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The electron diffusion region (EDR) is a key region for magnetic reconnection, but the typical energy transport and conversion in EDRs is still not well understood. In this work, we perform a statistical study of 80 previously published near X‐line events identified at the dayside magnetopause in Magnetospheric Multiscale data. We find 44 events that clearly present all commonly accepted EDR signatures and use this database to investigate energy flux partition and energy conversion. We find that energy partition is changed inside EDRs, with a 71%–29% allocation of particle energy flux density between electrons and ions respectively. The electron enthalpy flux density is found to dominate locally at all EDRs and is predominantly oriented in the out‐of‐plane direction, perpendicular to the reconnecting magnetic field. We also examine the transition from electron‐ to ion‐dominated energy flux partition further from the EDR, finding this typically occurs at scales of the order of the ion inertial length, larger than the typical EDR size. We then investigate energy conversion and transport and highlight complex processes, with potential non‐steady‐state energy accumulation and release near the EDR. We discuss the implications of our results for reconnection energy conversion, and for magnetopause dynamics in general. Magnetic reconnection is a key plasma phenomenon that occurs in many astrophysical systems, such as in the atmosphere of stars and in the vicinity of magnetized planets like the Earth. It enables rapid conversion of energy as particles gain energy from the magnetic field and are accelerated and heated. In 2015, the 4‐satellite Magnetospheric Multi‐Scale (MMS) mission launched to specifically probe magnetic reconnection close to the Earth. Here we analyze MMS data, first reviewing all previously reported measurements of the very heart of the reconnection region by MMS, and cross‐analyzing them to provide a catalog of 44 confirmed events. We use this catalog to understand how energy is changing during reconnection, finding that energy is mostly deposited to electrons at the heart of the reconnection region. The transport of thermal energy is most important there, and this energy is flowing out of the reconnection region in a direction transverse to the magnetic field. We find that the transfer of energy between field and particles is complex, with temporal effects at play near the reconnection region. These findings bring new insight into the physics of reconnection energetics and have wide implications for wherever reconnection is observed. We provide the first comparative statistical study of all previously reported MMS dayside magnetopause EDRs and confirm 44 clear encountersEnergy flux partition changes at the EDR, it is locally dominated by the electron enthalpy flux oriented in the out‐of‐plane directionWe highlight complex field‐particle energy exchange near the EDR where temporal and non linear effects seem play a role We provide the first comparative statistical study of all previously reported MMS dayside magnetopause EDRs and confirm 44 clear encounters Energy flux partition changes at the EDR, it is locally dominated by the electron enthalpy flux oriented in the out‐of‐plane direction We highlight complex field‐particle energy exchange near the EDR where temporal and non linear effects seem play a role

