside the Southern Auroral Oval at 0.1 and 7 mbar, and C2H6 shows an increase polewards [ABSTRACT FROM AUTHOR]

Using images at multiple mid‐infrared wavelengths, acquired in 2018 May using the Very Large Telescope Imager and Spectrometer (VISIR) instrument on ESO's Very Large Telescope (VLT), we study Jupiter's pole‐to‐pole thermal, chemical and aerosol structure in the troposphere and stratosphere. We confirm that the pattern of cool and cloudy anticyclonic zones and warm cloud‐free cyclonic belts persists throughout the mid‐latitudes, up to the polar boundaries, and evidence a strong correlation with the vertical maximum windshear and the locations of Jupiter's zonal jets. At high latitudes, VISIR images reveal a large region of mid‐infrared cooling poleward ∼64°N and ∼67°S extending from the upper troposphere to the stratosphere, co‐located with the reflective aerosols observed by JunoCam, and suggesting that aerosols play a key role in the radiative cooling at the poles. Comparison of zonal‐mean thermal properties and high‐resolution visible imaging from Juno allows us to study the variability of atmospheric properties as a function of altitude and jet boundaries, particularly in the cold southern polar vortex. However, the southern stratospheric polar vortex is partly masked by a warm mid‐infrared signature of the aurora. Co‐located with the southern main auroral oval, this warming results from the auroral precipitation and/or joule heating which heat the atmosphere and thus cause a significant stratospheric emission. This high emission results from a large enhancement of both ethane and acetylene in the polar region, reinforcing the evidence of enhanced ion‐related chemistry in Jupiter's auroral regions. Plain Language Summary: A fundamental inquiry driving NASA's Juno mission was the investigation of the potential changes of Jupiter's famous banded structure below the top most clouds. As NASA's Juno spacecraft lacks instrumentation sensitive to the mid‐infrared, we have used the ground‐based Very Large Telescope Imager and Spectrometer (VISIR) on ESO's Very Large Telescope (VLT) to support the mission since 2016. The 2018 May data set provides a comprehensive view of Jupiter's pole‐to‐pole thermal, chemical, and aerosol structure; including the Great Red Spot; and the auroral‐related heating in the southern polar stratosphere. We show that the alternating pattern of cool cloudy zones and warm cloud‐free belts correlate to the zonal winds locations, extends from the equator to the boundary of the polar vortices (∼64°N and ∼67°S). Comparing this ground‐based data set with Juno observations, we show that the polar regions experience radiative cooling from the upper troposphere to the stratosphere, probably induced by the reflective polar aerosols, and confined at the poles by the polar vortices. However, the southern stratospheric polar vortex is partly masked by a large auroral emission, a signature of an interaction between the magnetosphere and stratosphere of Jupiter, which causes a ∼20 K warming as deep as the middle stratosphere. Excess hydrocarbons within the polar domain reinforces the evidence of enhanced ion‐related chemistry in Jupiter's auroral regions, resulting from charged particles precipitating from the top of the atmosphere to lower altitudes. Key Points: Jupiter's belt/zone thermal structure extends from the equator to the edge of the polar vortices and correlates with the zonal jetsThe cold polar vortices coincides with reflective aerosols, suggesting dynamical entrainment by the northernmost and southernmost jetsTemporal evolution of the southern auroral hotspot shows a stratospheric cooling after a solar wind compression event [ABSTRACT FROM AUTHOR]

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. Plain Language Summary: Jupiter's atmosphere displays a wide variety of perturbations in its temperatures, clouds and aerosols. In this study, we use a large set of ground‐based observations captured in the mid‐infrared between 1984 and 2019 to characterize long‐term changes in the temperatures and aerosols. This long‐term analysis show a number of cyclic disturbances, and allows us to distinguish between seasonal and non‐seasonal changes in Jupiter's atmosphere. In particular, we observe that the northern mid‐latitudes above 30° are continuously warmer than their counterpart latitudes in the south at 10 mbar pressure level (the stratosphere), potentially due to differences in the polar haze in Jupiter, which extends to lower latitudes in the north compared to the south. Additionally, our study reveals for the first time that the thermal oscillation present in Jupiter's equatorial stratosphere at the 10‐mbar pressure level (known as Jupiter's Equatorial Stratospheric Oscillation) is also observed to descend to higher pressures (330 mbar), meaning that it is not confined to the stratosphere. Finally, we also discuss the lag between temperature and aerosol changes at diverse latitudes to try to identify the mechanisms responsible for the different atmospheric disturbances observed on Jupiter. Key Points: Ground‐based multi‐wavelength images are used to compute stratospheric and tropospheric temperature and tropospheric aerosol opacity mapsResults reveal that upper‐tropospheric equatorial temperatures are coupled to Jupiter's Equatorial Stratospheric OscillationStratospheric temperatures at 10 mbar show a permanent hemispherical asymmetry at mid‐latitudes, with northern mid‐latitudes overall warmer than their counterparts [ABSTRACT FROM AUTHOR]

Hubble Space Telescope Wide‐Field Camera 3 (HST/WFC3) observations spanning 2015 to 2021 confirm a brightening of Uranus' north polar hood feature with time. The vertical aerosol model of Irwin et al. (2023, https://doi.org/10.1038/s41550-023-02047-0) (IRW23), consisting of a deep haze layer based at ∼5 bar, a 1–2 bar haze layer, and an extended haze rising up from the 1–2 bar layer, was applied to retrievals on HST Space Telescope Imaging Spectrograph (STIS) (HST/STIS) observations (Sromovsky et al., 2014, 2019, https://doi.org/10.1016/j.icarus.2014.05.016, https://doi.org/10.1016/j.icarus.2018.06.026) revealing a reduction in cloud‐top CH4 volume mixing ratio (VMR) (i.e., above the deep ∼5 bar haze) by an average of 0.0019 ± 0.0003 between 40–80◦N (∼10% average reduction) from 2012 to 2015. A combination of latitudinal retrievals on the HST/WFC3 and HST/STIS data sets, again employing the IRW23 model, reveal a temporal thickening of the 1–2 bar haze layer to be the main cause of the polar hood brightening, finding an average increase in integrated opacity of 1.09 ± 0.08 (∼33% increase) at 0.8 µm north of ∼45°N, concurrent with a decrease in the imaginary refractive index spectrum of the 1–2 bar haze layer north of ∼40°N and longwards of ∼0.7 µm. Small contributions to the brightening were found from a thickening of the deep aerosol layer, with an average increase in integrated opacity of 0.6 ± 0.1 (58% increase) north of 45°N between 2012 and 2015, and from the aforementioned decrease in CH4 VMR. Our results are consistent with the slowing of a stratospheric meridional circulation, exhibiting subsidence at the poles. Plain Language Summary: Uranus' north polar hood—a bright cap‐like feature encircling the northern polar region within its atmosphere—is observed to be brightening over time. Using several observations of Uranus captured between 2012 and 2021 by the Hubble Space Telescope, this study aims to pinpoint, for the first time, the specific changes occurring within the atmosphere leading to this evolution. Analysis of the observations confirmed the predominant cause of the hood's brightening to be changes in the scattering properties of the atmosphere's aerosol layers. A vertical aerosol model consisting of 3 distinct haze layers was employed to investigate these changes. We find that the hood's brightening mainly stems from changes in the middle haze layer in the model (centered at 1–2 bar), finding a thickening of this layer concurrent with an increase in the reflectivity of its aerosols over time at latitudes coincident with the north polar hood (∼45–90°N). Small contributions to the temporal brightening were also found from a ∼10% reduction in cloud‐top methane and a thickening of the deepest haze layer in the model (centered at ∼5 bar) at north polar hood latitudes. Key Points: We confirm that the brightening of Uranus' north polar hood is predominantly due to changes in aerosol scatteringA temporal thickening and increase in aerosol reflectivity of Irwin et al. (2023, https://doi.org/10.1038/s41550-023-02047-0)'s 1–2 bar haze is the main cause of the brighteningWe find a further reduction in polar cloud‐top methane over time from retrievals carried out on Hubble Space Telescope's/Space Telescope Imaging Spectrograph observations [ABSTRACT FROM AUTHOR]

