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This letter uses simultaneous observations from Magnetosphere Multiscale (MMS) and Time History of Events and Macroscale Interactions during Substorms (THEMIS) to address the dynamics of the magnetopause and magnetosheath boundary layers during the main phase of a storm during which the interplanetary magnetic field (IMF) reverses from south to north. Near the dawn terminator, MMS observes two boundary layers comprising open and closed field lines and containing energetic electrons and ring current oxygen. Some closed field line regions exhibit sunward convection, presenting an avenue to replenish dayside magnetic flux lost during the storm. Meanwhile, THEMIS observes two boundary layers in the pre‐noon sector which strongly resemble those observed at the flank by MMS. Observations from the three THEMIS spacecraft indicate the boundary layers are still evolving several hours after the IMF has turned northward. These observations advance our knowledge of the dynamic magnetopause and magnetosheath boundary layers under the combined effects of an ongoing storm and changing IMF. Plain Language Summary Earth's magnetic field, the magnetosphere, acts as a shield protecting the near Earth environment from the solar wind. During active times, this shield can be damaged and reduced in size, but during quieter times, the shield can expand and repair itself. This letter uses observations from multiple spacecraft to better understand how the edges of our magnetosphere change during the transition from active to more quiet times. We observe the development of boundary layers at the dayside and flanks of the magnetosphere. Convection in and around these layers can contribute to the growth of the magnetosphere after it has been eroded during active times. These observations also place limits on the size of the boundary layers and how quickly they may develop. Key Points Direct evidence of sunward transport of closed magnetic flux is observed by Magnetosphere Multiscale (MMS) at the dawn flank terminator MMS and Time History of Events and Macroscale Interactions during Substorms (THEMIS) observe nearly identical boundary layers at the dawn flank and pre‐noon sectors Boundary layers and sunward convecting flux tubes are populated with energetic electrons and ring current oxygen ions

Psychiatric and neurological disorders are influenced by an undetermined number of genes and molecular pathways that may differ among afflicted individuals. Functionally testing and characterizing biological systems is essential to discovering the interrelationship among candidate genes and understanding the neurobiology of behavior. Recent advancements in genetic, genomic, and behavioral approaches are revolutionizing modern neuroscience. Although these tools are often used separately for independent experiments, combining these areas of research will provide a viable avenue for multidimensional studies on the brain. Herein we will briefly review some of the available tools that have been developed for characterizing novel cellular and animal models of human disease. A major challenge will be openly sharing resources and datasets to effectively integrate seemingly disparate types of information and how these systems impact human disorders. However, as these emerging technologies continue to be developed and adopted by the scientific community, they will bring about unprecedented opportunities in our understanding of molecular neuroscience and behavior.

From 10 to 12 May 2024, a series of coronal mass ejections led to one of the strongest geomagnetic storms of the century, referred to as the Mother's Day or Gannon Storm. MMS's position on the dayside magnetosphere on 11 May provided observations of a strongly driven and compressed ∼7RE $\\left(\\sim 7\\ {R}_{E}\\right)$ reconnecting magnetopause. Because of the driving conditions, the magnetopause became saturated with O+ ${O}^{+}$ outflows that dominated the mass density of the plasma environment. In the reconnecting magnetopause, MMS observes signatures of parallel electron heating on the magnetopause's magnetosheath side, but anomalous and significant electron cooling, especially from the perpendicular electron temperature on the magnetosphere side, possibly driven by additional mechanisms besides reconnection. Even with the strong driving and O+ ${O}^{+}$ outflows, we find an expected (0.19±0.04) $(0.19\\pm 0.04)$ normalized reconnection rate for the primary exhaust, indicating insensitivity to these conditions. The unnormalized rate, however, is atypically large and scales with the driving conditions.

