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In this study, we show that non‐thermal collisions can play a significant role in shaping Europa's exospheric structure. Collisions between radiolytically produced O2 ${\mathrm{O}}_{2}$ and the O produced via electron impact dissociation of O2 ${\mathrm{O}}_{2}$ affect the exospheric structure and escape rates. Specifically, O + O2 ${\mathrm{O}}_{2}$ collisions lead to the production of a non‐thermal O2 ${\mathrm{O}}_{2}$ population, and increase the O2 ${\mathrm{O}}_{2}$ escape while decreasing the O escape. These collisions are dependent on three specific physical parameters: (a) the density of O2 ${\mathrm{O}}_{2}$, (b) the electron impact dissociation rate of O2 ${\mathrm{O}}_{2}$, and (c) the O + O2 ${\mathrm{O}}_{2}$ collision cross section. We demonstrate here that O + O2 ${\mathrm{O}}_{2}$ collisions affect Europa's atmosphere even in the lowest limits considered. Thus, to more accurately determine the influence O + O2 ${\mathrm{O}}_{2}$ collisions have on Europa's atmosphere in preparation for the forthcoming spacecraft missions, Europa Clipper and the JUpiter ICy moons Explorer (JUICE), these physical parameters need to be better constrained. Plain Language Summary: This study investigates the effects of collisions in Europa's atmosphere, specifically focusing on those involving oxygen atoms (O) and molecules (O2 ${\mathrm{O}}_{2}$). We find that collisions between O2 ${\mathrm{O}}_{2}$ produced within Europa's icy surface and the O it produces via dissociative processes while aloft in the atmosphere can affect the structure of Europa's atmosphere as well as the rates at which neutral particles escape to the local space environment. The study highlights three important factors that influence these collisions: the density of O2 ${\mathrm{O}}_{2}$ near Europa's surface, how often O2 ${\mathrm{O}}_{2}$ molecules are broken apart by electrons producing O, and the size of the O + O2 ${\mathrm{O}}_{2}$ collision cross section. Constraining these values is crucial for accurately modeling Europa's atmosphere in preparation for the forthcoming spacecraft missions, Europa Clipper and the JUpiter ICy moons Explorer (JUICE). Key Points: DSMC modeling demonstrates that collisions cannot be neglected in modeling or analysis studies of Europa's atmosphereCollisions between radiolytically produced O2 and its dissociated product O produce a non‐thermal O2 population and enhances O2 escapeThe O2 non‐thermal densities and escape rates produced via O + O2 collisions can far exceed those due to sputtering [ABSTRACT FROM AUTHOR]

We present measurements of 30–700 keV Solar Energetic Electrons (SEEs) near the Moon when within the terrestrial magnetotail by the Acceleration, Reconnection, Turbulence, and Electrodynamics of the Moon's Interaction with the Sun spacecraft. Despite their detection deep within the tail, the incident flux and spectral shape of these electrons are nearly identical to measurements taken upstream of Earth in the solar wind by the Wind spacecraft; however, their pitch angle distribution is isotropized compared to the more field‐aligned distribution upstream. We illustrate that SEEs initially traveling Earthward precipitate onto the lunar far‐side, generating extended shadows in the cis‐lunar electron distribution. By modeling the dynamics of these electrons, we show that their precipitation patterns on the lunar near‐side are comparatively reduced. The non‐uniform precipitation and accessibility of potentially hazardous electrons to the Moon's surface are highly relevant in the context of astronaut safety during the planned exploration of the lunar environment. Plain Language Summary: The Moon is located within the tail of Earth's magnetosphere during one‐third of its orbit. Although the strong terrestrial magnetic field prevents high‐energy particles from reaching Earth's surface, the Moon does not receive the same protection when it is within the terrestrial magnetotail. Instead, we show that the high‐energy electron flux near the Moon is unchanged during intense solar energetic electron events compared to measurements taken far upstream of Earth. However, the precipitation of these particles onto the lunar surface is non‐uniform. Since these electrons gain access to the magnetosphere from down‐tail of the Moon, they preferentially bombard the lunar far‐side surface. This creates a shadow in the electrons on the nearside that extends far beyond the Moon toward Earth. Hence, despite the high flux of these particles that are potentially hazardous to future activities on the lunar surface, there exist regions across the lunar near‐side where the relative flux of these electrons is reduced relative to the upstream value when the Moon is within the magnetotail. These findings provide context for the fundamental scientific understanding of high‐energy solar electrons and their access to the lunar surface. Key Points: High‐energy solar energetic electrons (SEEs) have direct access to the lunar environment when in the terrestrial magnetotailPrecipitation onto the lunar nightside carves‐out electrons from the ambient distribution, generating extended shadows far from the MoonWhen in the tail, the lunar surface is non‐uniformly bombarded by Earthward‐traveling SEEs, with reduced access to the dayside hemisphere [ABSTRACT FROM AUTHOR]

Ionospheric heavy ions in the distant tail of the Earth's magnetosphere at lunar distances are observed using the ARTEMIS mission. These heavy ions are originally produced in the terrestrial ionosphere. Using the ElectroStatic Analyzers (ESA) onboard the two probes orbiting the Moon, these heavy ions are observed as cold populations with distinct energies higher than the baseline energy of protons, with the energy‐per‐charge values for the heavy populations highly correlated with the proton energies. We conducted a full solar cycle survey of these heavy ion observations, including the flux, location, and drift energy, as well as the correlations with the solar wind and geomagnetic indices. The likelihood of finding these heavy ions in the preferred regions of observation called "loaded" quadrants of the terrestrial magnetotail is ∼90%, regardless of the z orientation of the IMF. We characterize the ratio of the heavy ion energy to the proton energy, as well as the velocity ratio of these two populations, for events from 2010 to mid‐2023. This study shows that the "common velocity" assumption for the proton and heavy ion particles, as suggested in previous work through the velocity filter effect, is not necessarily valid in this case. Challenges in the identification of the mass of the heavy ions due to the ESA's lack of ion composition discrimination are addressed. It is proposed that at the lunar distances the heavy ion population mainly consists of atomic oxygen ions (O+) with velocities ∼25% more than the velocity of the co‐located proton population. Key Points: We surveyed ARTEMIS observations of ionospheric heavy ions in the magnetotail at lunar distances over a full solar cycleHeavy ions in the magnetotail are highly correlated with solar wind and geomagnetic activity, and preferentially found in loaded quadrantsHeavy ions drift tailward at ∼25% higher velocities than the concurrently observed protons, implying additional acceleration [ABSTRACT FROM AUTHOR]

Background: The ZAP‐X system is a novel gyroscopic radiosurgical system based on a 3 MV linear accelerator and collimator cones with a diameter between 4 and 25 mm. Advances in imaging modalities to detect small and early‐stage pathologies allow for an early and less invasive treatment, where a smaller collimator matching the anatomical target could provide better sparing of surrounding healthy tissue. Purpose: A novel 3 mm collimator cone for the ZAP‐X was developed. This study aims to investigate the usability of a commercial diode detector (microSilicon) for the dosimetric characterization of this small collimator cone; and to investigate the underlying small field perturbation effects. Methods: Profile measurements in five depths as well as PDD and output ratio measurements were performed with a microSilicon detector and radiochromic EBT3 films. In addition, comprehensive Monte Carlo simulations were performed to validate the measurement observations and to quantify the perturbation effects of the microSilicon detector in these extremely small field conditions. Results: It is shown that the microSilicon detector enables an accurate dosimetric characterization of the 3 mm beam. The profile parameters, such as the FWHM and 20%–80% penumbra width, agree within 0.1 to 0.2 mm between film and detector measurements. The output ratios agree within the measurement uncertainty between microSilicon detector and films, whereas the comparisons of the PDD results show good agreement with the Monte Carlo simulations. The analysis of the perturbation factors of the microSilicon detector reveals a small field correction factor of approximately 3% for the 3 mm circular beam and a correction factor smaller than 1.5% for field diameters above 3 mm. Conclusions: It could be shown that the microSilicon detector is well‐suitable for the characterization of the new 3 mm circular beam of the ZAP‐X system. [ABSTRACT FROM AUTHOR]

This study presents evidence of stably trapped electrons at Jupiter's moon Ganymede. We model energetic electron pitch angle distributions and compare them to observations from the Galileo Energetic Particle Detector to identify signatures of trapped particles during the G28 encounter. We trace electron trajectories to show that they enter Ganymede's mini‐magnetospheric environment, become trapped, and drift around the moon for up to 30 min, in some cases stably orbiting the moon multiple times. Conservation of the first adiabatic invariant partially contributes to energy changes throughout the electrons' orbits, with additional acceleration driven by local electric fields, before they return to Jupiter's magnetosphere or impact the surface. These trapped particles manifest as an electron population with an enhanced flux compared to elsewhere within the mini‐magnetosphere that are detectable by future spacecraft. Plain Language Summary: The magnetized planets of the solar system are known to possess a population of high‐energy, orbiting electrons that are sustained for extended timescales. By comparison, Ganymede, the only moon in the solar system confirmed to have its own permanent magnetic field, should also retain a similar population of trapped particles. Observations from the Galileo mission hint at the existence of electrons that may be locally trapped at the moon, but information regarding their origin and the mechanism behind trapping these electrons is unknown. Furthermore, there are no constraints on the processes that help sustain such a trapped population, and the timescales over which they are maintained at Ganymede remain unknown. In this study, we provide evidence that trapped electrons exist at Ganymede, identify the mechanisms driving their dynamics, and answer open questions about the moon's local energetic particle environment. Key Points: We compare Galileo G28 energetic electron data with test particle tracing to identify a population of trapped electrons at GanymedeWe achieve a robust match between the energetic electron pitch angle distributions from our model compared to those observed by GalileoElectrons follow stable orbits that can encircle the moon multiple times before being lost to the surface or to Jupiter's magnetosphere [ABSTRACT FROM AUTHOR]