Saturn's northern summertime hemisphere was mapped by JWST/Mid‐Infrared Instrument (4.9–27.9 µm) in November 2022, tracing the seasonal evolution of temperatures, aerosols, and chemical species in the 5 years since the end of the Cassini mission. The spectral region between reflected sunlight and thermal emission (5.1–6.8 µm) is mapped for the first time, enabling retrievals of phosphine, ammonia, and water, alongside a system of two aerosol layers (an upper tropospheric haze p < 0.3 bars, and a deeper cloud layer at 1–2 bars). Ammonia displays substantial equatorial enrichment, suggesting similar dynamical processes to those found in Jupiter's equatorial zone. Saturn's North Polar Stratospheric Vortex has warmed since 2017, entrained by westward winds at p < 10 mbar, and exhibits localized enhancements in several hydrocarbons. The strongest latitudinal temperature gradients are co‐located with the peaks of the zonal winds, implying wind decay with altitude. Reflectivity contrasts at 5–6 µm compare favorably with albedo contrasts observed by Hubble, and several discrete vortices are observed. A warm equatorial stratospheric band in 2022 is not consistent with a 15‐year repeatability for the equatorial oscillation. A stacked system of windshear zones dominates Saturn's equatorial stratosphere, and implies a westward equatorial jet near 1–5 mbar at this epoch. Lower stratospheric temperatures, and local minima in the distributions of several hydrocarbons, imply low‐latitude upwelling and a reversal of Saturn's interhemispheric circulation since equinox. Latitudinal distributions of stratospheric ethylene, benzene, methyl, and carbon dioxide are presented for the first time, and we report the first detection of propane bands in the 8–11 µm region. Plain Language Summary: The Saturn system, with its seasonally varying atmosphere, delicate rings, and myriad satellites, presented an ideal early target for JWST. Saturn's extended disc, rapid rotation, and infrared brightness provided a challenge for the small fields‐of‐view of the Mid‐Infrared Instrument (MIRI), requiring a mosaic to map Saturn's northern summertime hemisphere. This exquisite data set reveals Saturn's banded structure, discrete vortices, the warm polar vortices, and the continued evolution of an oscillatory pattern of warm and cool anomalies over Saturn's equator. We show evidence that a stratospheric circulation pattern detected by Cassini during northern winter has now fully reversed in northern summer, with the low‐latitude stratosphere being cool and depleted in aerosols due to summertime upwelling. MIRI provides access to spectral regions that were not possible with the Cassini spacecraft, particularly in the 5–7 μm region where reflected sunlight and thermal emission blend together. Ammonia and phosphine are enriched at Saturn's equator, suggesting strong mixing from the deeper troposphere. MIRI's high sensitivity enables the first identification of previously unseen emission propane bands, along with the first measurements of the distribution of several gaseous species: tropospheric water, and stratospheric ethylene, benzene, methyl, and carbon dioxide. Key Points: Saturn's northern summertime hemisphere was mapped by JWST/Mid‐Infrared Instrument (MIRI) to study seasonal evolution of temperatures, aerosols, and compositionThe data show evidence for changing temperatures and winds in the equatorial oscillation, polar vortices, and interhemispheric stratospheric circulationMIRI spectral coverage and sensitivity enables mapping of several gases for the first time, particularly in ranges inaccessible to Cassini [ABSTRACT FROM AUTHOR]

Objective: Improve data‐driven research to inform clinical decision‐making with pediatric epilepsy surgery patients by expanding the Pediatric Epilepsy Research Consortium Epilepsy Surgery (PERC‐Surgery) Workgroup to include neuropsychological data. This article reports on the process and initial success of this effort and characterizes the cognitive functioning of the largest multi‐site pediatric epilepsy surgery cohort in the United States. Methods: Pediatric neuropsychologists from 18 institutions completed surveys regarding neuropsychological practice and the impact of involvement in the collaborative. Neuropsychological data were entered through an online database. Descriptive analyses examined the survey responses and cognitive functioning of the cohort. Statistical analyses examined which patients were evaluated and if composite scores differed by domain, demographics, measures used, or epilepsy characteristics. Results: Positive impact of participation was evident by attendance, survey responses, and the neuropsychological data entry of 534 presurgical epilepsy patients. This cohort, ages 6 months to 21 years, were majority White and non‐Hispanic, and more likely to have private insurance. Mean intelligence quotient (IQ) scores were below to low average, with weaknesses in working memory and processing speed. Full‐scale IQ (FSIQ) was lowest for patients with younger age at seizure onset, daily seizures, and magnetic resonance imaging (MRI) abnormalities. Significance: We established a collaborative network and fundamental infrastructure to address questions outlined by the Epilepsy Research Benchmarks. There is a wide range in the age and IQ of patients considered for pediatric epilepsy surgery, yet it appears that social determinants of health impact access to care. Consistent with other national cohorts, this US cohort has a downward shift in IQ associated with seizure severity. [ABSTRACT FROM AUTHOR]

We present maps of Ganymede's surface composition with almost complete longitude coverage, acquired using high spatial resolution near‐infrared (0.95–1.65 μm) observations from the ground‐based VLT/SPHERE instrument. Observed reflectance spectra were modeled using a Markov Chain Monte Carlo method to estimate abundances and associated uncertainties of water ices, acids, salts and a spectrally flat darkening agent. Results confirm Ganymede's surface is dominated by water ice in young bright terrain (impact craters, sulci), and low‐albedo spectrally flat material in older dark terrain (e.g., Galileo Regio). Ice grain size has strong latitudinal and longitudinal gradients, with larger grains at the equator and on the trailing hemisphere. These trends are consistent with the effects of the latitudinal thermal gradient and global variations in radiation driven sputtering. Sulfuric acid has a low abundance and appears potentially spatially correlated with plasma bombardment, where Ganymede's poles are exposed to the external Jovian magnetic field. Best‐estimate abundances suggest a mixture of salts could be present, although their low abundances, spectral degeneracies and associated uncertainties mean individual salt species cannot be detected with confidence. If present, sodium magnesium sulfate and magnesium chlorate appear tentatively correlated with exogenic plasma bombardment, while magnesium chloride and sulfate appear tentatively correlated with younger terrain, implying a possible endogenic origin. MCMC modeling was also performed on Galileo/NIMS data, showing comparable distributions. The high spatial resolution of SPHERE allows the precise mapping of small scale (<150 km) surface features, which could be used along with higher spectral resolution observations to jointly confirm the presence and distribution of potential species. Plain Language Summary: We have observed Jupiter's icy moon Ganymede, the solar system's largest moon, with the Very Large Telescope in Chile. These observations recorded the amount sunlight reflected from Ganymede's surface at different infrared wavelengths, producing a "reflectance spectrum." We used these reflectance spectra to understand the surface composition of Ganymede by using a computer model that compares each observed spectrum to spectra of different substances that have been measured in laboratories. Ultimately, this model allows us to calculate the amount of each material at each location on Ganymede's surface. Our results show how Ganymede's surface is made up to two main types of terrain: young areas have large amounts of water ice, whereas ancient areas mainly consist of a dark gray material which we were unable to identify. We detected sulfuric acid near Ganymede's poles, which is likely to originate from the gasses which surround Jupiter. A range of different salts were detected, some of which may originate from within Ganymede itself. These surface composition maps will be useful for understanding the processes happening on, and under, Ganymede's surface. They will also help to plan for the robotic space missions which are due to explore Ganymede up‐close in the coming decades. Key Points: VLT/SPHERE maps show Ganymede's surface is mainly water ice in young terrain and a dark, spectrally flat material in old terrainWater ice grain size varies on global scales, controlled by radiation driven sputtering and temperature gradientsHydrated salts and sulfuric acid have lower abundances, with uncertainties making it difficult to make confident detections [ABSTRACT FROM AUTHOR]