Magnetopause boundary layers (BLs) play an important role mediating plasma and energy exchange between the solar wind/magnetosheath and Earth's magnetosphere. Energy exchange across the magnetopause is enhanced during storms, yet little work has been done investigating BLs during storms. In this letter, using MMS and THEMIS observations, we investigate the structure and formation of magnetopause BLs during a large coronal mass ejection (CME) driven storm containing 20 hours of low Alfvén Mach number solar wind (MA<3${< } 3$ ). Separated by ∼9${\\sim} 9$Earth radii (RE${\\mathrm{R}}_{E}$ ), MMS and THEMIS observe a low latitude boundary layer (LLBL), magnetosheath boundary layer (MSBL), and formation of a plasma depletion layer after a northward interplanetary magnetic field turning. MMS observations indicate lobe reconnection drives the MSBL and LLBL formation. Observations of CME ions on closed field lines demonstrate dual reconnection can trap solar wind plasma under sub‐Alfvenic solar wind conditions and constrain the trapped populations' dwell time.

The detailed mechanisms coupling the solar wind to Earth's magnetosphere are not yet fully understood. Solar wind plasma is heated non-adiabatically as it penetrates the magnetosphere, and this process must span scale sizes. Reconnection alone is not able to account for the observed heating; other mechanisms must be at work. One potential process is the Kelvin-Helmholtz instability (KHI). The KHI is a convective instability which operates at the fluid scale in plasmas, but is capable of driving secondary process at smaller scales. Previous work has shown evidence of magnetic reconnection, various ion scale wave modes, mode conversion, and turbulence associated with the KHI, all of which can contribute to heating and/or plasma transport across the magnetopause boundary. The launch of the Magnetosphere Multiscale (MMS) mission in 2015 offered a new opportunity to study secondary processes associated with the KHI down to the electron scale. The MMS mission's goal was to study the microphysics of magnetic reconnection at the dayside magnetopause and in the magnetotail. It comprises 4 identical spacecraft, which fly in formation and are equipped with the highest resolution instrumentation available. MMS is the first mission capable of resolving electron scale processes due to its combination of high temporal resolution instrumentation and its record breaking spacecraft separation. The work presented in this dissertation focuses on the fluid and ion scale behavior of the KHI as a proof of concept for the techniques used. Future work will apply these methods to smaller scales to fully take advantage of MMS's capabilities.This work uses MMS observations of 45 KHI events between September 2015 and March 2020 to determine the influence of the KHI on magnetosphere dynamics and solar wind-magnetosphere coupling. The observed events are well distributed along the magnetopause, and occur for the full range of solar wind conditions and IMF orientations. The KHI growth rates and the percent of the solid angle unstable to the development of the KHI (which we term the unstable solid angle) are not effected by the solar wind conditions or IMF strength. The observed KHI grow more quickly and in more unstable regions the farther downtail they occur.Ion scale wave intervals observed within the KHI are consistent with the ion cyclotron, kinetic Alfvén, and kinetic magnetosonic wave modes, all of which can contribute to enhanced ion heating across the magnetopause. These ion scale wave intervals are compared with observations made when the KHI is not active. The KHI is associated with strong increases in quasi-perpendicular (quasi-parallel) ion scale wave activity in the magnetosphere (magnetosheath), consistent with previous studies of data from the Cluster spacecraft. Observations show electron beta is decreased and ion temperature anisotropy is increased in the magnetosheath when the KHI is present, which can help explain a KHI associated increase in quasi-parallel wave activity in the sheath. Additionally, parallel velocity shears are increased when the KHI is active, which may further drive wave activity in all regions. Ion scale wave intervals show enhanced Poynting flux in all regions and at all wave angles when the KHI is active, suggesting more energy is available to drive ion heating during the KHI. Increased Poynting flux is also well correlated with larger changes in energy during KH associated ion scale waves. The rate of heating, described by the characteristic heating frequency, also increases for ion scale waves associated with the KHI. These findings suggest that plasma heating is both increased and more efficient in the presence of the KHI.

We present a comprehensive study of Magnetospheric Multiscale (MMS) spacecraft encounter with KHI during a geomagnetic storm, focusing on elucidating key turbulence properties and reconnection signatures observed at the edges of KH vortices. The spectral slope for electric field stays approximately constant for frequencies below the ion cyclotron frequency and exhibits a break around the lower hybrid frequency, indicating wave activity. Furthermore, MMS observes a current sheet accompanied by intense electron jets and features consistent with strong guide-field asymmetric reconnection across the magnetopause. Substantial agyrotropy (by a factor of 10) in electron distribution functions is observed in the reconnecting current sheet and at the edges of KH. Our observation presents a multi-scale view into KH turbulence under strongly driven conditions and into the dynamics occurring at electron dissipation scales.