This study investigates the escape of Mercury's sodium‐group ions (Na+‐group, including ions with m/q from 21 to 30 amu/e) and their dependence on true anomaly angle (TAA), that is, Mercury's orbital phase around the Sun, using measurements from MESSENGER. The measurements are categorized into solar wind, magnetosheath, and magnetosphere, and further divided into four TAA intervals. Na+‐group ions form escape plumes in the solar wind and magnetosheath, with higher fluxes along the solar wind's motional electric field. The total escape rates vary from 0.2 to 1 × 1025atoms/s with the magnetosheath being the main escaping region. These rates exhibit a TAA dependence, peaking near the perihelion and similar during Mercury's remaining orbit. Despite Mercury's tenuous exosphere, Na+‐group ions escape rate is comparable to other inner planets. This can be attributed to several processes, including that Na+‐group ions may include several ion species, efficient photoionization frequency for elements within Na‐group, etc. Atmospheric escape is defined as the loss of atmospheric particles in the form of neutrals and ions into outer space. Understanding atmospheric escape is a fundamental science question for studying the evolution of planetary atmosphere and habitability, as it can provide insight into how life can form on a planet. While atmospheric escape has been extensively studied in Venus, Earth, and Mars through in situ measurements and simulations, it remains poorly understood at Mercury. In this study, we investigate the escape of the most abundant heavy ions at Mercury, specifically the Na+‐group ions, using MESSENGER's measurements. Our findings show that the escape rates of the Na+‐group ions are dependent on Mercury's orbital phase around the Sun, exhibiting a seasonal effect with rates from 0.2 to 1 × 1025atoms/s. This rate is comparable to the ion's escape rates at other inner planets, which is surprising given that Mercury only has a tenuous exosphere. We propose that this can be attributed to several processes such as efficient photoionization, solar wind sputtering, and solar wind momentum exchange at Mercury, and the Na+‐group ions include several ion species such as Na+, aluminum ion (Al+), silicon ion (Si+) and magnesium ion (Mg+) etc. Na+‐group ions form escape plumes in solar wind and magnetosheath, with higher fluxes in the positive solar wind electric field hemisphereThe escape rate ranges from 0.2 to 1 × 1025atoms/s, with the magnetosheath being the main escaping regionEscape rates peak near perihelion, and are similar during other true anomaly angle (TAA) intervals Na+‐group ions form escape plumes in solar wind and magnetosheath, with higher fluxes in the positive solar wind electric field hemisphere The escape rate ranges from 0.2 to 1 × 1025atoms/s, with the magnetosheath being the main escaping region Escape rates peak near perihelion, and are similar during other true anomaly angle (TAA) intervals

Deep learning techniques have been used in various disciplines, ranging from simple data processing to complicated image classification tasks. Deepfakes is a deep learning approach with benefits and drawbacks impacting the world. However, deepfakes are now cutting-edge technology being exploited for nefarious purposes such as the breach of human privacy and identity. Because deep learning is advancing rapidly daily, people use AI to produce deepfakes videos and images. Hence newer AI technology to detect deepfakes is critical. Therefore, the study has proposed detecting video and image deepfakes based on convolutional neural network (CNN) combined with the long short-term memory (LSTM) model, which constructs a deep learning model classifying images and video deepfakes. The proposed model investigated a novel approach to research more powerful models which can be applied to any large dataset. The experimental results demonstrated that the proposed method had achieved promising performance on modified datasets from Celeb-DF with high AUC performance up to 0.7584 and MCC reaching 0.558. Besides, this paper presents brief research on creating and detecting the image and video deepfakes technologies and points out the challenges of using deepfakes in many different contexts.

Space storms1are the dominant contributor to space weather. During storms, rearrangement of the solar wind and Earth’s magnetic field lines at the dayside enhances global plasma circulation in the magnetosphere2,3. As this circulation proceeds, energy is dissipated into heat in the ionosphere and near-Earth space. As Earth’s dayside magnetic flux is eroded during this process, magnetotail reconnection must occur to replenish it. However, whether dissipation is powered by magnetotail (nightside) reconnection, as in storms’ weaker but more commonplace relatives, substorms4,5, or by enhanced global plasma circulation driven by dayside reconnection is unknown. Here we show that magnetotail reconnection near geosynchronous orbit powered an intense storm. Near-Earth reconnection at geocentric distances of ~6.6–10 Earth radii—probably driven by the enhanced solar wind dynamic pressure and southward magnetic field—is observed from multi-satellite data. In this region, magnetic reconnection was expected to be suppressed by Earth’s strong dipole field. Revealing the physical processes that power storms and the solar wind conditions responsible for them opens a new window into our understanding of space storms. It encourages future exploration of the storm-time equatorial near-Earth magnetotail to refine storm driver models and accelerate progress towards space weather prediction.