Background and purpose: Task‐based functional MRI (fMRI) mapping of the motor function prior to epilepsy surgery has limitations in children with epilepsy. We present a data‐driven method to automatically delineate the motor cortex using task‐free, resting‐state fMRI (rsfMRI) data. Methods: We used whole‐brain rsfMRI for independent component analysis (ICA). A template matching process with Discriminability Index‐based Component Identification score was used for each participant to select and combine motor ICA components in their native brain space, resulting in a whole‐brain ICA Motor Map (wIMM). We validated wIMM by comparing individual results with bilateral finger‐tapping motor task fMRI activation, and evaluated its reproducibility in controls. Results: Data from 64 patients and 12 controls were used to generate group wIMM maps. The hit rate between wIMM and motor task activation ranged from 60% to 79% across all participants. Sensitivity of wIMM for capturing the task activation peak was 87.5% among 32 patients and 100% in 12 controls with available motor task results. We also showed high similarity in repeated runs in controls. Conclusions: Our results show the sensitivity and reproducibility of an automated motor mapping method based on ICA analysis of rsfMRI in children with epilepsy. The ICA maps may provide different, but useful, information than task fMRI. Future studies will expand our method to mapping other brain functions, and may lead to a surgical planning tool for patients who cannot perform task fMRI and help predict their postsurgical function. [ABSTRACT FROM AUTHOR]

Objective: Reorganization of the language network from typically left‐lateralized frontotemporal regions to bilaterally distributed or right‐lateralized networks occurs in anywhere from 25%–30% of patients with focal epilepsy. In patients who have been recently diagnosed with epilepsy, an important question remains as to whether it is the presence of seizures or the underlying epilepsy etiology that leads to atypical language representations. This question becomes even more interesting in pediatric samples, where the typical developmental processes of the language network may confer more variability and plasticity in the language network. We assessed a carefully selected cohort of children with recent‐onset epilepsy to examine whether it is the effects of seizures or their underlying cause that leads to atypical language lateralization. Methods: We used functional magnetic resonance imaging (fMRI) to compare language laterality in children with recently diagnosed focal unaware epilepsy and age‐matched controls. Age at epilepsy onset (age 4 to 6 years vs age 7 to 12 years) was also examined to determine if age at onset influenced laterality. Results: The majority of recent‐onset patients and controls exhibited left‐lateralized language. There was a significant interaction such that the relationship between epilepsy duration and laterality differed by age at onset. In children with onset after age 6, a longer duration of epilepsy was associated with less left‐lateralized language dominance. In contrast, in children with onset between 4 and 6 years of age, a longer duration of epilepsy was not associated with less left language dominance. Significance: Our results demonstrate that although language remained largely left‐lateralized in children recently diagnosed with epilepsy, the impact of seizure duration depended on age at onset, indicating that the timing of developmental and disease factors are important in determining language dominance. [ABSTRACT FROM AUTHOR]

Objective: The purpose of this study was to evaluate if focal cortical dysplasia (FCD) co-localization to cortical functional networks is associated with the temporal distribution of epilepsy onset in FCD.Methods: International (20 center), retrospective cohort from the Multi-Centre Epilepsy Lesion Detection (MELD) project. Patients included if >3 years old, had 3D pre-operative T1 magnetic resonance imaging (MRI; 1.5 or 3 T) with radiologic or histopathologic FCD after surgery. Images processed using the MELD protocol, masked with 3D regions-of-interest (ROI), and co-registered to fsaverage_sym (symmetric template). FCDs were then co-localized to 1 of 7 distributed functional cortical networks. Negative binomial regression evaluated effect of FCD size, network, histology, and sulcal depth on age of epilepsy onset. From this model, predictive age of epilepsy onset was calculated for each network.Results: Three hundred eighty-eight patients had median age seizure onset 5 years (interquartile range [IQR] = 3-11 years), median age at pre-operative scan 18 years (IQR = 11-28 years). FCDs co-localized to the following networks: limbic (90), default mode (87), somatomotor (65), front parietal control (52), ventral attention (32), dorsal attention (31), and visual (31). Larger lesions were associated with younger age of onset (p = 0.01); age of epilepsy onset was associated with dominant network (p = 0.04) but not sulcal depth or histology. Sensorimotor networks had youngest onset; the limbic network had oldest age of onset (p values <0.05).Interpretation: FCD co-localization to distributed functional cortical networks is associated with age of epilepsy onset: sensory neural networks (somatomotor and visual) with earlier onset, and limbic latest onset. These variations may reflect developmental differences in synaptic/white matter maturation or network activation and may provide a biological basis for age-dependent epilepsy onset expression. ANN NEUROL 2022;92:503-511. [ABSTRACT FROM AUTHOR]

Jupiter's atmosphere is dominated by multiple jet streams which are strongly tied to its 3D atmospheric circulation. Lacking a rigid bottom boundary, several models exist for how the meridional circulation extends into the planetary interior. Here, we show, collecting evidence from multiple instruments of the Juno mission, the existence of midlatitudinal meridional circulation cells which are driven by turbulence, similar to the Ferrel cells on Earth. Different than Earth, which contains only one such cell in each hemisphere, the larger, faster rotating Jupiter can incorporate multiple cells. The cells form regions of upwelling and downwelling, which we show are clearly evident in Juno's microwave data between latitudes 60°S $60{}^{\circ}\mathrm{S}$ and 60°N $60{}^{\circ}\mathrm{N}$. The existence of these cells is confirmed by reproducing the ammonia observations using a simplistic model. This study solves a long‐standing puzzle regarding the nature of Jupiter's subcloud dynamics and provides evidence for eight cells in each Jovian hemisphere. Plain Language Summary: The cloud layer of Jupiter is divided into dark and bright bands that are shaped by strong east‐west winds. Such winds in planetary atmospheres are thought to be tied with a meridional circulation. The Juno mission collected measurements of Jupiter's atmosphere at various wavelengths, which penetrate the cloud cover. Here, we provide evidence, using the Juno data, of eight deep Jovian circulation cells in each hemisphere encompassing the east‐west winds, gaining energy from atmospheric waves, and extending at least to a depth of hundreds of kilometers. Different than Earth, which has only one analogous cell in each hemisphere, known as a Ferrel cell, Jupiter can contain more cells due to its larger size and faster spin. To support the presented evidence, we modeled how ammonia gas would spread under the influence of such cells and compared it to the Juno measurements. The presented results shed light on the unseen flow structure beneath Jupiter's clouds. Key Points: Measurements from multiple instruments of the Juno mission are interpreted to reveal the meridional circulation beneath Jupiter's clouds16 Jet‐paired deep cells, extending from the cloud deck down to at least 240 bar, are revealed between latitudes 60°S $60{}^{\circ}\mathrm{S}$ and 60°N $60{}^{\circ}\mathrm{N}$, driven by turbulence similar to Earth's Ferrel cellsThe findings are supported by modeling the advection of tracers due to the cells, showing agreement with NH3 ${\mathrm{N}\mathrm{H}}_{3}$ data [ABSTRACT FROM AUTHOR]