We report Magnetospheric Multiscale observations of oxygen ions (O+) during a coronal mass ejection in April 2023 when the solar wind was sub-Alfvénic and Alfvén wings formed. For the first time, O+ characteristics are studied at the contact region between the unshocked solar wind and the magnetosphere. The O+ ions show energies between 100s eV and ~30 keV. The possible sources are the ring current, the warm plasma cloak, and the ionosphere. The O+ ions exhibit bi-directional streaming along newly-formed closed field lines (CFLs), and dominantly anti-parallel on earlier-formed CFLs. Escaping O+ ions in the unshocked solar wind are observed. During the recovery phase, the O+ pitch-angle distribution associated with flux tubes shows dispersion, indicating potential loss to the solar wind. Our results show escaping as well as trapped O+ ions in the region where a magnetic cloud, an Alfvén wing, and magnetospheric field lines are mixed.

On April 24th, 2023, a CME event caused the solar wind to become sub-Alfvenic, leading to the development of an Alfven Wing configuration in the Earth's Magnetosphere. Alfven Wings have previously been observed as cavities of low flow in Jupiter's magnetosphere, but the observing satellites did not have the ability to directly measure the Alfven Wings' current structures. Through in situ measurements made by the Magnetospheric Multiscale (MMS) spacecraft, the April 24th event provides us with the first direct measurements of current structures during an Alfven Wing configuration. We have found two distinct types of current structures associated with the Alfven Wing transformation as well as the magnetosphere recovery. These structures are observed to be significantly more anti-field-aligned and electron-driven than typical magnetopause currents, indicating the disruptions caused to the magnetosphere current system by the Alfven Wing formation.

The twenty-first century has witnessed a wave of severe infectious disease outbreaks, not least the COVID-19 pandemic, which has had a devastating impact on lives and livelihoods around the globe. The 2003 severe acute respiratory syndrome coronavirus outbreak, the 2009 swine flu pandemic, the 2012 Middle East respiratory syndrome coronavirus outbreak, the 2013–2016 Ebola virus disease epidemic in West Africa and the 2015 Zika virus disease epidemic all resulted in substantial morbidity and mortality while spreading across borders to infect people in multiple countries. At the same time, the past few decades have ushered in an unprecedented era of technological, demographic and climatic change: airline flights have doubled since 2000, since 2007 more people live in urban areas than rural areas, population numbers continue to climb and climate change presents an escalating threat to society. In this Review, we consider the extent to which these recent global changes have increased the risk of infectious disease outbreaks, even as improved sanitation and access to health care have resulted in considerable progress worldwide.Global change, including climate change, urbanization and global travel and trade, has affected the emergence and spread of infectious diseases. In the Review, Baker, Metcalf and colleagues examine how global change affects infectious diseases, highlighting examples ranging from COVID-19 to Zika virus disease.

We report a systematic review and meta-analysis of research using animal models of chemotherapy-induced peripheral neuropathy (CIPN). We systematically searched 5 online databases in September 2012 and updated the search in November 2015 using machine learning and text mining to reduce the screening for inclusion workload and improve accuracy. For each comparison, we calculated a standardised mean difference (SMD) effect size, and then combined effects in a random-effects meta-analysis. We assessed the impact of study design factors and reporting of measures to reduce risks of bias. We present power analyses for the most frequently reported behavioural tests; 337 publications were included. Most studies (84%) used male animals only. The most frequently reported outcome measure was evoked limb withdrawal in response to mechanical monofilaments. There was modest reporting of measures to reduce risks of bias. The number of animals required to obtain 80% power with a significance level of 0.05 varied substantially across behavioural tests. In this comprehensive summary of the use of animal models of CIPN, we have identified areas in which the value of preclinical CIPN studies might be increased. Using both sexes of animals in the modelling of CIPN, ensuring that outcome measures align with those most relevant in the clinic, and the animal's pain contextualised ethology will likely improve external validity. Measures to reduce risk of bias should be employed to increase the internal validity of studies. Different outcome measures have different statistical power, and this can refine our approaches in the modelling of CIPN.