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. 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 Magnetotail reconnection onset was triggered by electron tearing during a solar wind pressure pulse Onset was characterized by the rapid collapse of the current sheet thickness and kinetic‐scale flux rope formation A primary X‐line was established within minutes of the onset

We analyze a magnetotail reconnection onset event on 3 July 2017 that was observed under otherwise quiescent magnetospheric conditions by a fortuitous conjunction of six space and ground‐based observatories. The study investigates the large‐scale coupling of the solar wind–magnetosphere system that precipitated the onset of the magnetotail reconnection, focusing on the processes that thinned and stretched the cross‐tail current layer in the absence of significant flux loading during a 2‐hr‐long preconditioning phase. It is demonstrated with data in the (a) upstream solar wind, (b) at the low‐latitude magnetopause, (c) in the high‐latitude polar cap, and (d) in the magnetotail that the typical picture of solar wind‐driven current sheet thinning via flux loading does not appear relevant for this particular event. We find that the current sheet thinning was, instead, initiated by a transient solar wind pressure pulse and that the current sheet thinning continued even as the magnetotail and solar wind pressures decreased. We suggest that field line curvature‐induced scattering (observed by magnetospheric multiscale) and precipitation (observed by Defense Meteorological Satellite Program) of high‐energy thermal protons may have evacuated plasma sheet thermal energy, which may require a thinning of the plasma sheet to preserve pressure equilibrium with the solar wind. Magnetotail reconnection onset was observed during a fortuitous multiscale conjunction of the heliophysics observatoriesA transient solar wind pressure pulse triggered thinning and stretching of the cross‐tail current sheet without significant flux loadingA second solar wind pressure pulse caused the thinned current sheet to rapidly collapse and reconnect Magnetotail reconnection onset was observed during a fortuitous multiscale conjunction of the heliophysics observatories A transient solar wind pressure pulse triggered thinning and stretching of the cross‐tail current sheet without significant flux loading A second solar wind pressure pulse caused the thinned current sheet to rapidly collapse and reconnect

While double ion populations, with a cold population originating from the solar wind and a hotter one from the magnetosphere, are frequently observed in the low‐latitude boundary layers at the Earth's magnetopause, similar double electron populations are observed less often. A preliminary study of magnetopause crossings characteristics was used to determine the typical locations and energy spectra of ion and electron populations near the magnetopause. Then, we set up an automated detection algorithm for identifying regions with concomitant double populations in both ion and electron energy spectra. The statistical study was carried out on 7 years of Time History of Events and Macroscale Interactions during Substorms particle data, to determine the interplanetary magnetic field conditions in the upstream solar wind for these double populations. The results suggest that such concomitant ion and electron double population boundary layers form preferentially in the subsolar region and under northward interplanetary magnetic field but with a significant BYcomponent. We interpret this finding as the result of reconnection of the same magnetosheath field line in both hemispheres with at least one end reconnecting in its hemisphere at lower latitude with a closed magnetospheric field line that already contains a hot electron source. Frequent observation of concomitant double electron and ion population in Earth's boundary layersStatistical analyses show that double populations in both ions and electrons occur mainly at dayside during northward IMF with a large ByResult of reconnection between a magnetosheath field line and a magnetospheric field lines already containing hot electrons

We analyzed 20 reconnection events observed by the Magnetosphere MultiScale mission, finding that in a subregion of the magnetospheric inflow, the electron temperature parallel to the magnetic field (Te||) decreases toward the separatrix with increasing densities. Such Te||variation is not consistent with the heating through the parallel potential mechanism for magnetospheric electrons. Associated with the change in Te||, low‐energy gyrotropic magnetosheath‐like electrons are observed. These electrons may come from the magnetosheath, penetrate to the magnetospheric side possibly due to waves in the lower hybrid frequency range, and do not experience as much energization as those from deeper in the magnetosphere. In addition, as Te||decreases, the high‐energy field‐aligned phase‐space densities decrease or fluctuate significantly over time. Wave‐particle interaction might produce energy conversion and cause the high‐energy phase‐space density variations. A sublayer in the magnetospheric inflow with decreasing Te||and increasing density toward the separatrix is shown to be a common featurePenetration of fresh magnetosheath electrons may partially account for the Te||decrease and density increase toward the separatrixHigh‐energy electron phase‐space density variations in magnetosphere inflow are collocated with waves in the lower hybrid frequency range

