Search

Rayleigh wave ellipticity measurements from seismic ambient noise recorded on the Greenland Ice Sheet (GrIS) show complex and anomalous behavior at wave periods sensitive to ice (T < 3–4 s). To understand these complex observations, we compare them with synthetic ellipticity measurements obtained from synthetic ambient noise computed for various seismic velocity and attenuation models, including surface wave overtone effects. We find that in dry snow conditions within the interior of the GrIS, to first order the anomalous ellipticity observations can be explained by ice models associated with the accumulation and densification of snow into firn. We also show that the distribution of ellipticity measurements is strongly sensitive to seismic attenuation and the thermal structure of the ice. Our results suggest that Rayleigh wave ellipticity is well suited for monitoring changes in firn properties and thermal composition of the Greenland and Antarctic ice sheets in a changing climate. Plain Language Summary: Surface meltwater is increasingly being routed and distributed through the Greenland Ice Sheet (GrIS) changing the mechanical and thermal properties of the ice and resulting in accelerated ice flow. Here we observe complex and anomalous Rayleigh wave ellipticity measurements at periods sensitive to the ice structure. We compare our observations with ellipticity measurements made on simulated seismic noise for various seismic velocity and attenuation models. We demonstrate that in the interior of the GrIS the ellipticity is sensitive to the accumulation and densification of snow as it compacts into glacier ice. The variation in the measurements is strongly sensitive to the thermal structure of the ice sheet which we estimate to be warmer than about −10°. These results demonstrate that Rayleigh wave ellipticity is well suited for monitoring changes in firn properties and thermal composition of the Greenland and Antarctic ice sheets in a changing climate. Key Points: Densification of snow into firn has a first order effect on ellipticity measurements at periods sensitive to the iceThe distribution of ellipticity measurements is sensitive to the thermal composition of the iceEllipticity is a promising method for long term monitoring of ice properties and thickness beneath the seismic station [ABSTRACT FROM AUTHOR]

The Pre‐Industrial climate model simulation is intended as an equilibrium control experiment that uses constant external forcing, yet in the Coupled Model Intercomparison Project Phase 6 (CMIP6) model HadGEM3‐GC31‐LL a distinct change in climate state occurs around year 500 of the 2000 year simulation. The global mean near surface air temperature increases by almost 0.5 K associated with a reduction in southern hemisphere sea ice area of almost 20%. Here we show this step change in the state of the climate to be a consequence of the onset of deep convection in the Weddell and Ross Sea gyres. The delayed onset of convection in the gyres is a consequence of a positive, downward, top‐of‐atmosphere radiative balance, and continual ocean heat up‐take during the model spin‐up and the initial pre‐industrial control simulation. Consequently, model spin‐up strategy should be revised to initialize pre‐industrial simulations that are in energy balance. Plain Language Summary: The Pre‐industrial control simulation of climate models is a reference for climate change simulations. Consequently it should simulate a stable climate. However, if the model is not in radiative equilibrium, the ocean continually accumulates heat, becoming unstable at high latitudes and generating large climate fluctuations. This results in a control simulation that is not a steady state. Consequently the methodologies used to initialize and formulate climate models should be revised to ensure a steady state is achieved. Key Points: The long timescales associated with deep ocean heat uptake suggests simulations may not be equilibriated before forcing is perturbedSouthern Ocean venting of heat reduces sea ice cover and increases global mean temperature, leading to a warmer climate stateNet top‐of‐atmosphere energy imbalance can have implications for the methodologies used for climate model spin‐up [ABSTRACT FROM AUTHOR]