Standard geodetic models simplify magma sheet injection to the opening of geometrically simple dislocations in a linearly elastic, homogeneous medium. Intrusion geometries are often complex, however, and non‐elastic deformation mechanisms can dominate the response of heterogeneous rocks to magma‐induced stresses. We used three‐dimensional near‐surface displacements of a scaled laboratory experiment in which a steeply inclined analog magma sheet was injected into granular material. We ran forward models and inverted for eight parameters of an "Okada‐type" tensile rectangular dislocation in a homogeneous, isotropic, and linearly elastic half‐space. Displacements generated by a forward model largely mismatch the experimental displacements, but full or restricted non‐linear inversions of geometrical parameters reduce the residual displacements. The intrusion opening, dip, depth, and to a lesser degree length and width mismatch the most between the experiment and inversion results, whereas location and strike mismatch the least. Our results challenge assumptions made by many analytical and geodetic models. Plain Language Summary: Standard models of volcano deformation simplify a magma intrusion to simple geometries injected in a medium with simplified mechanical behavior. However, intrusion geometries are often complex in nature. Rocks also predominantly respond in a complex manner to magma intrusion. We used the three‐dimensional displacement of the surface of a scaled laboratory experiment in which golden syrup, a magma analog, was injected into a sand‐plaster mixture, an analog for the Earth's crust. Our forward models and inversions show that the modeled simplified geometry and mechanical response largely mismatch the laboratory experiment outcome as observed in X‐ray Computed Tomography imagery. Our results challenge the assumptions made by models commonly used to model and interpret deformation signals measured in volcanically active areas. Key Points: Analog magma intrusions in granular material are approximated by tensile opening dislocations in a linearly elastic half‐spaceInversion results match analog intrusion x‐y location and strike, but mismatch intrusion dip, opening, and depthSimplifying the host rock response to linear elasticity of homogeneous material results in inaccurate inversion model results [ABSTRACT FROM AUTHOR]

Objective. Lung cancer (LC) patients suffer from multiple cooccurring symptoms. Interventions that have the potential to impact more than one symptom within a symptom cluster should be identified. The aim of this review was to examine nonpharmacological interventions that were effective in the management of one or more of the following symptoms in LC patients: dyspnea, fatigue, physical functioning (PF), and role functioning (RF). Methods. Preferred Reporting Items for Systematic Reviews and Meta-Analyses (PRISMA) was used for reporting this systematic review. The Cochrane Central Register of Controlled Trials (CENTRAL), MEDLINE (using the PubMed interface), Embase (using the embase.com interface), and Web of Science were used as electronic databases. Randomized controlled studies were included if they assessed the effects of nonpharmacological interventions on dyspnea, fatigue, PF, and/or RF in patients with LC. Studies were evaluated with the Cochrane risk of bias tool, and relevant data were extracted and narratively summarized. Results and Conclusions. In total, 89 articles were included. Search results (until April 2023) show that most evidence was found for exercise interventions, followed by multicomponent, psychoeducational, diet, acupuncture, and other interventions. Studies that had an effect on multiple symptoms were observed to have the most frequent instances of positively affecting dyspnea, followed by PF, fatigue, and RF. [ABSTRACT FROM AUTHOR]

This article discusses the basibranchial structure and its impact on cardiac morphology in Atlantic salmon. The study finds that farmed salmon often experience structural abnormalities in their hearts, which may be caused by intensive breeding programs and stressful farming practices. These abnormalities can lead to cardiac collapse and increased mortality, particularly during treatments against sea lice. The article also highlights the importance of understanding optimal cardiac function in order to address these issues. The authors suggest that the basibranchial cartilaginous structure may play a role in altering the shape and function of the ventricle, negatively affecting the heart's performance. However, further research is needed to fully understand the causes and implications of these findings. [Extracted from the article]

Jupiter's plasma sheet has been understood to be primarily composed of Io‐genic sulfur and oxygen, along with protons at lower mass density. These ions move radially away from Jupiter, filling its magnetosphere. The material in the plasma sheet interacts with Europa, which is also a source of magnetospheric pickup ions, primarily hydrogen and oxygen. Juno's thermal plasma instrument JADE, the Jovian Auroral Distributions Experiment, has provided comprehensive in situ observations of the composition of Jupiter's plasma sheet ions with its Time‐of‐Flight mass‐spectrometry capabilities. Here, we present observations of the magnetospheric composition in the Europa‐Ganymede region of Jupiter's magnetosphere. We find material from Europa is intermittently present at comparable densities to Io‐genic plasma. The intermittency of Europa‐genic signatures suggests Europa's neutral oxygen toroidal cloud is more localized to Europa's vicinity than its hydrogen cloud. These observations reveal a more complex and compositionally diverse magnetosphere than previously thought. Plain Language Summary: Jupiter's charged particle environment is overwhelmingly driven by material lost from Io. This material interacts with the icy moon Europa, which can also inject charged particles into the environment. We find that Europa appreciably contributes to and modifies its local charged particle environment, revealing a more complex and compositionally diverse magnetosphere than previously thought. Key Points: Three distinct heavy ion populations observed in Jupiter's plasma sheet: Io‐genic plasma, Europa‐genic plasma, and Io‐genic energetic particlesThe mixture of Io‐genic and Europa‐genic plasma varies greatly throughout the Europa‐Ganymede regionWe find evidence Europa's oxygen neutral toroidal clouds are more localized than its hydrogen cloud [ABSTRACT FROM AUTHOR]

Inflation of viscous magma intrusions in Earth's shallow crust often induces strain and fracturing within heterogeneous host rocks and dome‐shaped ground deformation. Most geodetic models nevertheless consider homogeneous, isotropic, and linear‐elastic media wherein stress patterns indicate the potential for failure, but without simulating actual fracturing. We present a two‐dimensional Discrete Element Method (DEM) application to simulate magma recharge in a pre‐existing laccolith intrusion. In DEM models, fractures can propagate during simulations. We systematically investigate the effect of the host rock toughness (resistance to fracturing), stiffness (resistance to deformation) and the intrusion depth, on intrusion‐induced stress, strain, displacement and spatial fracture distribution. Our results show that the spatial fracture distribution varies between two end‐members: (a) for high stiffness or low toughness host rock or a shallow intrusion: extensive cracking, multiple vertical surface fractures propagating downward and two inward‐dipping highly cracked shear zones that connect the intrusion tip with the surface; and (b) for low stiffness or high toughness host rock or a deeper intrusion: limited cracking, one central vertical fracture initiated at the surface, and two inward‐dipping fractures at the intrusion tips. Abrupt increases in surface displacement magnitude occur in response to fracturing, even at constant magma injection rates. Our modeling application provides a novel approach to considering host rock mechanical strength and fracturing during viscous magma intrusion and associated dome‐shaped ground deformation, with important implications for interpreting geodetic signals at active volcanoes and the exploitation of geothermal reservoirs and mineral deposits. Plain Language Summary: Most viscous magmas are stored and solidified in the upper 1–2 km of Earth's crust and rarely reach the surface to produce explosive volcanic eruptions. At such shallow depths, these viscous magmas often form intrusions with a flat base and dome‐shaped roof, or "laccoliths." To accommodate the emplaced volume, the deformation of the host rock produces dome‐shaped ground uplift at the surface. Geological and geophysical observations show that laccolith emplacement often coincides with intense host rock fracturing. However, most of the numerical laccolith emplacement models ignore that fracturing and severely simplify the mechanical response of the host rock. To assess the effect of host rock fracturing on ground deformation, we designed a two‐dimensional Discrete Element Method (DEM) application, which can simulate the fracturing of the host rock during magma injection. We found that varying the strength of the host rock and/or the intrusion depth controls the spatial distribution of fracturing and magnitude of the ground uplift. Our results help to understand complex interplays between the depth of magma injection and the mechanical properties of host rocks, and to improve the modeling tools used to routinely monitor magmatic activity. Key Points: We present a two‐dimensional Discrete Element Method model that simulates host rock fracturing during the inflation of a magmatic laccolithThe host rock toughness and stiffness along with source depth control spatial fracture distribution between two end‐membersAt a constant injection rate, the vertical displacement maximum and lateral extent show sudden changes in response to host rock fracturing [ABSTRACT FROM AUTHOR]

Purpose: There is uncertainty about the effect of increased neonatal protein intake on neurodevelopmental outcomes following preterm birth. The aim of this study was to assess the effect of a change in neonatal nutrition protocol at a major tertiary neonatal intensive care unit intended to increase protein intake on ophthalmic and visual development in school‐age children born very preterm. Methods: The study cohort comprised children (n = 128) with birthweight <1500 g or gestational age < 30 weeks born at Auckland City Hospital before (OldPro group, n = 55) and after (NewPro group, n = 73) a reformulation of parenteral nutrition that resulted in increased total protein intake during the first postnatal week and decreased carbohydrate, total parenteral fluid and sodium intake. Clinical and psychophysical vision assessments were completed at 7 years' corrected age, including visual acuity, global motion perception (a measure of dorsal stream function), stereoacuity, ocular motility and ocular health. Composite measures of favourable overall visual, binocular and functional visual outcomes along with individual vision measures were compared between the groups using logistic and linear regression models. Results: Favourable overall visual outcome did not differ between the two groups. However, global motion perception was better in the NewPro group (p = 0.04), whereas the OldPro group were more likely to have favourable binocular visual outcomes (60% vs. 36%, p = 0.02) and passing stereoacuity (p = 0.02). Conclusions: These results indicate subtle but complex associations between early neonatal nutrition after very preterm birth and visual development at school age. [ABSTRACT FROM AUTHOR]