Cloud‐tracked wind observations document the role of eddies in putting momentum into the zonal jets. Chemical tracers, lightning, clouds, and temperature anomalies document the rising and sinking in the belts and zones, but questions remain about what drives the flow between the belts and zones. We suggest an additional role for the eddies, which is to generate waves that propagate both up and down from the cloud layer. When the waves break they deposit momentum and thereby replace the friction forces at solid boundaries that enable overturning circulations on terrestrial planets. By depositing momentum of one sign within the cloud layer and momentum of the opposite sign above and below the clouds, the eddies maintain all components of the circulation, including the stacked, oppositely rotating cells between each belt‐zone pair, and the zonal jets themselves. Plain Language Summary: The dark belts and bright zones that circle the planet at constant latitude, along with the jet streams on the belt‐zone boundaries, are the iconic dynamical features of Jupiter's atmosphere. But the circulation cells with rising, sinking, and cross‐latitude motion are just as important because they maintain the storms and turbulent eddies. Voyager and Cassini have shown that the turbulent eddies put energy into the jet streams. We argue that the eddies also put energy into the circulation cells. They do this by generating waves that break as they propagate above and below the clouds. The breaking waves provide the essential forces that replace those that occur on planets with solid boundaries. Key Points: This study proposes a dynamical mechanism that maintains the circulation cells connecting neighboring belts and zones of JupiterWaves that propagate down from the cloud layer are key; when they break they produce a drag force that mimics the effect of a solid boundaryEddies within the clouds drive the zonal jets and probably drive the waves, thereby driving all aspects of the zonal mean circulation [ABSTRACT FROM AUTHOR]

The Ultraviolet Spectrograph (UVS) instrument on the Juno mission records far‐ultraviolet reflected sunlight from Jupiter. These spectra are sensitive to the abundances of chemical species in the upper atmosphere and to the distribution of the stratospheric haze layer. We combine observations from the first 30 perijoves of the mission in order to study the meridional distribution of acetylene (C2H2) in Jupiter's stratosphere. We find that the abundance of C2H2 decreases toward the poles by a factor of 2–4, in agreement with previous analyses of mid‐infrared spectra. This result is expected from insolation rates: near the equator, the UV solar flux is higher, allowing more C2H2 to be generated from the UV photolysis of CH4. The decrease in abundance toward the poles suggests that horizontal mixing rates are not rapid enough to homogenize the latitudinal distribution. Plain Language Summary: The Ultraviolet Spectrograph instrument on the Juno mission to Jupiter is primarily used to study the planet's ultraviolet auroras, but also records reflected sunlight from the planet's upper atmosphere. These ultraviolet reflected sunlight observations can be used to measure the abundances of different gases in Jupiter's stratosphere. In this study, we focus on one prominent molecule, acetylene, and study how its abundance varies with latitude. We find that its abundance decreases toward Jupiter's poles, which agrees with previous results obtained from studying the same molecule with infrared observations. Key Points: Ultraviolet reflected sunlight observations from Juno Ultraviolet Spectrograph were used to study the C2H2 abundance in Jupiter's stratosphereThe stratospheric C2H2 abundance decreases at high latitudes, in agreement with previous studies using infrared dataThe latitudinal distribution of C2H2 can be used to constrain horizontal mixing rates [ABSTRACT FROM AUTHOR]

NASA's Juno spacecraft has been monitoring Jupiter in 53‐day orbits since 2016. Its six‐frequency microwave radiometer (MWR) is designed to measure black body emission from Jupiter over a range of pressures from a few tenths of a bar to several kilobars in order to retrieve details of the planet's atmospheric composition, in particular, its ammonia and water abundances. A key step toward achieving this goal is the determination of the latitudinal dependence of the nadir brightness temperature and limb darkening of Jupiter's thermal emission through a deconvolution of the measured antenna temperatures. We present a formulation of the deconvolution as an optimal estimation problem. It is demonstrated that a quadratic expression is sufficient to model the angular dependence of the thermal emission for the data set used to perform the deconvolution. Validation of the model and results from a subset of orbits favorable for MWR measurements is presented over a range of latitudes that cover up to 60° from the equator. A heuristic algorithm to mitigate the effects of nonthermal emission is also described. Plain Language Summary: One of the instruments on the Juno spacecraft that is currently orbiting Jupiter every 53 days is the microwave radiometer (MWR). It has been sensing the atmosphere for the first time over a wide range of depths below the top‐most clouds, covering pressures from less than the Earth's surface pressure to several thousand times that value. This enables a deeper exploration than ever before of how winds distribute gases that can condense, such as water (as in the Earth's atmosphere) and ammonia (which forms Jupiter's highest level clouds). One challenge in understanding the MWR data is to convert each of its raw measurements into an estimate of the true brightness temperature of Jupiter as though it were observed in a perfect, narrow beam, a process known as a deconvolution. We determined that this correction for the angular dependence can be done reliably with a three‐term (quadratic) expression. The results of this approach have formed the basis of all of the analysis of MWR data to date, and we show some of the intriguing results from orbits that allowed for the best MWR observing geometry over latitudes that cover up to 60° from the equator. Key Points: A method to deconvolve Jupiter's thermal emission measured by the Juno microwave radiometer is presented and validatedDeconvolved nadir brightness temperatures and limb darkening results are presented for Juno observations between July 2016 and April 2018 [ABSTRACT FROM AUTHOR]

We use ground‐based mid‐infrared (8–20 μm) data acquired by three different instruments between 2005 and 2008 to characterize the variability of tropospheric temperature and aerosol opacity during the 2006–2007 Equatorial Zone disturbance. This disturbance is part of a repeating pattern of cloud‐clearing events at Jupiter's equator, observed as a significant brightening at 5 μm (sensing the 2‐ to 7‐bar region) and darkening at visible wavelengths (sensing the ∼0.7‐bar pressure level). The data reveal a brightness temperature increase of ∼3.1 K between 2005 and February 2007 at 8.6‐μm sensing tropospheric aerosol opacity and temperature near 0.6–0.8 bar. At wavelengths sensing tropospheric ammonia and temperatures between 150 and 600 mbar, the brightness temperature remains largely invariant between 2005 and 2008. The tropospheric vertical temperature profile and the tropospheric aerosol opacity were derived from images captured in different filters on four different dates, one for each year. The retrieved aerosol opacity at ∼0.6–0.8 bar shows a decrease at 2–5°S of ∼45% in 2006 and ∼65% in 2007, with respect to 2008. This is consistent with cloud clearing/thinning during the coloration of the Equatorial Zone at visible wavelengths. This brightening at 8.6 μm started in 2005 and preceded the brightening at 5 μm, which started in April 2006. The results also suggest that cloud clearing during the Equatorial Zone disturbances is not simply the result of tropospheric warming, at least at p < 0.7 bar. We propose that cloud clearing occurs due to a decrease in the ammonia gas upwelling at the equator. Plain Language Summary: Jupiter's equatorial latitudes between ∼7°, known as the Equatorial Zone (EZ), undergo dramatic planetary‐scale disturbances that completely alter its appearance at different altitudes of the troposphere between 0.7 and 4 bar. Here we characterize the last EZ disturbance, observed in 2006–2007, to investigate what atmospheric conditions vary during these disturbances. Retrieved aerosol opacity at ∼0.6 bar shows a decrease at 2–5°S of ∼45% in 2006 and ∼65% in 2007, with respect to 2008, consistent with cloud clearing/thinning during these events. This removal of aerosol opacity is observed to start in 2005, a year before the deeper clouds are cleared. These results indicate that the EZ disturbance involves the clearing of both the ammonia ice cloud near 0.7 bar and the deeper NH4SH clouds with each cloud deck responding at different times. Results also suggest that cloud clearing during the EZ disturbances is not simply the result of tropospheric warming in the middle‐to‐high troposphere. We propose that cloud clearing occurs due to a decrease in the ammonia gas upwelling from deeper levels. Key Points: We characterize the 2006–2007 Equatorial Zone disturbance that completely altered the appearance of Jupiter's equatorial latitudesRetrieved aerosol opacity at ∼0.6 bar decreases by 45–65% at 2–5°S during the EZ disturbances, consistent with cloud clearing/thinningCloud clearing during the EZ disturbances is not simply the result of tropospheric warming, at least at p < 0.7 bar [ABSTRACT FROM AUTHOR]

