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This article discusses a study that validates the MAGNetosphere-Ionosphere-Thermosphere (MAGNIT) model against AMPERE measurements of field-aligned currents (FACs) during the "Galaxy 15" space weather event. The study compares the performance of three ionosphere electrodynamic models and finds that MAGNIT exhibits slightly improved predictions compared to other models. The article provides valuable information on auroral precipitation sources and their impact on FACs, which can be used to enhance the model. The study also analyzes various metrics and provides recommendations for optimizing the model's performance. [Extracted from the article]

In order to help inform efforts to fulfill the National Science Foundation (NSF) Geospace Environment Modeling (GEM) community's ethical goal toward pursuing diversity, equity, inclusion, and justice (DEIJ) the authors administered the 2023 GEM Climate Survey to attendees of the 2023 GEM Workshop. Its main goals were to 1) obtain organized demographic information about the GEM community, and 2) to provide a quantitative assessment of the GEM community's perceptions of its own culture primarily with respect to inclusion and belonging. Responses indicate the GEM community is comparable or slightly more diverse than heliophysics as a whole and the American Geophysical Union (AGU) general membership, but still not close to reflecting the population of the United States or the world. The average responses to survey items about feelings of belonging in the GEM community indicate that members feel they belong in the GEM community, that the GEM community climate is broadly inclusive, and that efforts to support that cultural climate are improving over time. This is true across the entire population regardless of career stage, as well as for female respondents; Lesbian, Gay, Bisexual, Transgender, Queer/Questioning, Pansexual, Asexual (LGBTQPA+) respondents; Asian/Asian Subcontinent respondents; and non-Asian respondents of color. Division of the dataset into subgroups also indicates work to build a fully inclusive community is not complete, particularly with respect to workplace hostility these groups witness. This report recommends continuing work to capture the time history of demographics and trends in the community culture in response to inclusion efforts and initiatives. [ABSTRACT FROM AUTHOR]

We analyze the local dynamics of magnetotail reconnection onset using Magnetospheric Multiscale (MMS) data. In conjunction with MMS, the macroscopic dynamics of this event were captured by a number of other ground and space‐based observatories, as is reported in a companion paper. We find that the local dynamics of the onset were characterized by the rapid thinning of the cross‐tail current sheet below the ion inertial scale, accompanied by the growth of flapping waves and the subsequent onset of electron tearing. Multiple kinetic‐scale magnetic islands were detected coincident with the growth of an initially sub‐Alfvénic, demagnetized tailward ion exhaust. The onset and rapid enhancement of parallel electron inflow at the exhaust boundary was a remote signature of the intensification of reconnection Earthward of the spacecraft. Two secondary reconnection sites are found embedded within the exhaust from a primary X‐line. The primary X‐line was designated as such on the basis that (a) while multiple jet reversals were observed in the current sheet, only one reversal of the electron inflow was observed at the high‐latitude exhaust boundary, (b) the reconnection electric field was roughly five times larger at the primary X‐line than the secondary X‐lines, and (c) energetic electron fluxes increased and transitioned from anti‐field‐aligned to isotropic during the primary X‐line crossing, indicating a change in magnetic topology. The results are consistent with the idea that a primary X‐line mediates the reconnection of lobe magnetic field lines and accelerates electrons more efficiently than its secondary X‐line counterparts. Key Points: Magnetotail reconnection onset was triggered by electron tearing during a solar wind pressure pulseOnset was characterized by the rapid collapse of the current sheet thickness and kinetic‐scale flux rope formationA primary X‐line was established within minutes of the onset [ABSTRACT FROM AUTHOR]

The Whole Heliosphere and Planetary Interactions initiative was established to leverage relatively quiet intervals during solar minimum to better understand the interconnectedness of the various domains in the heliosphere. This study provides an expansive mosaic of observations spanning from the Sun, through interplanetary space, to the magnetospheric response and subsequent effects on the ionosphere‐thermosphere‐mesosphere (ITM) system. To accomplish this, a diverse set of observational datasets are utilized from 2019 July 26 to October 16 (i.e., over three Carrington rotations, CR2220, CR2221, and CR2222) with connections of these observations to the more focused studies submitted to this special issue. Particularly, this study focuses on two long‐lived coronal holes and their varying impact in sculpting the heliosphere and driving of the magnetospheric system. As a result, the evolution of coronal holes, impacts on the inner heliosphere solar wind, glimpses at mesoscale solar wind variability, magnetospheric response to these evolving solar wind drivers, and resulting ITM phenomena are captured to reveal the interconnectedness of this system‐of‐systems. Plain Language Summary: The field of Heliophysics research spans a large range of plasma regimes and disciplines that are all linked through the complex interactions each system has with one another. To better explore the interconnected nature of the heliosphere, this study combines observations from across the sub‐domains of Heliophysics to construct snapshots of the Sun, solar wind, and the magnetospheric and ionospheric systems at Earth over three revolutions of the Sun. This allows for a unique vantage point to put these systems in perspective of one another and understand how they impact one another. Key Points: The evolution and impacts of two coronal holes are investigated over three Carrington rotationsThe evolution of the coronal hole led to changes in the solar wind throughout the inner solar systemSubsequent geospace response differed with each passage due to both changes in the solar wind and preconditioning within the systems [ABSTRACT FROM AUTHOR]