This study focuses on constraining the role that Callisto's perturbed electromagnetic environment had on energetic charged particle signatures observed during the Galileo mission. To do so, we compare data from the Energetic Particle Detector (EPD) obtained during four close encounters of the moon with a model framework that combines hybrid simulations for low‐energy plasma and test‐particle tracing simulations for high‐energy particles. By comparing model results for energetic particle dynamics in both uniform and perturbed electromagnetic fields, we systematically disentangle the role that geometric effects (i.e., absorption of particles by Callisto's solid surface) have on observed energetic particle signatures compared to those associated with Callisto's perturbed electromagnetic environment (generated by the moon's induced magnetic field and plasma interaction currents). We show that observed flux drop‐outs in the energetic ion pitch angle distributions (PADs) are largely driven by their absorption by Callisto's surface: their large gyroradii exceed the size of the moon, facilitating their impact onto the icy surface and preventing their detection by EPD. However, features observed in the energetic electron PADs can only be explained with an accurate representation of the moon's perturbed environment, since electrons closely follow the orientation of the electromagnetic fields. Our findings therefore illustrate the key role that the moon's induced field and magnetospheric plasma interaction have on the dynamics of energetic electrons, emphasizing the importance of accurately modeling Callisto's locally perturbed electromagnetic environment when attempting to interpret data from past and future encounters, including those anticipated from the upcoming JUICE mission. Plain Language Summary: Jupiter's moon Callisto is continuously exposed to a combination of low‐energy plasma and high‐energy charged particles. As the moon interacts with these populations, its local electromagnetic field environment becomes highly perturbed. During four Callisto encounters during the Galileo mission to Jupiter, a sensor onboard the spacecraft detected clear signatures of the high‐energy ions and electrons. To understand the degree to which Callisto's low‐energy plasma interaction affects these signatures, we systematically model the dynamics of energetic particles as they travel through various electromagnetic field configurations. We find that the energetic ion observations are not strongly affected by the perturbed fields, but instead can be understood in terms of the particles being absorbed by Callisto's solid surface. However, electrons are highly sensitive to the draped fields, and the Galileo observations can only be understood when considering the perturbed electromagnetic environment near the moon. Our results underscore the importance of accurately modeling Callisto's perturbed environment when hoping to understand energetic particle signatures observed during the upcoming JUICE mission. Key Points: We compare energetic charged particle data with a model to explain pitch angle distributions observed during four Galileo flybys of CallistoElectron flux drop‐outs are shaped by the perturbed fields associated with Callisto's induced field and magnetospheric plasma interactionObserved ion fluxes can be mainly explained through geometric considerations, with Callisto's surface shadowing particles from detection [ABSTRACT FROM AUTHOR]

The localized crustal magnetic fields of Mars play an important role in the planet's ionosphere‐solar wind interaction. Various physical processes in the induced magnetosphere, such as particle precipitation, field‐aligned currents, and ion outflow, are usually associated with the crustal magnetic cusp regions, where field lines are mostly vertical and open to space. Due to the small spatial scale (a few hundred km) of the Martian crustal magnetic cusps, localized models with high spatial resolutions and ion kinetics are needed to understand the physical processes. We adapt the simulation platform HYB developed at the Finnish Meteorological Institute to a moderately strong magnetic cusp above the Martian exobase with a 2‐D simulation domain assuming periodic boundary conditions on the third dimension. Two plasma sources are included in the simulation: hot protons from the induced magnetosphere and cold heavy ions (O+) from the ionosphere. Our model results can qualitatively reproduce the vertical electric potential drop, particle transport, and field aligned current in the cusp region. The vertical electric potential is built up mostly by the Hall electric field as a result of the separation between ion and electron fluxes of the downward plasma flow. By varying the model inputs, we found that the vertical potential drop depends on ionospheric ion density and magnetic field strength. These results tell us that energy is transferred from magnetospheric plasma to ionospheric plasma through the vertical electric potential buildup in magnetic cusps and how this process may affect electron precipitation, ion escape, and ionosphere conditions at Mars. Key Points: A hybrid model qualitatively reproduced the vertical potential drop and field aligned currents in Martian crustal magnetic cusp regionsThe vertical electric potential drop is mostly from the Hall electric field as a result of energy input from the downward plasma flowThe vertical electric potential drop decreases with ionospheric ion density and increases with magnetic field strength [ABSTRACT FROM AUTHOR]

Background: Surface‐guided radiation therapy (SGRT) systems have been widely installed and utilized on linear accelerators. However, the use of SGRT with proton therapy is still a newly developing field, and published reports are currently very limited. Purpose: To assess the clinical application and alignment agreement of SGRT with CT‐on‐rails (CTOR) and kV‐2D image‐guided radiation therapy (IGRT) for breast treatment using proton therapy. Methods: Four patients receiving breast or chest wall treatment with proton therapy were the subjects of this study. Patient #1′s IGRT modalities were a combination of kV‐2D and CTOR. CTOR was the only imaging modality for patients #2 and #3, and kV‐2D was the only imaging modality for patient #4. The patients' respiratory motions were assessed using a 2‐min surface position recorded by the SGRT system during treatment. SGRT offsets reported after IGRT shifts were recorded for each fraction of treatment. The agreement between SGRT and either kV‐2D or CTOR was evaluated. Results: The respiratory motion amplitude was <4 mm in translation and <2.0° in rotation for all patients. The mean and maximum amplitude of SGRT offsets after application of IGRT shifts were ≤(2.6 mm, 1.6°) and (6.8 mm, 4.5°) relative to kV‐2D‐based IGRT; ≤(3.0 mm, 2.6°) and (5.0 mm, 4.7°) relative to CTOR‐based IGRT without breast tissue inflammation. For patient #3, breast inflammation was observed for the last three fractions of treatment, and the maximum SGRT offsets post CTOR shifts were up to (14.0 mm, 5.2°). Conclusions: Due to the overall agreement between SGRT and IGRT within reasonable tolerance, SGRT has the potential to serve as a valuable auxiliary IGRT tool for proton breast treatment and may improve the efficiency of proton breast treatment. [ABSTRACT FROM AUTHOR]

Efforts to tailor instruction to match students' purported learning style continue to be used in higher education despite evidence challenging their value. Students were matched and mismatched to their self‐reported online learning preference to investigate the impact on academic outcomes. A total of 114 graduate health students were randomly assigned to an online lecture either matching or mismatching their previously reported preference (synchronous or asynchronous lecture participation). All students took the same multiple‐choice examination following the lecture. Independent t‐test analysis revealed no significant differences between students who were matched and mismatched to their participation preference. Asynchronous groups achieved significantly higher scores than synchronous groups. Analysis via two‐way ANOVA revealed no significant interaction between method of participation and compatibility with learning preference on examination scores. Based on the results of this study, method of participation impacted examination performance; however, matching or mismatching to students' stated learning preference did not impact performance. [ABSTRACT FROM AUTHOR]

Solar wind ions weather the optical, physical, and chemical properties of the lunar surface. While the solar wind ion number density is dominated by the thermal population, the study of suprathermal ions is important to understand weathering effects that may develop at depth larger than the penetration depth of the bulk solar wind. Possible manifestations of suprathermal ion weathering include the creation of thick amorphous rims, contamination of isotopic ratios at depth, and alteration of the optical reflectance at infrared wavelengths. Furthermore, while the thermal population forms a beam parallel to the ecliptic plane, suprathermal ions may have a large northward or southward velocity component and can therefore directly access and weather the lunar polar regions, including the interiors of the Permanently Shadowed Regions (PSRs). In this article, we constrain the long‐term properties of the solar wind suprathermal ions using 17 years of observations by the SupraThermal Ion Composition Spectrometer onboard the Wind spacecraft (Wind‐STICS). We find that the 17‐year omnidirectional energy spectra of protons, helium ions, and oxygen ions observed by Wind‐STICS are in excellent agreement with the 11‐month estimates published by Mewaldt et al. (2001, https://doi.org/10.1063/1.1433995) and Mewaldt et al. (2007, https://doi.org/10.1007/978-0-387-74184-0%5f32). This agreement validates the conclusions of Nénon and Poppe (2020, https://doi.org/10.3847/PSJ/abbe0c) who proposed that suprathermal ions heavier than helium may increase the rate of amorphous rim formation in lunar samples by 50%. Furthermore, the Wind‐STICS observations of out‐of‐ecliptic ions reveal that the lunar PSRs are weathered by the same flux of >15 keV/nucleon as anywhere else on the lunar surface. Plain Language Summary: The lunar surface is directly exposed to space and constantly bombarded by positively charged particles known as "ions." These particles in turn modify the optical, physical, and chemical properties of the planetary surface. In this article, we use 17 years of ion observations by the Wind spacecraft to constrain the long‐term‐averaged characteristics of the ions flowing in the solar wind with a velocity much greater than the solar wind group speed. Owing to their greater velocity, these fast ions can modify the surface at larger depth than typical solar wind particles. We find that the long‐term 17‐year flux of fast ions observed by Wind is consistent with an 11‐month estimate previously published in 2001. We also find that the fluxes of ions flowing in and out of the ecliptic plane, where most planets orbit, become similar above a minimum ion velocity. This finding reveals that the interiors of the lunar polar craters, which are not exposed to the typical solar wind, are in fact altered by at least these out‐of‐ecliptic ions. The presented characterization of precipitating ions is a first step toward understanding the alteration of polar craters by space plasma ions, including the sources and sinks of water ice. Key Points: Wind‐STICS constrains the long‐term flux of the suprathermal solar wind ions that weather the lunar surfaceThe 17‐year‐averaged energy spectra of protons, helium ions, and oxygen ions are in agreement with an 11‐month estimate published in 2001Lunar Permanently Shadowed Regions are weathered by the same flux of >15 keV/nucleon ions as anywhere else on the lunar surface [ABSTRACT FROM AUTHOR]