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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. Plain Language Summary: JunoCam, the visible camera on the Juno spacecraft orbiting Jupiter, has detected hundreds of small‐scale waves and wave‐like features, some as small as 30 km, shorter than ever measured before. Some waves appear near larger features, which may be associated with their origin, but others must be the result of winds hidden beneath the clouds. Most of the waves appear like long trains of narrow, parallel lines, but there is a wide variety of other types of wave‐like features. Some waves converge on each other or cross over each other, and some wavefronts appear to radiate outward from a hurricane‐like storm. Although waves are found over a wide range of latitudes from 20°S to 45°N, the overwhelming majority are found in a narrow band between 5°S and 5°N. The vast majority of these features are found at latitudes with strong prevailing eastward winds, heading in the same direction as Jupiter's rotation. The lack of motion associated with waves at the equator and their similarity to waves measured over even longer time spans by previous spacecraft imply that they are like ripples in a pond but in a rotating fluid, a phenomenon known as inertia‐gravity waves. Key Points: In the first 20 orbits of the Juno mission, over 150 waves and wave‐like features have been detected by the JunoCam public‐outreach cameraA wide variety of wave morphologies were detected over a wide latitude range, but the great majority were found near Jupiter's equatorBy analogy with previous studies of waves in Jupiter's atmosphere, most of the waves detected are likely to be inertia‐gravity waves [ABSTRACT FROM AUTHOR]

Objectives: To determine the effect of ventilation tube (VT) surgery on quality of life (QoL) in children with persistent otitis media with effusion (OME). Design: Secondary analysis of trial data (oral steroids versus placebo for persistent OME), comparing QoL by history of VT surgery performed between 5 weeks and 12 months post‐randomisation. Multilevel regression models were used to identify the association between VT surgery and QoL scores at 12 months, controlling for pre‐exposure risk factors associated with surgery, including pre‐surgery hearing level. Setting: Ear, nose and throat (ENT), paediatric audiology and audiovestibular medicine (AVM) departments in Wales and England. Participants: A total of 327 children aged 2‐8 years with OME symptoms for at least three months and audiometry‐proven bilateral hearing loss with VT surgery status. Main outcome measures: Otitis Media questionnaire (OM8‐30) and Paediatric Quality of Life Inventory (PedsQL) total and subscale scores, and the Health Utilities Index Mark 3 (HUI3) at 12 months post‐randomisation. Results: Participants who had VT surgery had no significant difference in OM8‐30, PedsQL or HUI total scores. OM8‐30 hearing difficulty (HD) subscale scores at 12 months were better in those who had VT surgery (adjusted mean difference (aMD) = −0.46 (95% confidence interval: −0.69 to −0.23), P <.001), and this varied by when the surgery occurred (aMD for surgery between 5 weeks and 6 months = −0.4 [−0.67 to −0.13], P =.004 and between 6 and 12 months = −0.54, [−0.87 to −0.22], P =.001). Conclusion: Ventilation tube surgery was associated with an improvement in HD‐related functional health status but no change in overall QoL. [ABSTRACT FROM AUTHOR]

Objectives: Orthodontic treatment consists of numerous appliance activations that rely on stimulation of osteoclasts at alveolar bone sites. However, the action of osteoclast-like cells on dentin ("odontoclasts") is a pathological side effect of orthodontic treatment. The aim of this article is twofold: (a) To report preliminary results from ongoing cell culture experiments to identify unique markers of dentin resorption, and (b) To discuss our work using nanoparticle tracking analysis (NTA) and exosomes for developing biological fluid-based biopsies to monitor clastic cell activity.Setting and Sample Population: Twelve healthy volunteers in permanent dentition.Material and Methods: For the in vitro experiments, murine clastic cell precursors were cultured on dentin or bone slices for 7 days and phage-display biopanning was used to identify molecular surface differences between osteoclasts and odontoclasts. In the human study, gingival crevicular fluid (GCF) samples were collected using different tools and analysed for protein and exosome recovery.Results: Biopanning generated antibody fragments that were uniquely reactive to odontoclasts. Numerous nanoparticles in the size range of exosomes were detected in all of the human GCF samples.Conclusions: Our results support that there are molecular differences between osteoclasts and odontoclasts. Emerging technologies may allow the use of exosomes in GCF as a clinical tool to detect markers of root resorption. [ABSTRACT FROM AUTHOR]

Summary: Objective: We aimed to predict language deficits after epilepsy surgery. In addition to evaluating surgical factors examined previously, we determined the impact of the extent of functional magnetic resonance imaging (fMRI) activation that was resected on naming ability. Method: Thirty‐five adults (mean age 37.5 ± 10.9 years, 13 male) with temporal lobe epilepsy completed a preoperative fMRI auditory description decision task, which reliably activates frontal and temporal language networks. Patients underwent temporal lobe resections (20 left resection). The Boston Naming Test (BNT) was used to determine language functioning before and after surgery. Language dominance was determined for Broca and Wernicke area (WA) by calculating a laterality index following statistical parametric mapping processing. We used an innovative method to generate anatomic resection masks automatically from pre‐ and postoperative MRI tissue map comparison. This mask provided the following: (a) resection volume; (b) overlap between resection and preoperative activation; and (c) overlap between resection and WA. We examined postoperative language change predictors using stepwise linear regression. Predictors included parameters described above as well as age at seizure onset (ASO), preoperative BNT score, and resection side and its relationship to language dominance. Results: Seven of 35 adults had significant naming decline (6 dominant‐side resections). The final regression model predicted 38% of the naming score change variance (adjusted r2 = 0.28, P = 0.012). The percentage of top 10% fMRI activation resected (P = 0.017) was the most significant contributor. Other factors in the model included WA LI, ASO, volume of WA resected, and WA LI absolute value (extent of laterality). Significance: Resection of fMRI activation during a word‐definition decision task is an important factor for postoperative change in naming ability, along with other previously reported predictors. Currently, many centers establish language dominance using fMRI. Our results suggest that the amount of the top 10% of language fMRI activation in the intended resection area provides additional predictive power and should be considered when planning surgical resection. [ABSTRACT FROM AUTHOR]

