The search for life in the Solar System hinges on data from planetary missions. Detecting biosignatures based on molecular identity, isotopic composition or chiral excess requires measurements that current and planned missions can only partially provide. We introduce a new class of biosignatures, defined by the statistical organization of molecular assemblages and quantified using diversity metrics. Using this framework, we analysed amino-acid diversity across a dataset spanning terrestrial and extraterrestrial contexts. We found that biotic samples are consistently more diverse-and therefore distinct-than their sparser abiotic counterparts. This distinction also holds for fatty acids, indicating that the diversity signal reflects a fundamental biosynthetic signature. It also proves persistent under modelled space-like degradation. Relying only on relative abundances, this biogenicity assessment strategy is applicable to any molecular composition data from archived, current and planned planetary missions. By capturing a fundamental statistical property of the chemical organization of life, it may also transcend biosignatures that are contingent on Earth's evolutionary history.

Context. Jupiter’s polar upper troposphere and stratosphere host a persistent cold vortex poleward of 65°N, but its detailed structure and dynamics have remained difficult to resolve. Aims. The goal is to characterize the thermal structure and dynamics of the polar vortex using new and complementary remote sensing techniques. Methods. We used a combination of high-resolution vertical profiles derived from Juno’s recent radio occultation measurements and mid-infrared imaging from the VLT/VISIR instrument. The former provided direct retrievals of temperature and density near and within the vortex, while VISIR imaging revealed spatial thermal contrasts across the region. Results. Our analysis confirms the presence of a steep meridional temperature jump at 65°N, of about 7±1 K at 100 mbar, which is consistent with a strong vertical wind shear and a prograde polar stratospheric jet reaching up to 80 ms−1 at the 10 mbar level. We find the atmosphere to be thermally stable above 0.55 bar, reaching a Brunt-Väisälä frequency of 0.025 s−1 in the mid-stratosphere. Thermal contrasts observed in the infrared data align with the vertical structures inferred from radio occultations, which validates the presence and extent of the cold vortex. Conclusions. These findings offer a quantitative analysis of the thermal structure and the dynamical behavior of Jupiter’s polar atmosphere and demonstrate the diagnostic power of combining radio occultation and thermal infrared techniques in planetary atmospheric studies.

Abstract Thermal tides on Venus have been extensively studied near the cloud tops, where their three‐dimensional structure and contribution to the atmospheric momentum budget have been characterized from temperature and wind fields. However, their downward propagation and influence within the deep atmosphere remain uncertain, and their behavior in the deep atmosphere, particularly near the surface, remains poorly constrained. Using the LMD Venus Planetary Climate Model, we investigate the near‐surface thermal tides and their governing timescales. The simulations show that these tides are generated by heat transfer from the surface to the planetary boundary layer and produce a diurnal pressure response with a phase lag of about corresponding to a radiative adjustment timescale of about 10 Earth days. In addition, a 35‐day oscillation appears within the stably stratified 10–20 km layer, consistent with a planetary‐scale internal gravity wave. These results suggest that coherent oscillations beyond the diurnal tide can develop in the deep atmosphere, with the surface pressure variability dominated by a superposition of three modes: the diurnal and semidiurnal tides and the 35‐day oscillation. Together, these components account for about 70 of the total surface pressure variance, with potential implications for gravity measurements by forthcoming missions such as VERITAS and EnVision.

Dynamics in Venus’s massive atmosphere drive large-scale mass redistribution, generating measurable perturbations in the planet's external gravitational field. Future high-precision gravity measurements from upcoming missions will provide new constraints on the planet’s internal structure and atmospheric mass redistribution. While the deep atmosphere is difficult to observe with traditional remote sensing, these gravitational signatures offer a direct probe into near-surface dynamics. In this study, we analyze atmospheric fields from the Venus Planetary Climate Model (VPCM) to evaluate time-varying gravitational harmonics and assess the expected magnitude of the signal relative to the sensitivity of future gravity measurements. Our analysis shows that low-degree harmonics (l≤4) may reach amplitudes large enough to be distinguishable from the static internal gravity field. Spectral analysis of the simulated harmonics reveals a signal dominated by the diurnal thermal tide, with additional contributions from the semi-diurnal tide and a 35-day wave signal. This suggests that time-variable gravity measurements may be sensitive not only to thermally forced tides, but also to atmospheric wave activity in Venus’s deep atmosphere. We show that the dominant tidal and wave frequencies may be detectable in future gravity-tracking observations. Furthermore, we present a series of sensitivity experiments to determine how variations in atmospheric parameters influence the gravity signal amplitude and temporal structure. By identifying which atmospheric properties control these signatures, we demonstrate how future gravity data can be used to retrieve specific characteristics of the Venusian atmosphere.