Molluscum contagiosum (MC) is a contagious infection that, although benign, can become an aesthetic burden and lead to other opportunistic infections, secondary dermatitis, and self‐isolation. Currently, several treatment options are available for MC, including the newly investigated nitric oxide‐releasing berdazimer gel, leading this review to evaluate randomized controlled trials (RCT) comparing berdazimer gel with a vehicle for treating MC. The meta‐analysis included three reports and four RCT involving 1854 patients, with 1106 (59.6%) randomized to receive berdazimer. Our findings suggest that berdazimer is effective in the management of MC lesions, but the increased clearance of lesions and reduction of scarring must be weighed against the potential for topical adverse effects, particularly when considering the use of this therapy in pediatric patients. [ABSTRACT FROM AUTHOR]

Lunar surface charging is a scientifically and practically important topic at the Moon that is largely determined by the electron currents near the surface. Among those electron populations, lunar photoelectrons (PHE) and backscattered electrons (BSE) produced by incident electrons that make up the high‐energy tail of lunar emitted electrons are not well characterized yet. Recently, Xu et al. (2021, https://doi.org/10.1029/2020je006790) reported oxygen Auger electron observations at the Moon by the Acceleration, Reconnection, Turbulence, and Electrodynamics of the Moon's Interaction with the Sun spacecraft, which provides a unique feature to identify lunar photoelectrons. We utilize this feature to isolate cases of emitted electrons dominated by BSE over PHE. With selected BSE cases, we characterize how the backscattering coefficient η varies with primary electron energy, which decreases with increasing energy. Our results also reveal η to be dependent on the magnetic dip angle, as a fraction of BSE re‐impact the surface in a magnetized environment. The characterization of the backscattering coefficient not only gives insights into the lunar surface properties and lunar surface charging but could also be potentially applied to other airless bodies. Plain Language Summary: Lunar surface is electrically charged to different degrees depending on the space environment of the Moon. Lunar surface charging is an important topic for robotic and human lunar exploration, as well as scientific observations from the surface. One of the quantities related to the lunar surface charging is the backscattering coefficient, which represents the probability that an incident electron is backscattered away from the lunar surface after impact as opposed to be absorbed by the surface. This study provides estimates of the electron backscattering probability with measurements from the Acceleration, Reconnection, Turbulence, and Electrodynamics of the Moon's Interaction with the Sun spacecraft. We have determined the probability to be 0.1–0.3 at different electron energies. This is also affected by the magnetized environment at the Moon, causing some initially scattered electrons to return to the surface. The characterization of the backscattering coefficient not only gives insights into lunar surface charging and the lunar surface properties but could also be potentially applied to other airless bodies. Key Points: We utilize the oxygen Auger electron peak to isolate cases of emitted electrons dominated by backscattered electrons (BSE) over photoelectronsWe derive the electron backscattering coefficient η of the lunar surface to be 0.1–0.3 for 50–600 eVWe reveal η to be dependent on the magnetic dip angle, as some BSE re‐impact the surface in a magnetized environment [ABSTRACT FROM AUTHOR]

Due to the lack of a dense atmosphere, the Moon directly interacts with ambient plasmas and solar radiation, leading to lunar surface charging. Solar X‐rays drive the emission of photoelectrons and Auger electrons from the lunar surface to space. The Auger electrons have characteristic energies intrinsic to the photo‐emitting atoms and were recently identified at the Moon by Acceleration, Reconnection, Turbulence, and Electrodynamics of the Moon's Interaction with the Sun (ARTEMIS) observations. In this study, we developed a numerical model of the energy spectrum of lunar photoelectrons and Auger electrons, thereby comparing the predicted and observed energy spectra. By adjusting a scaling factor, the model well reproduces the ARTEMIS observations obtained in the solar wind, where the energy spectra are minimally affected by surface charging. Meanwhile, the energy spectra obtained in the geomagnetic tail can be significantly altered by lunar surface potentials. We show that it is difficult to determine a unique combination of the scaling factor and the lunar surface potential with the ARTEMIS energy resolution because of a strong parameter degeneracy. Nevertheless, for a fixed scaling factor, a strong correlation is identified between the lunar surface potentials inferred from the shifts of the energy spectra and those from the upward photoelectron beam energies, providing a proof of concept for the use of the photo‐emitted electrons as a new remote sensing tool of the lunar surface potential. We advocate for future observations of lunar electrons with a high energy resolution. Key Points: We developed a numerical model of the energy spectrum of photoelectrons and Auger electrons emitted from the sunlit lunar surfaceThe model successfully reproduces Acceleration, Reconnection, Turbulence, and Electrodynamics of the Moon's Interaction with the Sun observations of upward‐traveling electrons from the sunlit lunar surfaceThe data‐model comparison suggests that the emitted electrons can be used as a new tool to remotely infer the lunar surface potential [ABSTRACT FROM AUTHOR]

We analyze the emission of energetic neutral atom (ENA) flux from charge exchange between Jovian magnetospheric ions and the atmospheres of Callisto and Europa. For this purpose, we combine the draped electromagnetic fields from a hybrid plasma model with a particle tracing tool for the energetic ions. We determine the ENA flux through a concentric sphere located just outside of each moon's atmosphere, thereby capturing the complete physics imprinted in these emission patterns. In order to constrain the modifications to the ENA emissions that arise from the periodic change of the ambient plasma conditions, we calculate the emission morphology at multiple positions during a Jovian synodic rotation. To isolate the influence of field line draping, we compare to the emission patterns in uniform fields. Our major results are: (a) At Europa and Callisto, the majority of detectable ENA emissions are concentrated into a band normal to the Jovian magnetospheric field. (b) The fraction of observable ENA flux that contributes to this band depends on the number of complete gyrations that the parent ions can complete within the moon's atmosphere. (c) Field line draping partially deflects impinging parent ions around both moons, thereby attenuating the ENA flux and driving significant morphological changes to the emission patterns. (d) The band of elevated ENA flux is locally maximized on the opposite (antipodal) side of the moon where the flux is locally minimized. At Europa, detectable ENA emissions are maximized slightly west of the ramside apex. At Callisto, they maximize near the Jupiter‐facing apex. Key Points: We model the energetic neutral atom (ENA) flux generated by charge exchange of magnetospheric ions with Callisto's and Europa's atmospheresThe bulk of the ENA flux is detectable in a band normal to the magnetospheric field and created by ions with pitch angles near 90°Magnetic field line draping attenuates the intensity of observable ENA flux and qualitatively alters the emission morphology at both moons [ABSTRACT FROM AUTHOR]

Observations of Callisto's atmosphere have indicated an O2 component should exist, but the evolution from its initial source to its inferred steady‐state abundance is not well understood. Herein we constrain the production of O2 via radiolysis within Callisto's exposed ice patches and determine the corresponding O2 column density. To do so, for the first time we simulate the thermal and energetic components of the Jovian magnetospheric plasma irradiating Callisto's atmosphere and estimate energy deposited therein by the impinging charged particles along their trajectories to the surface. We then calculate O2 source fluxes corresponding to the energy of the impacting plasma fluxes, which is coupled with estimated atmospheric lifetimes to determine the steady‐state abundance of O2. Our results suggest that production of O2 via radiolysis within the exposed ice on Callisto's surface does not produce a sufficiently dense atmosphere relative to the column densities inferred from observations by about 2–3 orders of magnitude. To resolve this discrepancy between estimated and observed abundances, we provide the first estimates for other potential sources of atmospheric O2. We also make similar estimates for the production of H2 in Callisto's atmosphere relative to constraints provided in the literature, and the conclusion is the same: a sufficiently dense atmosphere is not produced. Thus, we have shown that a better understanding of the production and fate of radiolytic products in Callisto's regolith is required in order to place firmer constraints on the generation mechanisms of its atmosphere in preparation for future observations. Plain Language Summary: Molecular oxygen (O2) has been inferred to exist in Callisto's atmosphere from observations taken across more than two decades by three separate instruments each using distinct measurement techniques. Exposure of Callisto's icy surface by the ions and electrons trapped in Jupiter's magnetic field is expected to produce O2, which subsequently releases into an atmosphere around Callisto. However, prior to this study, the amount of O2 produced through such pathways has not been explicitly quantified. Here, for the first time, we determine the amount of O2 produced by the irradiation of the exposed ice on Callisto's surface by Jupiter's plasma after depositing energy in the atmosphere. Our results show that this source of O2 does not produce nearly enough compared to what has been inferred from observations. Therefore, additional production mechanisms of O2 are required at Callisto. Key Points: We estimate the energy deposited by the thermal and energetic components of the Jovian magnetospheric plasma in Callisto's atmosphereWe calculate O2 column densities in Callisto's atmosphere corresponding to the energies of the plasma fluxes impacting the surfaceRadiolysis in the exposed ice on Callisto's surface is an insufficient source to produce the amount of O2 inferred from observations [ABSTRACT FROM AUTHOR]