Using a three-dimensional (3-D) global-scale hybrid code, the Magnetospheric Multiscale (MMS) reconnection event around 02:13 UT on 18 November 2015, highlighted in the Geospace Environment Modeling (GEM) Dayside Kinetic Challenge, is simulated, in which the interplanetary magnetic field (IMF) points southward and the geomagnetic field has a -27° dipole tilt angle. Strong southward plasma jets are found near the magnetopause as a result of the dayside reconnection. Our results indicate that the subsolar magnetopause reconnection X line shifts from the subsolar point toward the Northern Hemisphere due to the effect of the tilted geomagnetic dipole angle, consistent with the MMS observation. Subsequently, the reconnection X lines or sites and reconnection flux ropes above the equator propagate northward along the magnetopause. The formation and global distribution of the X lines and the structure of the magnetopause reconnection are investigated in detail with the simulation. Mirror mode waves are also found in the middle of the magnetosheath downstream of the quasi-perpendicular shock where the plasma properties are consistent with the mirror instability condition. As a special outcome of the GEM challenge event, the spatial and temporal variations in reconnection, the electromagnetic power spectra, and the associated D-shaped ion velocity distributions in the simulated reconnection event are compared with the MMS observation. [ABSTRACT FROM AUTHOR]

Introduction: NASA designated Reiner Gamma as the destination for the first Payloads and Research Investigations on the Surface of the Moon (PRISM) delivery (known as PRISM-1a). Reiner Gamma (RG) is home to a magnetic anomaly, a region of magnetized crustal rocks. The RG magnetic anomaly, on the western nearside, is co-located with the type example of a class of unusual high-reflectance markings known as lunar swirls. PRISM payloads will be carried on commercial landers as part of NASA's Commercial Lunar Payload Services (CLPS) program. The RG lander and PRISM-1a payload are designed for operation during one lunar daylight period. NASA selected APL's Lunar Vertex proposal for the PRISM-1a mission in June of 2021. APL is providing overall management of Lunar Vertex, systems engineering, safety and mission assurance, two magnetometer instruments, and rover integration and testing. The Lunar Vertex Science Operations Center will be at APL. Lunar Vertex Goals: A lunar magnetic anomaly is a natural laboratory for addressing a wide range of questions in planetary science [e.g., 1, 2]. Lunar Vertex has the following goals: 1) Investigate the origin of lunar magnetic anomalies; 2) Investigate the origin of lunar swirls; 3) Determine the structure of the mini-magnetosphere that forms over the RG magnetic anomaly. These goals are traceable to the Planetary Decadal Survey [3] and other community guiding documents [4-7]. The mission goals will be accomplished by payload elements on the CLPS lander and on a Lunar Vertex rover. Lander Instruments: The lander suite includes three elements. The Vertex Camera Array (VCA) is a set of fixedmounted cameras. VCA images will be used to (a) survey landing site geology, and (b) perform photometric modeling of regolith characteristics. VCA is being built by Redwire Aerospace of Littleton, Co., USA. The Vector Magnetometer-Lander (VML) is a suite of fluxgate magnetometers. VML will operate during cruise and descent and on the surface to measure the in-situ magnetic field at multiple altitudes and through varying upstream conditions. Built by APL, VML has a dual ring-core fluxgate sensor mounted at the end of a mast. VML also has four commercial miniature magnetometers arrayed in a tetrahedron near the base of the mast. Gradiometry allows for separation of the natural field from that of the lander. The Magnetic Anomaly Plasma Spectrometer (MAPS) measures the energy, flux, and direction of ions and electrons that reach the surface. MAPS is provided by the Southwest Research Institute of San Antonio, Tx., USA. Rover. The CLPS lander will deploy the Lunar Vertex rover, which conducts a traverse reaching =500 m distance, obtaining measurements outside the zone disturbed by the lander rocket exhaust. Measurements of undisturbed regolith are key to testing hypotheses for the origin of swirls. Determination of the magnetic field strength and direction along the traverse will help to constrain the nature of the magnetic source. The rover provider is Lunar Outpost (Golden, Co., USA). Rover Instruments. The rover carries two instruments. The Rover Multispectral Microscope (RMM) will collect images at wavelengths ~0.37-0.94 µm using active LED illumination. RMM (from Canadensys Aerospace of Bolton, On., Canada) will reveal the composition, texture, and particle-size distribution of the regolith beneath the rover. The APL Vector Magnetometer-Rover (VMR) is a copy of a portion of VML: the array of four mini-magnetometers. VMR magnetic measurements will be correlated with changes in regolith properties documented by RMM. Lander Selection. In November 2021, NASA selected Intuitive Machines of Houston, Tx., USA as the provider of the CLPS lander that will deliver Lunar Vertex to the Moon. Launch is planned for April 2024. [ABSTRACT FROM AUTHOR]