We investigate the onset of magnetic reconnection, utilizing a fully kinetic Particle‐In‐Cell (PIC) simulation. Characteristic features of the electron phase‐space distributions immediately before reconnection onset are identified. These include signatures of pressure non‐gyrotropy in the velocity distributions, and lemon shaped distributions in the in‐plane velocity directions. Further, we explain how these features form through particle energization by the out‐of‐plane electric field. Identification of these features in the distributions can aid in analysis of data where clear signatures of ongoing reconnection are not yet present. In any environment where magnetic fields and charged particles interact, magnetic reconnection will occur if the conditions are favorable. Magnetic reconnection can be described as magnetic explosions, since it releases stored magnetic energy and converts it into heat and movement of the plasma particles. In this paper, we use numerical simulations to take a closer look at how the reconnection process initiates, a fundamental question still not fully understood. Signatures indicating reconnection onset can be identified in the electron distributionsOnset signatures persist over extended spatial and temporal scalesThe particle distributions immediately preceding onset are characterized by features of non‐gyrotropy and acceleration Signatures indicating reconnection onset can be identified in the electron distributions Onset signatures persist over extended spatial and temporal scales The particle distributions immediately preceding onset are characterized by features of non‐gyrotropy and acceleration

The jump conditions are analyzed in detail for two slow shocks bounding a reconnection plasma jet, observed on 3 August 2008 by the spacecraft THEMIS D (Time History of Events and Macroscale Interactions during Substorms) on the dayside, low‐latitude magnetopause. Both shocks are near the switch‐off limit. They have been previously examined by Sonnerup et al. (2016), on the basis of the simplest MHD version of the jump conditions. In the present paper, those conditions now include the pressure anisotropy, normal heat fluxes, and a finite normal magnetic field component, the effects of all of which are found to be small. We also present and discuss the, mostly field‐aligned, measured total heat fluxes, which are found to be substantial and directed away from the reconnection site. We show that the double‐adiabatic (Chew‐Goldberger‐Low) invariants are far from invariant. Their combination indicates a large entropy increase across the shock on the magnetospheric side with a much smaller increase across the shock on the magnetosheath side. The detailed cause of the entropy changes remains unclear but appears to involve irreversible transfer of energy between thermal motion parallel and perpendicular to the magnetic field. The new results confirm the previously found presence of heavy ions and the values of the effective ion mass on both sides of the event. They also confirm the need for an ion pressure correction in the shock on the magnetospheric side. Back‐to‐back switch‐off shocks in magnetopause reconnection are examined by use of gyrotropic and pressure tensor modelsNormal heat fluxes are small, directed away from each shock. Total heat fluxes are larger, directed away from the reconnection siteThe CGL invariants show large anticorrelated variations and net entropy increases across each shock

Measurements from the Magnetospheric Multiscale (MMS) mission are reported to show distinct features of electron energization and mixing in the diffusion region of the terrestrial magnetopause reconnection. At the ion jet and magnetic field reversals, distribution functions exhibiting signatures of accelerated meandering electrons are observed at an electron out‐of‐plane flow peak. The meandering signatures manifested as triangular and crescent structures are established features of the electron diffusion region (EDR). Effects of meandering electrons on the electric field normal to the reconnection layer are detected. Parallel acceleration and mixing of the inflowing electrons with exhaust electrons shape the exhaust flow pattern. In the EDR vicinity, the measured distribution functions indicate that locally, the electron energization and mixing physics is captured by two‐dimensional reconnection, yet to account for the simultaneous four‐point measurements, translational invariant in the third dimension must be violated on the ion‐skin‐depth scale. Distribution functions of accelerated meandering electrons in the diffusion region are observedEffects of meandering electrons on the electric field normal to the reconnection layer are detectedMixing of the inflowing and exhaust electrons shapes the exhaust flow pattern