The reflection of solar wind protons as energetic neutral atoms (ENAs) from the lunar surface has regularly been used to study the plasma‐surface interaction at the Moon. However, there still exists a fundamental lack of knowledge of the scattering process. ENA emission from the surface is expected to similarly occur at Mercury and will be studied by BepiColombo. Understanding this solar wind backscattering will allow studies of both Mercury's plasma environment as well as properties of the hermean surface itself. Here, we expand on previous simulation studies of the solar‐wind‐regolith interaction with 3D grains in SDTrimSP‐3D to compare the predicted scattering energies and angles to ENA measurements from the Moon by the Chandrayaan‐1 and IBEX missions. The simulations reproduce a backward emission toward the Sun, which can be connected to the geometry of the regolith grain stacking. In contrast, the ENA energy distribution and its Maxwellian shape is mostly connected to the solar wind velocity. Our simulations also correctly describe a lunar ENA albedo between 10% and 20% and support its decrease with solar wind velocity. We further expand our studies to illustrate how BepiColombo will be able to observe ENAs at Mercury using hybrid simulations of Mercury's magnetosphere as an input for the complex surface precipitation patterns. We demonstrate that the variable ion precipitation will directly influence ENA emission from the surface. The orbits of BepiColombo's Mercury Planetary Orbiter and Mercury Magnetospheric Orbiter/Mio spacecraft are shown to be suitable to observe ENA emission patterns both on a local and a global scale. Plain Language Summary: The Sun emits a continuous stream of charged particles, the solar wind. Recently, it was observed that these solar wind particles get reflected from the Moon in a similar way as it is the case for light from the Sun. The reflection is the result of a large number of collisions between the solar wind particles and atoms at the Moon's surface. This is expected to occur similarly at the planet Mercury. To better understand this process, we present a theoretical model of the reflection process. Our simulations take into account all the collisions with atoms, as well as the geometry of the lunar soil as a large number of loosely stacked grains. The model achieves very good agreement with most of the observations from the Moon, showing that sunward scattering and the scattering probability can be explained by the porous regolith. Consequently, we also sketch how particle scattering would occur at Mercury, where the solar wind only reaches the surface at select locations due to the planet's magnetic field. Our results confirm the variability of the scattered particles around Mercury and that the BepiColombo mission is well‐suited to observe them for imaging solar wind impacts onto the surface. Key Points: We model the solar wind proton reflection from lunar regolith grains to study energetic neutral atom (ENA) emission characteristicsENA emission angles are successfully connected to the regolith geometry, while ENA energies are mostly determined by the solar wind energyExpanding the model to Mercury, we predict ENA fluxes that will be observed by BepiColombo [ABSTRACT FROM AUTHOR]

Background and purpose: As a part of the commissioning and quality assurance in proton beam therapy, lateral dose profiles and output factors have to be acquired. Such measurements can be performed with point detectors and are especially challenging in small fields or steep lateral penumbra regions as the detector's volume effect may lead to perturbations. To address this issue, this work aims to quantify and correct for such perturbations of six point detectors in small proton fields created via three different delivery techniques. Methods: Lateral dose profile and output measurements of three proton beam delivery techniques (pencil beam scanning, pencil beam scanning combined with collimators, passive scattering with collimators) were performed using high‐resolution EBT3 films, a PinPoint 3D 31022 ionization chamber, a microSilicon diode 60023 and a microDiamond detector 60019 (all PTW Freiburg, Germany). Detector specific lateral dose response functions K(x,y) acting as the convolution kernel transforming the undisturbed dose distribution D(x,y) into the measured signal profiles M(x,y) were applied to quantify perturbations of the six investigated detectors in the proton fields and correct the measurements. A signal theoretical analysis in Fourier space of the dose distributions and detector's K(x,y) was performed to aid the understanding of the measurement process with regard to the combination of detector choice and delivery technique. Results: Quantification of the lateral penumbra broadening and signal reduction at the fields center revealed that measurements in the pencil beam scanning fields are only compromised slightly even by large volume ionization chambers with maximum differences in the lateral penumbra of 0.25 mm and 4% signal reduction at the field center. In contrast, radiation techniques with collimation are not accurately represented by the investigated detectors as indicated by a penumbra broadening up to 1.6 mm for passive scattering with collimators and 2.2 mm for pencil beam scanning with collimators. For a 3 mm diameter collimator field, a signal reduction at field center between 7.6% and 60.7% was asserted. Lateral dose profile measurements have been corrected via deconvolution with the corresponding K(x,y) to obtain the undisturbed D(x,y). Corrected output ratios of the passively scattered collimated fields obtained for the microDiamond, microSilicon and PinPoint 3D show agreement better than 0.9% (one standard deviation) for the smallest field size of 3 mm. Conclusion: Point detector perturbations in small proton fields created with three delivery techniques were quantified and found to be especially pronounced for collimated small proton fields with steep dose gradients. Among all investigated detectors, the microSilicon diode showed the smallest perturbations. The correction strategies based on detector's K(x,y) were found suitable for obtaining unperturbed lateral dose profiles and output factors. Approximation of K(x,y) by considering only the geometrical averaging effect has been shown to provide reasonable prediction of the detector's volume effect. The findings of this work may be used to guide the choice of point detectors in various proton fields and to contribute toward the development of a code of practice for small field proton dosimetry. [ABSTRACT FROM AUTHOR]

This study presents observations of Solar Energetic Particle (SEP) protons that have penetrated Earth's magnetotail to reach the lunar environment. We apply data from Wind as an upstream monitor and compare to observations from THEMIS‐ARTEMIS within the tail to show clear signatures of SEPs at the Moon during two events. Combining modeling and data analysis, we show that SEPs above energies of ∼25 keV gain access to the Moon's position deep within the magnetotail through field lines that are open on one end to the solar wind. These results contradict previous studies that have suggested that the magnetotail is effective in shielding the Moon from SEPs with energies up to 1 GeV. Instead, we highlight that Earth's magnetosphere provides poor protection to the Moon from SEPs, which irradiate the lunar surface even within the tail. Our results have important implications regarding the safety of astronauts during upcoming lunar missions. Plain Language Summary: During two thirds of its orbit, the Moon is located outside of Earth's magnetosphere. At these locations, the lunar surface is exposed to a variety of charged particles including (low‐energy) solar wind plasma and (high‐energy) Solar Energetic Particles (SEPs), the latter of which are responsible for weathering and chemically altering the lunar surface. For the remaining one third of its orbit, the Moon is located within Earth's magnetosphere. Previous studies have suggested that the ambient magnetic field within this cavity shields the Moon from the highly energetic SEPs. However, we report clear observations by NASA's THEMIS‐ARTEMIS mission of these potentially hazardous charged particles when the Moon was embedded deep within Earth's magnetosphere. We also apply computer simulations to illustrate that Earth's magnetic tail is porous, allowing SEPs to efficiently leak into the terrestrial magnetosphere. Our findings are therefore highly relevant for the safety of astronauts during the upcoming missions to explore the lunar environment. Key Points: The two Acceleration, Reconnection, Turbulence, and Electrodynamics of the Moon's Interaction with the Sun probes observe Solar Energetic Particle (SEP) events at the Moon when located deep within the terrestrial magnetotailSEPs enter the magnetotail far downstream beyond the lunar orbit, along open field lines that are connected on one end to Earth's polar capsThe terrestrial magnetosphere is ineffective in shielding SEPs from accessing the lunar orbit while within the magnetotail [ABSTRACT FROM AUTHOR]

We use data from the plasma and energetic particle instruments on the Juno spacecraft, JADE and JEDI, to study the equatorial pitch angle distributions of energetic protons within Jupiter's inner magnetosphere during Juno's prime mission from 2016 to 2021. Averaging over all observations made by Juno within M‐shell bins between M = 6 and M = 30, we find protons at energies between 10 and 50 keV are predominantly field‐aligned at all M‐shells. In contrast, those at energies above 200 keV transition from being predominantly field‐aligned at M = 20 to having pancake‐like distributions at M < 10. We find the observed distributions are consistent either with charge exchange of protons with neutral toroidal clouds, or with adiabatic acceleration of protons originating from Jupiter that are transported inward from the middle magnetosphere. Plain Language Summary: Protons are seen throughout Jupiter's magnetosphere. Where these protons come from and how they evolve is not well understood. Previous observations by the Galileo spacecraft showed that protons in the vicinity of Europa have properties consistent with charge exchange with a neutral species, which effectively removes the charged particles from the magnetosphere. Using data from the Juno spacecraft, we survey proton distributions at different energies. Although charge exchange remains a plausible explanation for the observations, another possibility is that the distribution is a result of adiabatically transporting the protons through Jupiter's magnetic field. Key Points: 10–50 keV protons at Jupiter are predominantly field‐aligned at M‐shells between M = 7 and M = 20Normalized pitch angle distributions of >200 keV protons show evidence of adiabatic acceleration during inward radial transportObserved proton distributions could result from charge‐exchange with neutrals or conservation of adiabatic invariants during transport [ABSTRACT FROM AUTHOR]

The Pm3‾n cubic and other low‐symmetry Frank–Kasper phases are known to be formed by soft spheres, ranging from metals to block copolymer micelles and colloidal nanoparticles. Here, we report a series of X‐shaped polyphiles composed of sticky rods and two non‐symmetric branched side‐chains, which self‐assemble into the first example of a cubic liquid‐crystalline phase representing a tetrahedral network of rods with a Pm3‾n lattice. It is the topological dual to the Weaire–Phelan foam, being the Voronoi tessellation of the A15 sphere packing, from which this network is obtained by Delaunay triangulation. [ABSTRACT FROM AUTHOR]