Summary: Objective: To assess the ability of functional MRI (fMRI) to predict postoperative language decline compared to direct cortical stimulation (DCS) in epilepsy surgery patients. Methods: In this prospective case series, 17 patients with drug‐resistant epilepsy had intracranial monitoring and resection from 2012 to 2016 with 1‐year follow‐up. All patients completed preoperative language fMRI, mapping with DCS of subdural electrodes, pre‐ and postoperative neuropsychological testing for language function, and resection. Changes in language function before and after surgery were assessed. fMRI activation and DCS electrodes in the resection were evaluated as potential predictors of language decline. Results: Four of 17 patients (12 female; median [range] age, 43 [23‐59] years) experienced postoperative language decline 1 year after surgery. Two of 4 patients had overlap of fMRI activation, language‐positive electrodes in basal temporal regions (within 1 cm), and resection. Two had overlap between resection volume and fMRI activation, but not DCS. fMRI demonstrated 100% sensitivity and 46% specificity for outcome compared to DCS (50% and 85%, respectively). When fMRI and DCS language findings were concordant, the combined tests showed 100% sensitivity and 75% specificity for language outcome. Seizure‐onset age, resection side, type, volume, or 1 year seizure outcome did not predict language decline. Significance: Language localization overlap of fMRI and direct cortical stimulation in the resection influences postoperative language performance. Our preliminary study suggests that fMRI may be more sensitive and less specific than direct cortical stimulation. Together they may predict outcome better than either test alone. [ABSTRACT FROM AUTHOR]

We analyze the potential vorticity of Saturn's polar regions, as it is a fundamental dynamical tracer that enables us to improve our understanding of the dynamics of these regions and their seasonal variability. In particular, we present zonally averaged quasi‐geostrophic potential vorticity maps between 68° planetographic latitude and the poles at altitudes between 500 and 1 mbar for three different epochs: (i) June 2013 (early northern summer) for the north polar region, (ii) December 2008 (late northern winter) for both polar regions, and (iii) October 2006 (southern summer) for the south, computed using temperature profiles retrieved from Cassini Composite Infrared Spectrometer data and wind profiles obtained from Cassini's Imaging Science Subsystem. The results show that quasi‐geostrophic potential vorticity maps are very similar at all the studied epochs, showing positive vorticities at the north and negative at the south, indicative of the dominance of the Coriolis parameter 2Ωsinϕ at all latitudes, except near the pole. The meridional gradients of the quasi‐geostrophic potential vorticity show that dynamical instabilities, mainly due to the barotropic term, could develop at the flanks of the Hexagon at 78°N, the jet at 73.9°S, and on the equatorward flank of both polar jets. There are no differences in potential vorticity gradients between the two hemispheres that could explain why a hexagon forms in the north and not in the south. No seasonal variability of the potential vorticity and its meridional gradient has been found, despite significant changes in the atmospheric temperatures over time. Plain Language Summary: Saturn's polar regions are characterized by a wide variety of cloud morphologies, some of them apparently unique to Saturn, such as the Hexagon wave encircling the north pole. Additionally, Saturn's polar regions undergo strong seasonal variations of sunlight over a 29.5‐year cycle (one Saturnian solar orbit), which affect the atmospheric dynamics of these regions. In this study, we analyze the behavior of the polar atmospheric dynamics and its temporal variability, by computing a fundamental tracer of atmospheric motions and meteorology, known as "potential vorticity." For this purpose, we use wind profiles from October 2006, December 2008, and June 2013, measured from images captured by the Cassini Imaging Science Subsystem Instrument, and temperatures retrieved from the Cassini Composite and Infrared Spectrometer. Our results show that Saturn's polar atmospheric dynamics displays a similar behavior at both hemispheres, without any significant seasonal variability. We also show that at all studied epochs dynamical instabilities (of barotropic or baroclinic character) could develop at the flanks of the Hexagon jet, at the equivalent polar jet in the south, and at the location of the strong polar cyclones. Our results do not show hints of why a Hexagon is only present in the northern hemisphere. Key Points: Quasi‐geostrophic potential vorticity maps of Saturn's polar regions are presentedMeridional gradients of quasi‐geostrophic potential vorticity cannot explain the existence of the Hexagon only at the northern hemisphereQuasi‐geostrophic potential vorticity maps do not show significant seasonal variability [ABSTRACT FROM AUTHOR]

Abstract: Using images from the Cassini spacecraft, we analyzed three ribbon waves in Saturn's 42°N eastward jet at 45°N, 42°N, and 39°N planetocentric latitudes. In this report, we demonstrate that the morphology, wavelength, and propagation of the ribbon waves are consistent with barotropic Rossby waves with a smaller baroclinic component. We report on the appearance and disappearance of these waves during Cassini's mission. We suggest that the temporal evolution of these waves are related to the great Saturn storm of 2010–2011. [ABSTRACT FROM AUTHOR]

Abstract: The quasi‐quadrennial oscillation (QQO) and its ∼4 year period in Jupiter's atmosphere were first discovered in 7.8 μm infrared observations spanning the 1980s and 1990s from detecting semiregular variations in equatorial brightness temperatures near 10 hPa. New observations that probe between 0.1 and 30 hPa in Jupiter's atmosphere using the Texas Echelon Cross Echelle Spectrograph (TEXES), mounted on the NASA Infrared Telescope Facility, have characterized the vertical structure of the QQO during a complete cycle between January 2012 and April 2016. These new observations show the thermal oscillation previously detected at 10 hPa and that it extends over a pressure range of 2–17 hPa. We have incorporated a spectrum of wave drag parameterizations into the Explicit Planetary Isentropic Code general circulation model to simulate the observed Jovian QQO temperature signatures inferred from the TEXES observations as a function of latitude. A new stochastic wave drag parameterization explores vertical wind structure and offers insight into the spectra of waves that likely exist in Jupiter's atmosphere to force the QQO. High‐frequency gravity waves produced from convection likely contribute significantly to the QQO momentum budget. The model temperature outputs show strong correlations to equatorial and surrounding latitude temperature fields retrieved from the TEXES data sets at different epochs. Our results reproduce the QQO phenomenon as a zonal jet that descends over time in response to Jovian atmospheric forcing (e.g., gravity waves from convection). [ABSTRACT FROM AUTHOR]

Objective Learning and memory are essential for academic success and everyday functioning, but the pattern of memory skills and its relationship to executive functioning in children with focal epilepsy is not fully delineated. We address a gap in the literature by examining the relationship between memory and executive functioning in a pediatric focal epilepsy population. Methods Seventy children with focal epilepsy and 70 typically developing children matched on age, intellectual functioning, and gender underwent neuropsychological assessment, including measures of intelligence (Wechsler Abbreviated Scale of Intelligence [ WASI]/Differential Ability Scales [ DAS]), as well as visual Children's Memory Scale ( CMS Dot Locations) and verbal episodic memory (Wide Range Assessment of Memory and Learning [ WRAML] Story Memory and California Verbal Learning Test for Children [ CVLT-C]). Executive functioning was measured directly ( WISC- IV Digit Span Backward; Clinical Evaluation of Language Fundamentals, Fourth Edition ( CELF- IV) Recalling Sentences) and by parent report (Behavior Rating Inventory of Executive Function [ BRIEF]). Results Children with focal epilepsy had lower delayed free-recall scores than controls across visual and verbal memory tasks (p = 0.02; partial η2 = 0.12). In contrast, recognition memory performance was similar for patients and controls (p = 0.36; partial η2 = 0.03). Children with focal epilepsy demonstrated difficulties in working memory (p = 0.02; partial η2 = 0.08) and planning/organization (p = 0.02) compared to controls. Working memory predicted 9-19% of the variance in delayed free recall for verbal and visual memory; organization predicted 9-10% of the variance in verbal memory. Patients with both left and right focal epilepsy demonstrated more difficulty on verbal versus visual tasks (p = 0.002). Memory performance did not differ by location of seizure foci (temporal vs. extratemporal, frontal vs. extrafrontal). Significance Children with focal epilepsy demonstrated memory ability within age-level expectations, but delayed free recall was inefficient compared to typically developing controls. Memory difficulties were not related to general cognitive impairment or seizure localization. Executive functioning accounted for significant variance in memory performance, suggesting that poor executive control negatively influences memory retrieval. [ABSTRACT FROM AUTHOR]