We discuss observations of reconnection, obtained by Time History of Events and Macroscale Interactions during Substorms (THEMIS) D during an outward bound traversal of the low‐latitude dayside magnetopause. The reconnection signatures include high magnetic shear, a southward directed Alfvénic jet, bounded by slow‐mode shocks near the switch‐off limit (as in the symmetric Petschek geometry), a small, sunward directed normal magnetic field and plasma inflow into the jet from both sides. We conclude that cold, unmeasured ionospheric ions helped establish the symmetry. The effective ion mass, estimated from the switch‐off condition, was 2.39 amu on the magnetospheric side, where the number density was inferred from the spacecraft potential, and 1.09 amu on the magnetosheath side. After a modest pressure correction in the magnetospheric shock, the MHD jump conditions for density, pressure, temperature, and entropy were well satisfied. The shock jumps were much larger on the magnetosphere side than on the magnetosheath side; we show this to be a plasma βeffect. The main dissipation mechanism appears to be irreversible transfer between thermal motion parallel and perpendicular to the field, such that both shocks bring about approximate downstream temperature isotropy. Hall currents and electric fields were present, albeit in a strongly asymmetric configuration. The magnetospheric shock had longer duration than the magnetosheath one, possibly as a result of a nonconstant magnetopause speed. We infer an average earthward magnetopause speed (14 km/s), corresponding nominal shock thicknesses (12 and 6 λi), dimensionless reconnection rates (0.061–0.085), and reconnection wedge angles (5° between shocks; 13° between separatrices). Unique magnetopause reconnection event, containing Alfvénic plasma jet wedged between switch‐off shocks, has been discovered and analyzedMHD shock jump conditions account well for density, pressure, temperature, and entropy changes, and their dependence on the plasma betaSwitch‐off condition reveals the presence of heavy ions in the event and allows determination of the effective ion mass

We report results of our multi‐spacecraft analysis of a solar wind reconnecting current sheet (RCS) and its solar wind magnetic hole (SWMH) observed on November 20, 2018. In the solar wind, the normal vector to the current sheet plane makes an angle of 32° with the Sun‐Earth line. A combination of tilted current sheet plane and foreshock effects cause an asymmetric interaction with the bow shock, in which the structure arrives at the quasi‐perpendicular side of the bow shock before the quasi‐parallel side. The magnetic field strength inside the magnetic hole decreases by ∼69 percent in the solar wind, with a similar depression rate observed inside the magnetosheath due to this structure. The solar wind flow slowdown and deflection during the bow shock crossing significantly disrupt the reconnection exhausts within the RCS. The interaction of the RCS and SWMH with the bow shock creates enhanced fluxes of accelerated electrons and ions. Plasma flow deflection in the magnetosheath also increases with the passage of the RCS. The ion density and temperature both increase within the current sheet to form a roughly pressure balanced structure. Field rotation and change in the dynamic pressure during this event modify the reconnection zones at the magnetopause and cause asymmetric inward motions in portions of the bow shock and the magnetopause boundaries (i.e., deformation). Unlike localized magnetosheath jets, an RCS and its associated SWMH in the solar wind have a global impact on the bow shock and the magnetopause. Space Weather is the study of effects of solar inputs on the space environment surrounding Earth. A source of solar input is through the solar wind, a stream of charged particles from the Sun carrying the interplanetary magnetic field. In this study, we analyze effects of a particular type of solar wind anomaly on Earth. The structure is initially observed by solar wind monitors far upstream of Earth, and later appears in the data of several near Earth spacecraft. We show that the structure can pass through the outer most boundary around Earth, the bow shock, and propagate closer to Earth. This study has significance in shaping our understanding of space weather as it describes near‐Earth effects of a commonly observed solar wind phenomenon. Asymmetric interaction is caused by the current sheet plane orientation in the solar wind and foreshock effectsFlux of accelerated electrons and ions increase in the magnetosheath due to current sheet and magnetic hole interactions at the bow shockThe structure causes deformation of the bow shock and magnetopause boundaries and modulates the reconnection process at the magnetopause Asymmetric interaction is caused by the current sheet plane orientation in the solar wind and foreshock effects Flux of accelerated electrons and ions increase in the magnetosheath due to current sheet and magnetic hole interactions at the bow shock The structure causes deformation of the bow shock and magnetopause boundaries and modulates the reconnection process at the magnetopause