Aims: We investigated titration patterns of angiotensin‐converting enzyme inhibitors (ACEis)/angiotensin receptor blockers (ARBs) and beta‐blockers, quality of life (QoL) over 6 months, and associated 1 year outcome [all‐cause mortality/heart failure (HF) hospitalization] in a real‐world population with HF with reduced ejection fraction (HFrEF). Methods and results: Participants with HFrEF (left ventricular ejection fraction <40%) from a prospective multi‐centre study were examined for use and dose [relative to guideline‐recommended maintenance dose (GRD)] of ACEis/ARBs and beta‐blockers at baseline and 6 months. 'Stay low' was defined as <50% GRD at both time points, 'stay high' as ≥50% GRD, and 'up‐titrate' and 'down‐titrate' as dose trajectories. Among 1110 patients (mean age 63 ± 13 years, 16% women, 26% New York Heart Association Class III/IV), 714 (64%) were multi‐ethnic Asians from Singapore and 396 were from New Zealand (mainly European ethnicity). Baseline use of either ACEis/ARBs or beta‐blockers was high (87%). Loop diuretic was prescribed in >80% of patients, mineralocorticoid receptor antagonist in about half of patients, and statins in >90% of patients. At baseline, only 11% and 9% received 100% GRD for each drug class, respectively, with about half (47%) achieving ≥50% GRD for ACEis/ARBs or beta‐blockers. At 6 months, a large majority remained in the 'stay low' category, one third remained in 'stay high', whereas 10–16% up‐titrated and 4–6% down‐titrated. Patients with lower (vs. higher) N‐terminal pro‐beta‐type natriuretic peptide levels were more likely to be up‐titrated or be in 'stay high' for ACEis/ARBs and beta‐blockers (P = 0.002). Ischaemic aetiology, prior HF hospitalization, and enrolment in Singapore (vs. New Zealand) were independently associated with higher odds of 'staying low' (all P < 0.005) for prescribed doses of ACEis/ARBs and beta‐blockers. Adjusted for inverse probability weighting, ≥100% GRD for ACEis/ARBs [hazard ratio (HR) = 0.42; 95% confidence interval (CI) 0.24–0.73] and ≥50% GRD for beta‐blockers (HR = 0.58; 95% CI 0.37–0.90) (vs. Nil) were associated with lower hazards for 1 year composite outcome. Country of enrolment did not modify the associations of dose categories with 1 year composite outcome. Higher medication doses were associated with greater improvements in QoL. Conclusions: Although HF medication use at baseline was high, most patients did not have these medications up‐titrated over 6 months. Multiple clinical factors were associated with changes in medication dosages. Further research is urgently needed to investigate the causes of lack of up‐titration of HF therapy (and its frequency), which could inform strategies for timely up‐titration of HF therapy based on clinical and biochemical parameters. [ABSTRACT FROM AUTHOR]

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Obstructive sleep apnoea (OSA) is a common disorder characterized by recurrent episodes of apnoea or hypopnea due to total or partial pharyngeal collapse and temporary upper airway obstruction during sleep. The prevalence of OSA is increasing and currently affects about 30% of men and 13% of women in Europe. Intermittent hypoxia, oxidative stress, systemic inflammation, and sleep fragmentation resulting from OSA can provoke subsequent cardiometabolic disorders. The relationships between endocrine disorders and OSA are complex and bidirectional. Indeed, several endocrine disorders are risk factors for OSA. Compared with the general population, the prevalence of OSA is increased in patients with obesity, hypothyroidism, acromegaly, Cushing syndrome, and type 1 and 2 diabetes. In some cases, treatment of the underlying endocrine disorder can improve, and occasionally cure, OSA. On the other hand, OSA can also induce endocrine disorders, particularly glucose metabolism abnormalities. Whether continuous positive airway pressure (CPAP) treatment for OSA can improve these endocrine disturbances remains unclear due to the presence of several confounding factors. In this review, we discuss the current state‐of‐the‐art based on the review of the current medical literature for key articles focusing on the bidirectional relationship between endocrine disorders and OSA and the effects of treatment. Screening of OSA in endocrine patients is also discussed, as it remains a subject of debate. [ABSTRACT FROM AUTHOR]

ESA's Mars Express (MEX) may have observed twice solar wind protons backscattered by Phobos. However, these detections remain uncertain and call for an independent confirmation. Here, we analyze the proton measurements collected by the Suprathermal And Thermal Ion Composition experiment onboard NASA's Mars Atmosphere and Volatile EvolutioN mission (MAVEN) during the 15 closest encounters of MAVEN with Phobos (closest approach between 80 and 370 km). We use a model of magnetic connectivity to the Martian bow shock and an exospheric pickup ion model to identify the origin of the protons observed close to the Martian moon. We find no evidence of protons backscattered by Phobos. Instead, foreshock‐shock foot protons and Martian exospheric pickup protons are often observed near Phobos. These results put into new context not only the past MEX detections, but also the future observation attempts of the upcoming JAXA Martian Moons Exploration mission. Plain Language Summary: The surface a solar system body that does not have an atmosphere can be directly bombarded and processed by the small positively charged particles ejected by the Sun, known as solar wind ions. At the Earth Moon, previous work discovered that 0.1%–1% of the solar wind protons hitting the lunar surface are backscattered in space as charged particles instead of traveling through the planetary surface. The only other place where this fundamental process may have been detected so far is Phobos, a small rocky moon that orbits the red planet Mars. Indeed, ESA's satellite Mars Express (MEX) may have previously observed such protons at Phobos, but these detections remain uncertain. To advance on the question of solar wind proton backscattering at Phobos, we analyze in this article the proton measurements gathered by NASA's Mars Atmosphere and Volatile EvolutioN mission (MAVEN) mission close to Phobos. Models are employed to identify the origin of the protons observed by MAVEN and we find no evidence of protons backscattered by the Martian moon. This result puts into new context the past MEX detections and the future observation attempts of the upcoming JAXA Martian Moons Exploration mission. Key Points: Mars Atmosphere and Volatile EvolutioN mission (MAVEN) flew by Phobos 15 times at a distance lower than 370 kmWe find no evidence of solar wind protons backscattered by the surface of Phobos in the MAVEN proton measurementsForeshock—shock foot protons and exospheric pickup protons are often detected and can be misidentified as solar wind backscattered protons [ABSTRACT FROM AUTHOR]

The porosity of the upper layers of regolith is key to the interaction of an airless planetary body with precipitating radiation, but it remains difficult to characterize. One of the effects that is governed by regolith properties is Energetic Neutral Atom (ENA) emission in the form of reflected and neutralized solar wind protons. We simulate this process for the surface of the Moon by implementing a regolith grain stacking in the ion‐solid‐interaction software SDTrimSP‐3D, finding that proton reflection significantly depends on the regolith porosity. Via comparison with ENA measurements by Chandrayaan‐1, we derive a globally averaged porosity of the uppermost regolith layers of 0.85−0.14+0.15 $0.8{5}_{-0.14}^{+0.15}$. These results indicate a highly porous, fairy‐castle‐like nature of the upper lunar regolith, as well as its importance for the interaction with impacting ions. Our simulations further outline the possibility of future regolith studies with ENA measurements, for example, by the BepiColombo mission to Mercury. Plain Language Summary: The Moon's surface is covered with regolith, a soil made up of stacked grains. Properties of this regolith influence how the Moon interacts with its environment. One example of such an effect are impact by charged particles emitted from the Sun called the "solar wind." We now present simulations of the reflection of such particles from the surface of the Moon, taking into account the grain structure of the regolith. We only find an agreement between the simulations and spacecraft measurements of reflected solar wind particles for very loosely stacked grains. Overall, the amount of reflected particles significantly depends on the structure of the regolith. Our simulations predict that 85% of the volume in the regolith is made up of empty space between grains. These results thus show how measurements of reflected particles can be applied for studying soil properties of the Moon, as well as other planetary bodies such as Mercury. Key Points: Reflection of solar wind protons from lunar regolith is simulated with SDTrimSP‐3DA precise agreement with spacecraft measurements of energetic neutral atom emission is only found for highly porous regolith structuresA lunar regolith porosity of 0.85−0.14+0.15 $0.8{5}_{-0.14}^{+0.15}$ is derived from solar wind proton reflection, which could also be applied to other airless bodies [ABSTRACT FROM AUTHOR]

This study investigates how Callisto's perturbed electromagnetic environment—generated by the moon's interaction with the low‐energy Jovian magnetospheric plasma—affects the dynamics of high‐energy ions and electrons. We constrain how these perturbed fields influence the energetic particle fluxes deposited onto the top of Callisto's atmosphere between energies of 4.5 keV ≤ E ≤ 11.8 MeV. We use a hybrid simulation to model the variability in Callisto's perturbed electromagnetic environment over a synodic period by considering three representative scenarios of the moon's plasma interaction, corresponding to various distances of the moon to the Jovian magnetospheric current sheet. The local field perturbations are maximized near the center of the sheet (forming, e.g., signatures of field‐line pileup, draping, and Alfvén wings) whereas far from the sheet, a mere superposition of the moon's induced dipole with the background field largely explains the perturbations. We then apply a test‐particle approach to investigate the dynamics of energetic electrons and ions (protons, oxygen, and sulfur) while exposed to these fields. Since electron gyroradii are smaller than Callisto, the field perturbations generate small‐scale non‐uniformities in their flux patterns onto the moon, while the ion flux patterns are more homogeneous. Energetic electrons dominate the number flux onto the atmosphere, whereas ions dominate the energy flux. Over a synodic period, the flux patterns onto Callisto's exobase closely resemble those when the moon is near the current sheet center, since the differential energetic particle fluxes in the ambient plasma decrease by an order of magnitude when the moon travels far outside of the sheet. Plain Language Summary: Callisto's ambient plasma environment is comprised of low‐ and high‐energy particles from Jupiter's magnetosphere that continually bombard the moon. Callisto's interaction with the low‐energy population generates currents that locally perturb the electric and magnetic fields, the structures of which vary periodically over a full rotation of Jupiter. These perturbed electromagnetic fields, in turn, strongly affect the dynamics of the high‐energy population—particles that are responsible for partially ionizing Callisto's atmosphere and sputtering the icy surface. This study constrains the degree to which these energetic ions and electrons are affected by Callisto's perturbed electromagnetic environment. We investigate how the high‐energy irradiation of Callisto's atmosphere varies not only with latitude and longitude, but also throughout the moon's orbit around its parent planet. We show that the electron influx patterns strongly depend on Callisto's location within the Jovian magnetosphere, while the ion patterns are more robust against changes to the moon's local environment. Key Points: We calculate the effect of Callisto's perturbed electromagnetic environment on energetic particle fluxes onto the top of the atmosphereElectron flux patterns are strongly affected by Callisto's plasma interaction, while ion fluxes are nearly uniform in the perturbed fieldsFluxes onto the exobase are largest within the Jovian current sheet, despite strong field perturbations generated by the plasma interaction [ABSTRACT FROM AUTHOR]