Objective To demonstrate an association between magnetic resonance imaging ( MRI) findings and pathologic characteristics in children who had surgery for medically refractory epilepsy due to focal cortical dysplasia ( FCD). Methods We retrospectively studied 110 children who had epilepsy surgery. Twenty-seven patients with FCD were included. Thirteen had temporal lobe epilepsy ( TLE) and 14 had extra-temporal lobe epilepsy ( ETLE). Three patients had associated mesial temporal sclerosis. Preoperative 3T MRIs interleaved with nine controls were blindly re-reviewed and categorized according to signal alteration. Pathologic specimens were classified according to the 2011 International League Against Epilepsy ( ILAE) classification and compared to MRI studies. Results Rates of pathology subtypes differed between TLE and ETLE (χ2(3) = 8.57, p = 0.04). FCD type I was more frequent in TLE, whereas FCD type II was more frequent in ETLE. In the TLE group, nine patients had temporal tip abnormalities. They all exhibited gray-white matter blurring with decreased myelination and white matter hyperintense signal. Blurring involved the whole temporal tip, not just the area of dysplasia. These patients were less likely to demonstrate cortical thickening compared to those without temporal tip findings (χ2(1) = 9.55, p = 0.002). Three of them had FCD Ib, three had FCD IIa, two had FCD IIIa, and one had FCD IIb; MRI features could not entirely distinguish between FCD subtypes. TLE patients showed more pronounced findings than ETLE on MRI (χ2(1) = 11.95, p = 0.003, odds ratio [ OR] 18.00). In all cases of FCD, isolated blurring was more likely to be associated with FCD II, whereas blurring with decreased myelination was seen with FCD I (χ2(6) = 13.07, p = 0.042). Significance Our study described associations between MRI characteristics and pathology in children with FCD and offered a detailed analysis of temporal lobe tip abnormalities and FCD subtypes in children with TLE. These findings may contribute to the presurgical evaluation of patients with refractory epilepsy. [ABSTRACT FROM AUTHOR]

Objective Functional magnetic resonance imaging ( fMRI) activation of the mesial temporal lobe ( MTL) may be important for epilepsy surgical planning. We examined MTL activation and lateralization during language fMRI in children and adults with focal epilepsy. Methods One hundred forty-two controls and patients with left hemisphere focal epilepsy (pediatric: epilepsy, n = 17, mean age = 9.9 ± 2.0; controls, n = 48; mean age = 9.1 ± 2.6; adult: epilepsy, n = 20, mean age = 26.7 ± 5.8; controls, n = 57, mean age = 26.2 ± 7.5) underwent 3T fMRI using a language task (auditory description decision task). Image processing and analyses were conducted using Statistical Parametric Mapping (SPM8); regions of interest ( ROIs) included MTL, Broca's area, and Wernicke's area. We assessed group and individual MTL activation, and examined degree of lateralization. Results Patients and controls (pediatric and adult) demonstrated group and individual MTL activation during language fMRI. MTL activation was left lateralized for adults, but less so in children (p's < 0.005). Patients did not differ from controls in either age group. Stronger left-lateralized MTL activation was related to older age (p = 0.02). Language lateralization (Broca's and Wernicke's) predicted 19% of the variance in MTL lateralization for adults (p = 0.001), but for not children. Significance Language fMRI may be used to elicit group and individual MTL activation. The developmental difference in MTL lateralization and its association with language lateralization suggests a developmental shift in lateralization of MTL function, with increased left lateralization across the age span. This shift may help explain why children have better memory outcomes following resection compared to adults. [ABSTRACT FROM AUTHOR]

Objective: Functional connectivity (FC) among language regions is decreased in adults with epilepsy compared to controls, but less is known about FC in children with epilepsy. We sought to determine if language FC is reduced in pediatric epilepsy, and examined clinical factors that associate with language FC in this population. Methods: We assessed FC during an age-adjusted language task in children with lefthemisphere focal epilepsy (n = 19) compared to controls (n = 19). Time series data were extracted for three left regions of interest (ROIS) and their right homologues: inferior frontal gyrus (IFG), middle frontal gyrus (MFG), and Wernicke's area (WA) using SPM8. Associations between FC and factors such as cognitive performance, language dominance, and epilepsy duration were assessed. Results: Children with epilepsy showed decreased interhemispheric connectivity compared to controls, particularly between core left language regions (IFG, WA) and their right hemisphere homologues, as well as decreased intrahemispheric right frontal FC. Increased intrahemispheric FC between left IFG and left WA was a positive predictor of language skills overall, and naming ability in particular. FC of language areas was not affected by language dominance, as the effects remained only when examining participants with left language dominance. Overall FC did not differ according to duration of epilepsy or age of onset. Significance: FC during a language task is reduced in children, similar to findings in adults. In specific, children with left focal epilepsy demonstrated decreased interhemispheric FC in temporal and frontal language connections and decreased intrahemispheric right frontal FC. These differences were present near the onset of epilepsy. Greater FC between left language centers is related to better language ability. Our results highlight that connectivity of language areas has a developmental pattern and is related to cognitive ability. [ABSTRACT FROM AUTHOR]

Objective Functional magnetic resonance imaging is sensitive to the variation in language network patterns. Large populations are needed to rigorously assess atypical patterns, which, even in neurological populations, are a minority. Methods We studied 220 patients with focal epilepsy and 118 healthy volunteers who performed an auditory description decision task. We compared a data-driven hierarchical clustering approach to the commonly used a priori laterality index (LI) threshold (LI < 0.20 as atypical) to classify language patterns within frontal and temporal regions of interest. We explored (n = 128) whether IQ varied with different language activation patterns. Results The rate of atypical language among healthy volunteers (2.5%) and patients (24.5%) agreed with previous studies; however, we found 6 patterns of atypical language: a symmetrically bilateral, 2 unilaterally crossed, and 3 right dominant patterns. There was high agreement between classification methods, yet the cluster analysis revealed novel correlations with clinical features. Beyond the established association of left-handedness, early seizure onset, and vascular pathology with atypical language, cluster analysis identified an association of handedness with frontal lateralization, early seizure onset with temporal lateralization, and left hemisphere focus with a unilateral right pattern. Intelligence quotient was not significantly different among patterns. Interpretation Language dominance is a continuum; however, our results demonstrate meaningful thresholds in classifying laterality. Atypical language patterns are less frequent but more variable than typical language patterns, posing challenges for accurate presurgical planning. Language dominance should be assessed on a regional rather than hemispheric basis, and clinical characteristics should inform evaluation of atypical language dominance. Reorganization of language is not uniformly detrimental to language functioning. ANN NEUROL 2014;75:33-42 [ABSTRACT FROM AUTHOR]