The Hadley circulation is Earth's dominant tropical overturning circulation, regulating atmospheric energy transport, tropical rainfall, and subtropical aridity. Although its variability has been extensively studied on seasonal to decadal climate-change timescales, its subseasonal behaviour remains poorly understood. Here we show that the Madden-Julian Oscillation (MJO), the leading mode of tropical intraseasonal variability, systematically modulates the Hadley circulation and influences global hydroclimate variability. Using reanalysis data and dynamical diagnostics, we identify a robust hemispherically asymmetric Hadley circulation anomaly associated with active MJO events, with amplitudes comparable to the climatological intraseasonal variability of the Hadley circulation. Breaking down the dynamical components reveals that the response is primarily maintained by latent heating associated with moist convection, while the overturning strength is driven by interhemispheric moisture gradients. Lead-lag analyses further show that the Hadley circulation lags the MJO by 4-15 days, indicating that MJO convection may drive overturning adjustments on subseasonal timescales. This coupled MJO-Hadley circulation state reveals a previously overlooked pathway linking tropical intraseasonal oscillations, meridional circulation and the hydrological cycle.

Jupiter, the fastest-rotating planet in the Solar System, exhibits a pronounced equatorial bulge, with its equatorial radius exceeding the polar radius by approximately 7

The eddy-driven jet meandering has been hypothesized to increase due to climate change. This meandering frequently relates to slow-moving patterns of surface low and high pressure anomalies, potentially causing extreme weather events such as droughts, flooding, heat waves, and cold spells. However, the quantitative link between jet meandering and storm development is still lacking, as well as a conclusive mechanism for the effect of climate change on jet meandering. In this study, we separate the physical components in the atmospheric complex system using an idealized moist global circulation model (GCM), performing a series of global warming simulations. We outline the connection between the decreasing equator-to-pole temperature gradient due to Arctic amplification and the meandering of the jet. We derive a theoretical relation between the 500-hPa geopotential height meridional gradient and jet meandering, indicating that the leading reason for the increase in jet meandering is the flattening of the midatmospheric meridional temperature gradient, constraining the variations of the streamfunction anomaly with latitude. As it decreases, the eddy-driven jet slows and its meridional layout widens. By Lagrangian tracking of cyclones and anticyclones, we link the jet meandering to the development of cyclones and anticyclones, showing that intense storms are more likely to be associated with jet meanders during their development stage. Furthermore, jet stream meanders with greater meridional extent will be more likely associated with intense storms. In simulations with increased mean surface temperature, our results demonstrate an increase in both jet meandering and storm intensity.

The intriguing circumpolar cyclone pattern at Jupiter's poles raises fundamental questions about how these systems are organized vertically and, further, how the planet's internal heat shapes and sustains them in the absence of solar insolation. We report recent close-in observations of Jupiter's north pole acquired by NASA's Juno Microwave Radiometer (MWR), which achieved comprehensive microwave mapping of the region at an unprecedentedly high resolution. Using six-channel measurements from eleven perijove passes (PJ51-PJ61) poleward of 75N, we derive polar-mean nadir brightness temperatures and limb-darkening spectra that together point to two equally plausible atmospheric scenarios: (1) a dry-adiabatic profile with slightly depleted ammonia gas at a few bars, or (2) a moist-adiabatic profile with uniform ammonia. Markov chain Monte Carlo retrievals yield a deep ammonia abundance of 354.8+12.0/-11.0 ppmv (3+/-0.1 x solar) and a water abundance of 1.8+1.5/-1.1 x 1000 ppmv (2.1+1.8/-1.3 x solar), resembling previous estimates at lower latitudes. Remarkably, the north pole is found to be 6-7 K warmer than the equator at the 1-bar level, although the inferred difference is close to the 1-sigma uncertainty level. If confirmed, this result would suggest an enhanced internal heat flux toward the poles, which is consistent with the more intense lightning activity observed at high latitudes.