The lunar exosphere is an ensemble of multiple overlapping, noninteracting neutral distributions that reflect the primary physical processes acting on the lunar surface. While previous observations have detected and constrained the behavior of some species, many others have only circumstantial evidence or theoretical modeling suggesting their presence. Many species are so tenuous as to be unobservable by direct neutral sampling, yet in comparison, measurements in their ionized form provide a particularly sensitive method of detection. To better aid the interpretation of past measurements and planning of future observations, we present a model for the production of lunar pickup ions from the Moon consisting of two components: An analytic model for the distributions of 18 neutral species produced by various mechanisms and an analytic model for the ionization and subsequent acceleration of 20 exospheric and surface‐sputtered pickup ion species. The dominant lunar pickup ions in the model are H2+ ${\mathrm{H}}_{2}^{+}$, He+, CO+, 40Ar+, Al+, Na+, K+, Si+, Ca+, and O+ with an asymmetric distribution favoring the positive interplanetary electric field hemisphere of the Moon. We compare the model predictions to statistically averaged pickup ion fluxes around the Moon as observed by the ARTEMIS spacecraft over the past decade. By filtering for interplanetary electric field‐aligned, high‐energy observations, we find that the pickup ion model lacks an additional source of heavy species. We suggest that a dense CO2 exosphere of 3 × 104 − 1 × 105 cm−3 could account for the missing pickup ion flux as part of the recycling of solar wind carbon ions incident to the Moon. Plain Language Summary: The Moon is surrounded by a thin neutral atmosphere comprised of multiple atomic and molecular species. This atmosphere, technically termed an "exosphere," is produced by multiple processes that are either internal or external to the Moon. As exospheric atoms and molecules are exposed to space, they are continuously ionized by photons, protons, and electrons from the Sun. Once ionized, these particles are accelerated by electromagnetic fields in interplanetary space and often lost from the Moon's environment. These "pickup ions" (so called because they are "picked up" into and carried along with the flow of particles in space by electromagnetic fields) provide information about the composition and distribution of the neutral lunar exosphere. We have constructed a model of 18 neutral and 20 ionized species in the lunar exosphere based on previous observations and/or models. The model predicts that the dominant pickup ion species in the lunar exosphere include carbon monoxide (CO+), 40‐argon (40Ar+), aluminum (Al+), sodium (Na+), and potassium (K+). The model is compared to observations of lunar pickup ions by NASA's ARTEMIS mission. We find that the model is missing a component of the pickup ion flux and suggest that the Moon may harbor a dense carbon dioxide (CO2) exosphere. Key Points: We constructed an observationally based model of 18 neutral and 20 ionized species from the lunar exosphereDominant pickup ion species are H2+ ${\mathrm{H}}_{2}^{+}$, He+, CO+, 40Ar+, Al+, Na+, K+, Si+, Ca+, and O+ with asymmetric spatial distributionThe model underestimates pickup ion fluxes when compared to ARTEMIS observations, and we suggest CO2+ ${\mathrm{C}\mathrm{O}}_{2}^{+}$ as the missing component [ABSTRACT FROM AUTHOR]

Background: Long-term mental health outcomes were characterized in patients who were diagnosed with Hodgkin lymphoma (HL), and risk factors for the development of mental health disorders were identified.Methods: Patients who were diagnosed with HL between 1997 and 2014 were identified in the Utah Cancer Registry. Each patient was matched with up to five individuals from a general population cohort identified within the Utah Population Database, a unique source of linked records that includes patient and demographic data.Results: In total, 795 patients who had HL were matched with 3575 individuals from the general population. Compared with the general population, patients who had HL had a higher risk of any mental health diagnosis (hazard ratio, 1.77; 95% confidence interval, 1.57-2.00). Patients with HL had higher risks of anxiety, depression, substance-related disorders, and suicide and intentional self-inflicted injuries compared with the general population. The main risk factor associated with an increased risk of being diagnosed with mental health disorders was undergoing hematopoietic stem cell transplantation, with a hazard ratio of 2.06 (95% confidence interval, 1.53-2.76). The diagnosis of any mental health disorder among patients with HL was associated with a detrimental impact on overall survival; the 10-year overall survival rate was 70% in patients who had a mental health diagnosis compared with 86% in those patients without a mental health diagnosis (p < .0001).Conclusions: Patients who had HL had an increased risk of various mental health disorders compared with a matched general population. The current data illustrate the importance of attention to mental health in HL survivorship, particularly for patients who undergo therapy with hematopoietic stem cell transplantation. [ABSTRACT FROM AUTHOR]

Informal caregivers, mainly family members and friends, provide supportive and palliative care for people with amyotrophic lateral sclerosis (ALS) during their terminal disease course. Informal caregiving for people with ALS continues towards palliative care and end‐of‐life care with the progression of the disease. In this study, we provide a theoretical understanding of informal caregiving in ALS utilising 23 semi‐structured interviews conducted with informal caregivers of people with ALS (pwALS) in Switzerland. Due to the expected death of the care recipient, our grounded theory approach outlines informal caregivers' caregiving work as an effort to secure a balance amongst different caregiving activities, which feed into the final stage of providing palliative care. Overall, our theoretical understanding of ALS informal caregiving work encompasses the core category 'holding the balance' and four secondary categories: 'Organising support', 'being present', 'managing everyday life' and 'keeping up with ALS'. The core category of holding the balance underlines the significance of ensuring care and normalcy even as disease progresses and until the end of life. For the informal caregivers, this balancing act is the key element of care provision to pwALS and therefore guides decisions surrounding caregiving. On this understanding, those caregivers that succeed in holding the balance can provide care at home until death. The balance is heavily influenced by contextual factors of caregiving, for example relating to personal characteristics of the caregiver, or activities of caregiving where the goal is to ensure the quality of life of the pwALS. As there is a heterogeneity of speed and subtype of progression of ALS, our work accounts for multiple caregiving trajectories. [ABSTRACT FROM AUTHOR]

Purpose: Monte Carlo (MC) simulation studies, aimed at evaluating the magnitude of tissue heterogeneity in 125I prostate permanent seed implant brachytherapy (BT), customarily use clinical post‐implant CT images to generate a virtual representation of a realistic patient model (virtual patient model). Metallic artifact reduction (MAR) techniques and tissue assignment schemes (TAS) are implemented on the post‐implant CT images to mollify metallic artifacts due to BT seeds and to assign tissue types to the voxels corresponding to the bright seed spots and streaking artifacts, respectively. The objective of this study is to assess the combined influence of MAR and TAS on MC absorbed dose calculations in post‐implant CT‐based phantoms. The virtual patient models used for 125I prostate implant MC absorbed dose calculations in this study are derived from the CT images of an external radiotherapy prostate patient without BT seeds and prostatic calcifications, thus averting the need to implement MAR and TAS. Methods: The geometry of the IsoSeed I25.S17plus source is validated by comparing the MC calculated results of the TG‐43 parameters for the line source approximation with the TG‐43U1S2 consensus data. Four MC absorbed dose calculations are performed in two virtual patient models using the egs_brachy MC code: (1) TG‐43‐based Dw,w‐TG43, (2) Dw,w‐MBDC that accounts for interseed scattering and attenuation (ISA), (3) Dm,m that examines ISA and tissue heterogeneity by scoring absorbed dose in tissue, and (4) Dw,m that unlike Dm,m scores absorbed dose in water. The MC absorbed doses (1) and (2) are simulated in a TG‐43 patient phantom derived by assigning the densities of every voxel to 1.00 g cm−3 (water), whereas MC absorbed doses (3) and (4) are scored in the TG‐186 patient phantom generated by mapping the mass density of each voxel to tissue according to a CT calibration curve. The MC absorbed doses calculated in this study are compared with VariSeed v8.0 calculated absorbed doses. To evaluate the dosimetric effect of MAR and TAS, the MC absorbed doses of this work (independent of MAR and TAS) are compared to the MC absorbed doses of different 125I source models from previous studies that were calculated with different MC codes using post‐implant CT‐based phantoms generated by implementing MAR and TAS on post‐implant CT images. Results: The very good agreement of TG‐43 parameters of this study and the published consensus data within 3% validates the geometry of the IsoSeed I25.S17plus source. For the clinical studies, the TG‐43‐based calculations show a D90 overestimation of more than 4% compared to the more realistic MC methods due to ISA and tissue composition. The results of this work generally show few discrepancies with the post‐implant CT‐based dosimetry studies with respect to the D90 absorbed dose metric parameter. These discrepancies are mainly Type B uncertainties due to the different 125I source models and MC codes. Conclusions: The implementation of MAR and TAS on post‐implant CT images have no dosimetric effect on the 125I prostate MC absorbed dose calculation in post‐implant CT‐based phantoms. [ABSTRACT FROM AUTHOR]