The article focuses on the potential of e-book business models for public libraries. Various business models have been used to support marketing of e-books into those libraries including the Store Front, Short Embargo with Premium Pricing Available and Preview Model. The benefits and limitations of e-book business models to libraries and publishers including single user, limited number of loans, and replication of the print book business models. Digitization of printed books was also addressed, where it began with the Rocket e-Book and Peanut Press.

We report an accelerated plasma flow event detected by Wind at the low‐latitude dawn tail magnetopause (xGSE≈−10 RE) when the local magnetic shear across the magnetopause was high (∼180°) and the GSM ycomponent of the interplanetary magnetic field was positive and much larger than the zcomponent. High time resolution (3 s) three‐dimensional ion and electron distributions were obtained for this event. We have performed rigorous tests of fluid and particle predictions of reconnection. Consistent with reconnection, we observed at the magnetopause (1) jetting of plasma, with a flow speed, measured in the deHoffmann‐Teller frame, at 98% of the Alfvén speed; (2) mixing of a nearly isotropic hot plasma sheet ion distribution with a field‐aligned magnetosheath distribution having a low‐energy cutoff at the predicted deHoffmann‐Teller velocity; (3) opposite streaming of magnetosheath and plasma sheet electrons consistent with open field topology; and (4) a finite inward (earthward) directed normal magnetic field (BN<0) at and an associated earthward plasma flow (at 94% of the normal Alfvén speed) across the magnetopause. The combined fluid and particle signatures provide a comprehensive set of evidence for reconnection at the magnetopause. These reconnection signatures were observed in the tail flank magnetopause, where the presence of fast plasma flow (at almost twice the local Alfvén speed) in the adjacent magnetosheath has been predicted to suppress reconnection. The sense of the flow enhancement, the direction of the electron heat flux, and the polarity of BNare all consistent with each other and with the spacecraft being located tailward and northward of the reconnection site. Our analysis places the reconnection site ∼7 Earth radii south of the magnetic equator. The dimensionless reconnection rate at this flank magnetopause is estimated to be in the range of 0.1 to 0.2, which is similar to values reported for the subsolar region. In essence, the present event provides unambiguous evidence for reconnection and shows that reconnection signatures at the tail flank magnetopause are not noticeably different from those predicted and observed in the subsolar region.

We have analyzed 4 days of Wind observations of high‐speed convective flows of up to ∼800 km s−1in the plasma sheet at XGSE∼ − 60 REduring late March and early April 1999. Both earthward and tailward flows were observed. The high‐speed flows had a duration of several hours, unlike the shorter‐lasting (tens of minutes) bursty bulk flows, which are typically observed closer to the Earth. We have analyzed in detail a ∼10 hour interval of high‐speed flows detected during rather low geomagnetic activity and northward interplanetary magnetic field. Our analysis indicates that the fast flows are produced by magnetic reconnection and that the observed flow reversals are consistent with the passage of a reconnection X line. First, the results of the shear stress balance test (the Walén test) indicate that the flow in the deHoffmann‐Teller frame, which is aligned with the magnetic field, has an average flow speed that is ∼60% of the Alfvén speed, consistent with the presence of slow shocks in the magnetotail reconnection layer. Furthermore, the slope of the Walén regression line switches sign at the flow reversals, as expected from reconnection. Consistent with the passage of a reconnection X line, the magnetic field component normal to the neutral sheet also reverses sign at the flow reversals. For this event the tailward flowing plasma is hotter than the earthward flowing plasma, consistent with the two plasmas being magnetically disconnected. Our observations imply that quasi‐steady reconnection can occur in the midmagnetotail region during periods of persistent northward interplanetary magnetic field.