The midlatitude climate and weather are shaped by storms, yet the factors governing their predictability remain insufficiently understood. Here, we use a Convolutional Neural Network (CNN) to predict and quantify uncertainty in the intensity growth and trajectory of over 200,000 storms simulated with a 200-year aquaplanet GCM. This idealized framework provides a controlled climate background for isolating factors that govern predictability. Results show that storm intensity is less predictable than trajectory. Strong baroclinicity accelerates storm intensification and reduces its predictability, consistent with theory. Crucially, enhanced jet meanders further degrade forecast skill, revealing a synoptic source of uncertainty. Quantitatively, jet meandering over the storm center and eastern regions is associated with a doubling of the predicted uncertainty sensitivity in storm growth to the jet structure. These findings highlight the potential of machine learning for advancing understanding of predictability and its governing mechanisms.

The giant planets exhibit a fundamental contrast in their equatorial circulation: Jupiter and Saturn are characterized by broad eastward equatorial jets, or superrotation, whereas Uranus and Neptune exhibit strong westward equatorial flow, or subrotation. This dichotomy has often been interpreted as evidence for distinct dynamical regimes on the gas and ice giants. However, here we show that these opposing equatorial states may instead arise from a common dynamical mechanism, with the direction of the equatorial jet determined by the way convection, rotation, and eddy momentum transport interact within the planetary interior and atmosphere.Here we present a unified perspective on the formation of super- and sub-rotating equatorial jets across the giant planets. In deep rotating convection models, columnar convective motions can organize angular momentum in a way that produces either eastward or westward equatorial flow. The two outcomes emerge as separate equilibrated branches of the same dynamical system, implying that the transition from superrotation to subrotation may be understood as a bifurcation rather than as a change in the underlying forcing. Importantly, both regimes are maintained by comparable wave and eddy processes, suggesting that the gas and ice giants need not require fundamentally different explanations for their equatorial jets.This picture connects naturally with idealized atmospheric 3D hydrodynamical simulations of the ice giants, which show that Uranus- and Neptune-like subrotation can be sustained when the modeled circulation extends sufficiently deep and allows eddy momentum fluxes to converge angular momentum away from the equator. Taken together, the two approaches suggest a continuous dynamical pathway linking the deep convective interiors of the gas giants with the deep atmospheric circulation of the ice giants. The observed contrast between superrotation and subrotation may therefore reflect different equilibrated states of a shared convective-eddy system, controlled by planetary parameters such as convective forcing, stratification, rotation rate, and effective dynamical depth.This unified framework provides a basis for interpreting the diversity of zonal winds among the giant planets and offers testable predictions for future observations of Uranus and Neptune, where the depth and maintenance of the equatorial jets remain key open questions.

Results from the Juno investigation of Jupiter have challenged our understanding of Jupiter origin and evolution. As the archetype of giant planets, the study of Jupiter provides knowledge needed to understand the origin of our own solar system and the planetary systems being discovered around other stars. Jupiter uniquely informs us about the origin of our own planetary system. The mass of Jupiter’s heavy element core and the abundance of heavy elements in the atmosphere discriminate among models for giant planet formation. Measurements by Juno of Jupiter’s gravity field suggest Jupiter’s core is diffuse, extended and contains compositional gradients. These new results require new models of Jupiter’s formation and evolution. The gravity science results on the measurement of J4 coupled to current estimates on the hydrogen and helium equation of state suggests Jupiter’s interior composition has low metallicity, potentially solar or even sub-solar. This is inconsistent with measurements of the atmosphere by both Juno and the Galileo probe which indicate the atmospheric composition is of higher metallicity (2-4x solar). The combined results from Juno provide new constraints on theories of Jupiter’s formation and evolution and giant planets in general. A summary of Juno’s results relevant to Jupiter’s formation and evolution will be presented along with a discussion of theoretical implications on Jupiter, and giant planets both within our solar system and beyond.

Midlatitude storms vary due to the slowly evolving climate and the rapidly changing synoptic conditions. While the impact of both factors has been studied extensively, their relative contributions remain poorly quantified. We use 84 years of ERA-5 reanalysis data and convolutional neural networks to assess the relative importance of seasonal climatology versus synoptic conditions in controlling averaged and individual storm activity. Our models successfully predict over 90% of the variability in mean storm activity, showing climatic conditions dominate it. However, only one-third of the variability in individual storm properties is attributed to climatic factors, indicating that synoptic conditions dominate individual storm characteristics. Further isolating the impact of long-term climate trends on individual storms shows that it contributes to storm-intensity variability only . In contrast, its contribution to storms' associated heat anomalies is over three times greater, demonstrating that variables directly linked to global warming provide a clearer pathway for weather attribution.