Background: Permanent pacemaker (PPM) and implantable cardioverter defibrillator (ICD) implant rates have increased in New Zealand over the past decade. Aims: To provide a contemporary analysis of regional variation in implant rates. Methods: New PPM and ICD implants in patients aged ≥15 years were identified for 10 years (2009–2018) using procedure coding in the National Minimum Datasets, which collects all New Zealand public hospital admissions. Age‐standardised new implant rates per million adult population were calculated for each of the four regions (Northern, Midland, Central and Southern) and the 20 district health boards (DHB) across those regions. Trend analysis was performed using joinpoint regression. Results: New PPM implant rates increased nationally by 3.4%/year (P < 0.001). The Northern region had the highest new PPM implant rate, increasing by 4.5%/year (P < 0.001). Excluding DHB with <50 000 people, the new PPM implant rate for 2017/2018 was highest in Counties Manukau DHB (854.3/million; 95% confidence interval (CI): 774.9–933.6/million) and lowest in Canterbury DHB (488.6/million; 95% CI: 438.1–539.0/million). New ICD implant rates increased nationally by 3.0%/year (P = 0.002). The Midland region had the highest new ICD implant rate, increasing by 3.8%/year (P = 0.013). Excluding DHB with <50 000 people, the new ICD implant rate for 2017−2018 was highest in the Bay of Plenty DHB (228.5/million; 95% CI: 180.4–276.6/million) and lowest in Canterbury DHB (90.2/million; 95% CI: 69.9–110.4/million). Conclusion: There was significant variation in PPM and ICD implant rates across regions and DHB, suggesting potential inequity in patient access across New Zealand. [ABSTRACT FROM AUTHOR]

However, the systematic measurement of IGF-1 might not be the most optimal cost-benefit approach to detect AM and, therefore, novel techniques to detect AM are urgently needed. Since these clinical features are the fundamental ones of AM patients, physicians taking care of OSAS patients should be trained to recognize acral enlargement features. Features at diagnosis of 324 patients with acromegaly did not change from 1981 to 2006: acromegaly remains under-recognized and under- diagnosed. Keywords: acromegaly; diabetes mellitus type 2; hypertension; obstructive sleep apnea; pituitary; sleep disordered breathing EN acromegaly diabetes mellitus type 2 hypertension obstructive sleep apnea pituitary sleep disordered breathing 918 921 4 05/05/22 20220601 NES 220601 To the Editor Acromegaly (AM) is an endocrine disorder in which the tongue is enlarged and, therefore, is a risk factor for obstructive sleep apnoea syndrome (OSAS).1 OSAS is detected in 26 to 70% of AM patients and results mainly from pharyngeal soft tissue swelling and maxillo-mandibular bones overgrowth.2 However, data on the prevalence of AM in patients with OSAS remain scarce, reporting prevalence's between 0.14% and 0.35%,3-5 significantly higher than those in the general population (0.003%-0.014%).6 Guidelines on OSAS management do not propose systematic screening for the presence of AM.7 The aim of our study was to investigate the prevalence of AM in patients with moderate-to-severe OSAS and to compare our findings to the prevalence of AM in the general population. [Extracted from the article]

Liquid state self‐assembly is important for the understanding of the complex structures developed in abiogenesis and biogenesis as well as for numerous potential technological applications. Herein we report the first body‐centered cubic liquid crystalline phase with 8‐connected network topology and open octahedral network structure. It is formed by dynamic soft self‐assembly of X‐shaped polyphiles with oligo(para‐phenylene‐ethynylene) cores. The π‐conjugated rods with perfluorinated inner benzene rings form networks conjoined by eight‐way junctions, which are formed by nano‐segregated spheres involving hydrogen‐bonded polar end groups, while the branched aliphatic chains at opposite sides of the cores fill the continuum. This novel cubic phase is based on the I‐WP minimal surface separating the frameworks of polyaromatic cores from the most disordered chain segments. It can also be considered as a dense sphere packing. Such liquid organic frameworks, representing hybrids of sphere packings and networks could be of interest for organic photonics and other technologies. [ABSTRACT FROM AUTHOR]

A series of bent‐shaped 4‐cyanoresorcinol bisterephthalates is reported. Some of these achiral compounds spontaneously form a short‐pitch heliconical lamellar liquid‐crystalline phase with incommensurate 3‐layer pitch and the helix axis parallel to the layer normal. It is observed at the paraelectric‐(anti)ferroelectric transition, if it coincides with the transition from random to uniform tilt and with the transition from anticlinic to synclinic tilt correlation of the molecules in the layers of the developing tilted smectic phase. For compounds with long chains the heliconical phase is only field‐induced, but once formed it is stable in a distinct temperature range, even after switching off the field. The presence of the helix changes the phase properties and the switching mechanism from the naturally preferred rotation around the molecular long axis, which reverses the chirality, to a precession on a cone, which retains the chirality. These observations are explained by diastereomeric relations between two coexisting modes of superstructural chirality. One is the layer chirality, resulting from the combination of tilt and polar order, and the other one is the helical twist evolving between the layers. At lower temperature the helical structure is replaced by a non‐tilted and ferreoelectric switching lamellar phase, providing an alternative non‐chiral way for the transition from anticlinic to synclinic tilt. [ABSTRACT FROM AUTHOR]

Water‐group gas continuously escapes from Jupiter's icy moons to form co‐orbiting populations of particles or neutral toroidal clouds. These clouds provide insights into their source moons as they reveal loss processes and compositions of their parent bodies, alter local plasma composition, and act as sources and sinks for magnetospheric particles. We report the first observations of H2+ pickup ions in Jupiter's magnetosphere from 13 to 18 Jovian radii and find a density ratio of H2+/H+ = 8 ± 4%, confirming the presence of a neutral H2 toroidal cloud. Pickup ion densities monotonically decrease radially beyond 13 RJ consistent with an advecting Europa‐genic toroidal cloud source. From these observations, we derive a total H2 neutral loss rate from Europa of 1.2 ± 0.7 kg s−1. This provides the most direct estimate of Europa's H2 neutral loss rate to date and underscores the importance of both ion composition and neutral toroidal clouds in understanding satellite‐magnetosphere interactions. Plain Language Summary: Jupiter's moons Europa, Ganymede, and Callisto all have icy surfaces which interact with their local environments. From this interaction, water‐group atoms and molecules are released from the icy surfaces and orbit Jupiter as a collection of material in "neutral toroidal clouds." The material in these toroidal clouds interact with the local charged particle environment, where neutrals in the toroidal clouds can become charged and incorporated into Jupiter's charged particle environment. Here, we highlight observations of Jupiter's charged particle environment and present the first detections of H2+ in this environment. These H2+ ions are shown to be originally produced from H2 lost from Europa and the abundance of detected ions allows us to determine Europa is losing 1.2 ± 0.7 kg s−1 of neutral H2. This provides the most direct estimate of Europa's H2 neutral loss rate to date and underscores the importance of both ion composition and neutral toroidal clouds in understanding how satellites interact with their local charged particle environments. Key Points: First identification of H2+ in the Jovian magnetosphere from 13 to 18 RJ, with a density ratio of H2+/H+ = 8 ± 4%H2+ in Jupiter's magnetosphere is predominantly produced by Europa's neutral toroidal cloudEuropa's total H2 neutral loss rate is 1.2 ± 0.7 kg s−1 [ABSTRACT FROM AUTHOR]

The collisional grinding of interplanetary meteoroids should continually produce grains over a wide range of sizes, including down to the nanometer‐size regime. Once generated, nanodust grains are subject to interplanetary electromagnetic forces from the solar wind due to their relatively large charge‐to‐mass ratios, resulting in complex and highly time‐dependent dynamics. Here, we use the coupled Wang‐Sheeley‐Arge solar corona and Enlil solar wind models together with a nanodust charging and dynamics model to explore the behavior and variability of nanodust dynamics in the inner heliosphere (<1 au) both within and across multiple solar cycles. In particular, we quantify the relative accessibility of these grains to 1 au across solar cycles 23 and 24, including focusing and defocusing heliospheric conditions. Finally, we qualitatively compare our model results with STEREO A (STA)/WAVES observations and identify correlations between the STA/WAVES single‐hit rate and the relative flux of >10 nm grains. Using solar cycle 23 as a proxy for the behavior of solar cycle 25, since both solar cycles share the same defocusing‐to‐focusing transition, we predict the relative flux of nanodust grains in the future and identify times at which nanodust impacts may reappear in the STA/WAVES data set. Continued analysis of future STA/WAVES observations will provide an important test of this prediction, either bolstering or weakening the interpretation of electromagnetically accelerated nanodust grains as the source of single‐hit events in the STA/WAVES Time Domain Sampler data set. Key Points: Inner heliospheric nanodust dynamics are modeled over a broad range of solar cycles and IMF polarityCessation of single‐hit impacts on STA/WAVES is correlated with model predictions of declining nanodust fluxes at 1 auWe predict single‐hit impacts due to nanodust impacts should gradually reappear in STA/WAVES between 2022 and 2028 [ABSTRACT FROM AUTHOR]

Climate change will affect the distribution of many tropical plant species. However, the understanding of how dioecious tropical species cope with different environmental conditions is still limited. To address this issue, we investigated how secondary trait attributes in populations of the dioecious tropical tree Myrsine coriacea change along an altitudinal gradient. Eighty individual plants (40 male and 40 female) were selected among seven natural populations. Leaf variation in morphological and stomatal traits, and carbon and nitrogen isotopic compositions were analyzed. Female plants had greater isotopic leaf carbon composition (δ13C) and nitrogen content than male plants, increasing their carboxylation capacity. Plants of both sexes had smaller stomata, greater water‐use efficiency (greater δ13C), and greater nitrogen isotopic composition (δ15N) at higher altitudes. They also showed lower δ15N and had greater carbon: nitrogen ratios at lower altitudes. There was a lack of coordination between stomatal and vein traits, which was compensated for by variation in specific leaf areas. This mechanism was essential for increasing plant performance under the limiting conditions found by the species at higher altitudes. [ABSTRACT FROM AUTHOR]