Two types of ubiquitinated inclusions have been described in motor neurone disease (MND). (1) Skein or globular ubiquitinated inclusions in the motor neurones (more frequently in the lower motor neurones). This is a characteristic feature of all motor neurone disease categories. (2) Dot-shape or crescentric ubiquitinated inclusions in the upper layers of cortex and dentate gyrus described in cases of motor neurone disease with dementia (DMND). We investigated the substantia nigra (SN) in MND cases; two cases of motor neurone disease inclusion body (MND-IB) dementia, six cases of DMND, 14 cases of MND (including one case from Guam and two cases of familial SOD1 mutation), four cases of Parkinson's disease (PD), and 10 cases of age-matched normal controls. SN and spinal cord sections were stained with ubiquitin (α-synuclein, tau, PGM1, SMI-31 and SOD1 antibodies). The neuronal density in SN was quantified by using a computer-based image analysis system. Four out of six DMND cases showed rounded ubiquitin positive inclusions with irregular frayed edges, associated with neuronal loss, reactive astrocytosis and a large number of activated microglia cells. These inclusions are negative with antibodies to (α-synuclein, tau, SMI-31 and SOD1). The SN in cases from MND-IB dementia and MND showed occasional neuronal loss and no inclusions. The ubiquitin-only inclusions in SN of DMND cases are similar (but not identical) to the ubiquitinated inclusions described previously in the spinal cord of MND cases and are distinct from Lewy bodies (LBs). The degeneration of SN is most likely a primary neurodegenerative process of motor neurone disease type frequently involving the DMND cases. MND disease is a spectrum and multisystem disorder with DMND located at the extreme end of a spectrum affecting the CNS more widely than just the motor system. [ABSTRACT FROM AUTHOR]

We use an infrared data set captured between 1984 and 2017 using several instruments and observatories to report five rare equatorial disturbances that completely altered the appearance of Jupiter's equatorial zone (EZ): the clearance of tropospheric clouds revealed a new 5‐μm‐bright band encircling the planet at the equator, accompanied by large 5‐μm‐bright filaments. Three events were observed in ground‐based images in 1973, 1979, and 1992. We report and characterize for the first time the entire evolution of two new episodes of this unusual EZ state that presented their maximum 5‐μm‐brightness in December 1999 and February 2007, coinciding with a brown coloration south of the equator and with large bluish filaments and white plumes in the northern EZ at visible wavelengths. We characterize their typical infrared‐bright lifetimes of 12–18 months, with possible periodicities of 6–8 or 13–14 years. We predict that a full‐scale equatorial disturbance could occur in 2019–2021. Plain Language Summary: Jupiter's banded structure, white zones (cloud‐covered regions) and brown belts (cloud‐free regions), exhibits dramatic planetary‐scale changes. In this paper, we report five rare events at Jupiter's equatorial zone that changed the appearance of this zone completely at the cloud forming region (1–4 bar), leaving a bright band at the equator, accompanied by narrow and bright filaments (festoons) at the northern equatorial zone. We use ground‐based 5‐μm data, which reveal the thermal emission from 1 to 4 bar region (bellow the ammonia cloud), captured between June 1984 and August 2017 (almost three Jovian years) to report and characterize for the first time two new disturbances at Jupiter's equatorial zone that took place in 1999–2000 and 2006–2007. We found that changes in the cloud morphology at the equatorial zone during these disturbances occurred first at the cloud tops (~700 mbar), months before they were observed at the cloud forming region at 1–4 bar. We also found that these disturbances are confined at the cloud deck (~150 mbar to 4 bar), lasting 12–18 months. After analyzing five documented equatorial zone disturbances, we conclude that these events are periodic/stochastic with typical intervals of 6–8 or 13–14 years. We predict a new disturbance in 2019–2021, during Juno's exploration epoch. Key Points: We report a pattern of cloud clearance events that completely change the appearance of Jupiter's equatorial zone in the infraredThe equatorial disturbance forms in less than 1 month and dissipates over 4 months, with a typical lifetime of 12–18 months at 5 μmA 6‐ to 8‐ or 13‐ to 14‐year periodicity is found. We predict a new equatorial zone disturbance at 5 μm to occur in 2019–2021 [ABSTRACT FROM AUTHOR]

Jupiter's tropospheric ammonia (NH3) abundance is studied using spatially resolved 5 μm observations from the cryogenic high-resolution infrared spectrograph (CRIRES) at the European Southern Observatory's Very Large Telescope. The high-resolving power ( R = 96,000) allows the line shapes of three NH3 absorption features to be resolved. We find that within the 1-4 bar pressure range, the NH3 abundance decreases with altitude. The instrument slit was aligned north-south along Jupiter's central meridian, allowing us to search for latitudinal variability. There is considerable uncertainty in the large-scale latitudinal variability, as the increase in cloud opacity in zones compared to belts can mask absorption features. However, we do find evidence for a strong NH3 enhancement at 4-6°N, consistent with a localized 'ammonia plume' on the southern edge of Jupiter's North Equatorial Belt. [ABSTRACT FROM AUTHOR]

An abstract of the article "Specific MS/MS Fragmentation of Lysine, Arginine, and Ornithine Glycation Products Provides an Opportunity for Their Selective Detection in Protein Acid Hydrolysates and Enzymatic Digests" by O.K. Argirov, N.D. Leigh, and B.J. Ortwerth is presented.

Introduction: Motor neuron disease (MND) is characterized by selective loss of upper and lower motor neurons, although other CNS regions may also be affected (Abrahams et al . Brain 1996; 119: 2105; Lloyd et al . Brain 2000; 123: 2289). We previously demonstrated reduced neuronal density within extra-motor cortical areas associated with astrocytic and microglial activation. We have now explored whether selective loss of inhibitory (GABAergic) neurones occurs in MND. Material and methods: The density of inhibitory interneurons immunoreactive for the calcium-binding proteins calbindin-D28K (CB), calretinin (CR), and parvalbumin (PV) was determined via quantitative image analysis in the primary motor cortex (PMC; Brodmann's area 4) and dorsolateral prefrontal cortex (DLPFC; Brodmann's area 9) from 13 MND and eight control cases, matched for age and postmortem interval. Results: There was a significant reduction in CB-+ve densities within lamina II of both area 4 and 9 in MND (Wilk's lambda multivariate test: P = 0.003). However, post hoc comparisons of individual regions showed that these changes were only significant in area 9 (P = 0.046). PV-+ve densities within cortical layer VI were significantly reduced in MND in both regions (P = 0.015), whereas the multivariate test showed no significant difference within the two regions (P = 0.951). Conclusions: These findings reveal a selective loss in the density of subpopulations of GABAergic neurons in PMC and DLPFC in MND. [ABSTRACT FROM AUTHOR]

Objectives: This study aimed to investigate the mechanisms through which social support and felt stigma influence the relationship between motor neurone disease (MND)-related stress and psychological distress for people with MND. Although a lack of social support has been identified as a significant predictor of psychological distress for individuals with MND, the mechanisms through which this relationship exists have not been assessed, nor have the predictive nature of stigma. Furthermore, the theoretical model specifying the effects of enacted stigma on self-stigma has not been tested in individuals with MND., Design: A cross-sectional design utilizing an online survey method was used. It was hypothesized that social support would moderate the relationship between MND-related stress (operationalized as enacted stigma or physical functioning) and psychological distress (operationalized as depression, anxiety, and stress). Furthermore, felt stigma would significantly mediate the relationship between MND-related stress (enacted stigma) and psychological distress., Methods: Individuals with a diagnosis of MND were recruited internationally through social media and through various organizations and support services. Seventy-seven participants completed the online survey., Results: Significant correlations were identified between social support, felt, and enacted stigma and psychological distress. Moderation analysis was not significant. However, the mediation analyses identified felt stigma as a significant mediator of the relationship between enacted stigma and psychological distress. A direct relationship between enacted stigma and stress (but not depression and anxiety) was also evident., Conclusions: A comprehensive approach to tackling stigma is important in ameliorating psychological distress for people with MND. Limitations of the current study are discussed, along with implications for clinical practice., (© 2020 The Authors. British Journal of Health Psychology published by John Wiley & Sons Ltd on behalf of British Psychological Society.)