Energetic particles continuously process water ice across astrophysical and planetary environments-from interstellar clouds and comets to icy planetary surfaces. Interpreting the resulting observables requires a physically grounded description of the underlying interactions, both to identify radiation-driven signatures and to distinguish them from superimposed chemical, thermal, and microphysical effects. We present Geant4-IcyMoons, an extension of Geant4-DNA developed for irradiated water ice and, ultimately, for materials embedded within it. In this study, we model the elastic and inelastic interactions of electrons with amorphous and hexagonal ice. For the first time, this enables a transport-ready Monte Carlo simulation of electron irradiation in water ice, linking incident-particle environments to the evolution of icy surfaces. We apply this framework to Jupiter's moon Europa as a representative case of electron bombardment of an icy surface. We show that on the trailing hemisphere, the stronger low-energy electron bombardment confines much of the deposited energy to the upper less than or similar to 0.1 cm, whereas on the leading hemisphere, the more energetic incident population drives deposition to depths of tens of centimeters. This may contribute to the observed lens-like enrichment of radiolysis products centered on the equator of the trailing hemisphere. This work lays the foundation for treatments of ion irradiation and radiation chemistry in water ice and embedded materials.

The Atlantic and Pacific storm tracks are regions of enhanced storm activity that shape the Northern Hemisphere climate. Basic theory predicts that stronger jet streams should accompany stronger storm activity. However, despite the Pacific jet being stronger in winter, Atlantic storms are more intense - a puzzling observation that has long challenged our understanding of midlatitude climate. Here, we address this paradox by examining how jet orientation affects interactions with midlatitude storms. Using 84 years of ERA5 data and winter storm tracks (validated with JRA-3Q), we show that the Pacific jet's zonal structure causes storms to exit high-intensity jet regions rapidly. Conversely, the Atlantic jet's tilted orientation aligns with storm trajectories, allowing storms to remain in high-intensity jet regions longer. Lagrangian energetic analyses reveal that while Pacific storms exhibit rapid initial growth, Atlantic storms remain longer in stronger baroclinic regions, enabling greater energy extraction, sustained growth, and higher peak intensities. These findings reconcile Northern Hemisphere winter storm activity with the energetic perspective on midlatitude climate and highlight the importance of representing individual storm dynamics for understanding present and future climates.