We investigate a possible negative ion feature observed by the Cassini Plasma Spectrometer (CAPS) during a flyby of Saturn's moon Dione that occurred on 7 April 2010. By examining possible particle trajectories, we find that the observed particles are consistent with negative pickup ions originating near the moon's surface. We find that the mass of the negative pickup ions is in the range of 15–25 u and tentatively identify this species as O−, likely resulting from ionization and subsequent pickup from Dione's O2‐CO2 exosphere. Our estimates show that the negative ion density is ~3 × 10−3 cm−3. This is comparable to, but slightly smaller than, that previously reported for the density of O2+ pickup ions for the same flyby, indicating that negative pickup ions may represent a major loss channel for Dione's exosphere. Key Points: Analysis of data from the Cassini Plasma Spectrometer confirms negative pickup ions originating from Saturn's moon DioneThe negative pickup ions are consistent with O− originating from Dione's exosphereDensity estimates indicate that negative pickup ions may represent a significant loss channel for Dione's exosphere [ABSTRACT FROM AUTHOR]

The inner boundary of Saturn's electron radiation belts, near the planet's A ring (∼2.27 Rs), is studied using Cassini's proximal orbit measurements. We find that variable convective flows transport energetic electrons to the A ring, which absorbs them instantaneously, forming the inner belt boundary. These flows are also responsible for a variable and longitudinally asymmetric boundary configuration. Prenoon, the boundary oscillates toward and away from the A ring with a 2‐week period. Postnoon, it maps persistently near the F ring (∼2.32 Rs) and coexists with localized MeV electron intensity enhancements (microbelts). We propose that the microbelts contain electrons in drift resonance with corotation, trapped in local time‐confined trajectories, which result from the aforementioned convective flows. The microbelts' collocation with the F ring implies either a local, secondary electron production due to galactic cosmic ray collisions with F ring dust or an enhanced resonant electron trapping due to an electrodynamic interaction between the F ring and Saturn's magnetosphere. Plain Language Summary: The material density of Saturn's main rings is large enough to instantaneously remove even the highest energy particles of the planet's radiation belts that come in contact with them. Even though this interaction does not sound trivial, Cassini observations indicate the opposite. The transition between Saturn's electron radiation belts and the Saturn's A ring, the outermost component of the main rings, was crossed 45 times during Cassini's final orbits. In all cases, the expected signature of electron depletion by the rings was observed but only twice this depletion mapped on the outer edge of the A ring. All other times, it was found several thousand kilometers away from its expected location. On certain areas in the afternoon sector of the radiation belts, the dropout was preceded by an unexpected, sharp increase of high‐energy electron intensities, which we named microbelts. Both the microbelts and the electron depletions map closer to Saturn's F ring, a highly structured, narrow ring of Saturn. The study investigates the topological properties of the microbelts and the electron belt depletion to demonstrate that the ring belts transition likely combines complex electron flows and a local F ring‐driven electron source that make its structure much more complex than ever anticipated. Key Points: The radial transport of energetic electrons onto Saturn's rings is dominated by convectionThe F ring contains regions of MeV electron pileup evolving separately from Saturn's electron beltsThe F ring may be both a source and a sink of energetic electrons [ABSTRACT FROM AUTHOR]

Abstract: Saturn's largest icy moon, Rhea, hosts a tenuous surface‐sputtered exosphere composed primarily of molecular oxygen and carbon dioxide. In this Letter, we examine Cassini Plasma Spectrometer velocity space distributions near Rhea and confirm that Cassini detected nongyrotropic fluxes of outflowing CO 2 + during both the R1 and R1.5 encounters. Accounting for this nongyrotropy, we show that these possess comparable along‐track densities of ∼2 × 10−3 cm−3. Negatively charged pickup ions, also detected during R1, are surprisingly shown as consistent with mass 26 ± 3 u which we suggest are carbon‐based compounds, such as CN−, C 2 H −, C 2 −, or HCO−, sputtered from carbonaceous material on the moon's surface. The negative ions are calculated to possess along‐track densities of ∼5 × 10−4 cm−3 and are suggested to derive from exogenic compounds, a finding consistent with the existence of Rhea's dynamic CO2 exosphere and surprisingly low O2 sputtering yields. These pickup ions provide important context for understanding the exospheric and surface ice composition of Rhea and of other icy moons which exhibit similar characteristics. [ABSTRACT FROM AUTHOR]