AbstractSince 2023, NASA’s Juno mission has been conducting radio occultations of Jupiter’s atmosphere, ionosphere, and aurorae. Radio occultations are enabled by the natural orbital evolution of the trajectory, placing Jupiter between the Juno spacecraft and Earth. As of September 2026, data from over two dozen occultation pairs have been analyzed to determine atmospheric temperature/pressure profiles and ionosphere electron density profiles over a wide range in latitudes, including the polar regions where auroral activity is present. Measurements of the radio frequencies at X-band (8.4 GHz) and Ka-band (32 GHz) are inverted into refractivity through classical numerical ray tracing techniques. From the refractivity, atmospheric temperature/pressure and ionosphere electron density are derived. These data reveal temperature distribution of Jupiter’s atmosphere in regions never before sampled and provide unique data on the polar structure. Future radio occultation opportunities will continue to probe the northern high latitude and equatorial regions.BackgroundJupiter’s atmosphere was sampled by the Pioneer and Voyager missions in the 1970s through radio occultation and the Galileo probe. Radio occultations are key to providing direct measurement of the temperature structure and electron density measurements. Juno’s extended mission offers dozens of occultation observation opportunities due to the natural orbital evolution of the spacecraft’s trajectory. These observations are distributed over a wide range of latitudes of the planet, from the equatorial regions to the north and south poles. These data are complementary to other data including Juno’s Microwave Radiometer (MWR), plasma wave instrument (Waves), and visible & infrared imaging (from both Juno instruments and ground-based observations).ObservationJuno Gravity Science Instrument (Asmar et. al. 2017) is a radio science instrument which utilizes dual-frequency X-band (8.4 GHz) and Ka-band (32 GHz) radio links between the Juno spacecraft and the Earth-based observing stations of NASA’s Deep Space Network (DSN). Although designed to measure gravity fields, the instrumentation is also excellent for radio occultations (Buccino et. al., 2022). As Juno passes behind Jupiter during closest approach, the received frequency is affected by refraction. The depth the occultation reaches is limited by spacecraft pointing: when the signal refracts outside the main beam of the antenna, the observation is concluded at a depth of approximately ~300 mbar. Although Juno is not capable of limb-tracking maneuvers as was done on Voyager, small offsets to the pointing enable a deeper probe depth than otherwise would be achieved (~500 mbar).Figure 1. Map of the conducted (as of August 2026) and future experiment opportunities for radio occultation locations on Jupiter with the Juno spacecraft. Triangles indicate an ingress occultation, and circles indicate an egress occultation. Overlaid is the magnetic field model (JRM33) and the atmospheric basemap, along with the auroral ovals (white lines).Regions of InterestJuno’s extended mission allowed for probing of the atmosphere and ionosphere at a wide range of latitudes beginning with PJ-53 (July 2023). As the occultation season progresses, the latitude becomes more poleward allowing probing of the circumpolar cyclones. A maximum of 88 N occurred on PJ-86 (August 2026), within the polar cyclone. In the south, a maximum of -88 S was achieved on PJ-83. As occultation season reaches its end on PJ-97 (August 2027), opportunities exist for mid-latitude and equatorial regions, including a near-equatorial occultation on PJ-90 (December 2026).ResultsThe atmosphere and ionosphere perturb the radio link causing measurable changes in frequency. Following the methodology in Schinder et. al. 2015, a numerical ray tracing technique is used to invert these frequency changes, along with the spacecraft’s trajectory and planetary ephemeris, into a refractivity profile. The first set of Jupiter occultations resulted in detailed temperature-pressure profiles from mid-latitude regions to the upper-latitude regions (Caruso et. al., 2025 and Smirnova et. al., 2025). These revealed cooler stratosphere and warmer troposphere at the equator. Further studies (Smirnova et. al., 2026) showed the polar stratospheric vortex is indeed cooler with a sharp temperature change at 65°N. Ionosphere electron density profiles of the same regions (Coffin et. al., 2025) show high variability in electron density layers, suggesting a complex interaction with the magnetosphere.AcknowledgementsThe work of DB, MP, RP, and SL was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. Government sponsorship acknowledged. AC, LGC, PT, and MZ are grateful to the Italian Space Agency (ASI) for financial support through Agreement No. 2022-16-HH.0, No. 2023-6-HH.0, and No. 2024-5-HH.0. PS was supported by NASA Contract NNM06AA75C from the Marshall Space Flight Center under subcontract 699054X from Southwest Research Institute.© 2026 California Institute of Technology. Government sponsorship acknowledged.ReferencesAsmar, Sami W., et al. "The Juno gravity science instrument." Space Science Reviews1 (2017): 205-218.Buccino, Dustin, et al. "Planning and execution of Juno radio occultation experiments at Jupiter." 2023 IEEE aerospace conference. IEEE, 2023.Schinder, P. J., et al. "A numerical technique for two-way radio occultations by oblate axisymmetric atmospheres with zonal winds." Radio Science7 (2015): 712-727.Caruso, Andrea, et al. "Probing Jupiter's atmosphere through Juno Radio occultations: Methodology and initial observations." Geophysical Research Letters22 (2025): e2024GL113231.Smirnova, Maria, et al. "Probing Jupiter's atmosphere through Juno radio occultations: Analysis of the atmospheric thermal structure." Geophysical Research Letters22 (2025): e2025GL116804.Smirnova, Maria, et al. "Juno radio occultations reveal the structure of Jupiter's cold northern polar vortex." Astronomy & Astrophysics706 (2026): A109.Coffin, Drew A., et al. "Juno‐derived electron density profiles of the high‐latitude Jovian ionosphere." Journal of Geophysical Research: Space Physics6 (2025): e2025JA033754.

Synoptic systems are understood to organize heat and momentum transport along jet streams, yet the diagnostics used to identify jets remain fundamentally Eulerian in nature. This creates conceptual tension: if the eddy-driven jet can be meaningfully separated from the synoptic eddies that maintain it, then it must be a persistent flow that Eulerian diagnostics are not designed to isolate. An alternative Lagrangian perspective on jet streams (JetLag) was recently developed and identifies jets not as maxima of wind speed (or derivative variables), but as maxima of isentropic displacement. In this view, jets become persistent features that remain identifiable over synoptic timescales. This definition recovers well-known features of the atmospheric circulation, with some systematic differences relative to Eulerian diagnostics. Here we adopt the Lagrangian definition to revisit jets and their variability using a hierarchy of models, ranging from idealized configurations to reanalyses. We explore the connections between synoptic systems and jets, and those between the upper troposphere and the surface.

The unresolved recent multidecadal cooling of the eastern Pacific and its uncertain future remain key puzzles in climate dynamics. We propose the land-sea heating contrast as a potential driver of this phenomenon. To test this, we amplify the land-sea contrast by quadrupling carbon dioxide (CO2) only over land in a global coupled climate model. We show that this causes a pronounced transient cooling of the eastern and equatorial Pacific. A transient 1%-per-year CO2 increase over land produces decadal cooling, suggesting relevance to the observed eastern Pacific cooling. Targeted simulations with locally increased CO2 concentrations over different land regions reveal three drivers of this cooling: a northward intertropical convergence zone shift, a westward convection shift over the western Pacific, and strengthened subtropical highs from Rossby waves. These insights recast the commonly used ocean dynamical thermostat mechanism as a feedback rather than a driver of transient cooling and contribute to understanding and predicting Pacific temperature patterns.

The position and intensity of storm tracks undergo significant changes in response to temporal and spatial variations in atmospheric forcing. Comprehending these changes from the viewpoint of individual cyclones and anticyclones is crucial both from a physical perspective, as they are the main drivers of energy and moisture, and because they are a leading cause of severe weather in the midlatitudes. This study delves into the impact of the jet characteristics on individual cyclones and anticyclones, focusing on their maximum strength and growth time. By utilizing tracks of cyclones and anticyclones spanning over 80 years of ERA5 reanalysis data, we identify unique temporal and spatial variations in maximum strength and growth time. These variations are then clarified through a detailed examination of how these properties respond to the characteristics of the jet. The study reveals that the vertical shear of the jet increases the maximum strength at low and medium regimes and decreases it for intense shear values, potentially playing a significant role in phenomena characterized by extreme shear, such as the midwinter minimum. Breaking down the storm maximum strength into the responses due to growth time and Lagrangian growth rate (effective average growth rate of the individual storms) indicates that while the Lagrangian growth rate is linear with vertical shear, as expected by linear theory, the saturation of maximum strength results from a decrease in growth time with vertical shear. The horizontal shear of the jet, which is less widely studied, was found to reduce the growth time of cyclones and anticyclones significantly. Additionally, horizontal shear has a smaller effect on the Lagrangian growth rate, with cyclones on the poleward side of the jet growing faster and anticyclones on the equatorward side growing faster. These findings provide insights into predicting how changes in jet characteristics in past and future climates influence midlatitude weather through the effect on cyclone and anticyclone activity.

The equatorial jets dominating the dynamics of the Jovian planets exhibit two distinct types of zonal flows: strongly eastward in the gas giants (superrotation) and strongly westward in the ice giants (subrotation). Existing theories propose different mechanisms for these patterns, but no single mechanism has successfully explained both. However, the planetary parameters of the four Solar System giant planets suggest that a fundamentally different mechanism is unlikely. In this study, we show that convection-driven columnar structures can account for both eastward and westward equatorial jets, framing the phenomenon as a bifurcation. Consequently, both superrotation and subrotation emerge as stable branches of the same mechanistic solution. Our analysis of these solutions uncovers similarities in the properties of equatorial waves and the leading-order momentum balance. This study suggests that the fundamental dynamics governing equatorial jet formation may be more broadly applicable across the Jovian planets than previously believed, offering a unified explanation for their two distinct zonal wind patterns.

The polar cyclones on Jupiter have been observed regularly since their discovery by the Juno mission in 2016. While the symmetrically spaced 9 and 6 cyclones at Jupiter's north and south pole (respectively) have largely maintained their locations, 5 years of Juno's observations showed oscillatory perturbations in their positions. In addition, an overall westward drift was measured for the cyclones at both poles. In this study, a mechanism for these motions is presented. This mechanism is driven by the known "beta-drift" effect, a poleward-westward acceleration experienced by cyclones under beta (the meridional gradient in planetary vertical vorticity). When considering the relative vorticity of other cyclones, in addition to beta, to evaluate beta-drift on each cyclone, the polar group of cyclones forms a dynamical system analogous to a system of springs. Using the Juno observations, we show that such a representation agrees well with the data describing the location and acceleration of the cyclones with time. In addition, a toy model, driven by such prescribed beta-drift forces, is able to reproduce motions similar to the observations. To explain the mean westward motion exhibited by the circumpolar cyclones in the north and south poles (4° and 7. 5° degrees longitude per year, respectively), we propose a center-of-mass approach. Using simulations, we show that the motion of cyclones in a group can be primarily divided into a contribution from beta and a contribution from the interactions between cyclones. When considering the group as a whole, their center of mass is only subject to beta, manifesting in a polar orbit of the group, which precesses westward. This precession is proposed as the mechanism for the westward drift of the individual cyclones. We conclude by showing observational evidence for this interpretation.