The Windspacecraft, launched on November 1, 1994, is a critical element in NASA’s Heliophysics System Observatory (HSO)—a fleet of spacecraft created to understand the dynamics of the Sun‐Earth system. The combination of its longevity (>25 years in service), its diverse complement of instrumentation, and high resolution and accurate measurements has led to it becoming the “standard candle” of solar wind measurements. Windhas over 55 selectable public data products with over ∼1,100 total data variables (including OMNI data products) on SPDF/CDAWeb alone. These data have led to paradigm shifting results in studies of statistical solar wind trends, magnetic reconnection, large‐scale solar wind structures, kinetic physics, electromagnetic turbulence, the Van Allen radiation belts, coronal mass ejection topology, interplanetary and interstellar dust, the lunar wake, solar radio bursts, solar energetic particles, and extreme astrophysical phenomena such as gamma‐ray bursts. This review introduces the mission and instrument suites then discusses examples of the contributions by Windto these scientific topics that emphasize its importance to both the fields of heliophysics and astrophysics. The Windspacecraft is a south ecliptic pointed spinning spacecraft that was launched on November 1, 1994. It is equipped with an array of instrument suites that measure electric and magnetic fields, electrons from thermal to relativistic energies, protons and alpha‐particles from thermal to suprathermal energies, and energetic ions from hydrogen to trans‐iron elements. Windcan also observe remote sources of electromagnetic radiation in the radio and gamma‐ray frequency ranges. This diverse array of instrumentation and numerous near‐Earth environments explored has allowed researchers to examine such a broad range of research topics including astrophysics, turbulence, kinetic physics, magnetic reconnection, interplanetary and interstellar dust, transient solar phenomena, and the radiation belts. Examples of the contributions of Windto the fields of heliophysics and astrophysics are reviewed. Windhas made seminal advances to the fields of astrophysics, turbulence, kinetic physics, magnetic reconnection, and the radiation beltsWindpioneered the study of the source and evolution of solar radio emissions below 15 MHzWindrevolutionized our understanding of coronal mass ejections, their internal magnetic structure, and evolution Windhas made seminal advances to the fields of astrophysics, turbulence, kinetic physics, magnetic reconnection, and the radiation belts Windpioneered the study of the source and evolution of solar radio emissions below 15 MHz Windrevolutionized our understanding of coronal mass ejections, their internal magnetic structure, and evolution

The article focuses on report of the U.S. Federal Agency and Federal Library on the National Center for Education Statistics Library Statistics Program, which surveys on the academic and public libraries in the U.S. Topics discussed include statistics of academic libraries from 1988 to 1998, survey of elementary and secondary schools and evaluation of public school district finance information. It also mentions the collection of statistic through web based data collection system.

A section of Part 1 of the book "Library & Book Trade Almanac" is presented, focusing on the Library Statistics Program initiated by the U.S. National Center for Education Statistics (NCES) in 1989. The aim was to collect and disseminate more complete statistical information about libraries. It details the two surveys administered by the NCES, the Academic Libraries Survey (ALS) and the School Library Media Centers Survey. Also discussed is how to obtain printed and electronic products.

The article discusses the programs and activities of the National Center for Education Statistics (NCES) Library Statistics Program of the U.S. Department of Education headquartered in Washington, D.C. as of May 2011. It explores the library surveys conducted by NCES, namely, the Academic Libraries Survey (ALS) and School Library Media Centers Survey (SLMCS). NCES publishes reports in the First Look format which includes a short collection of tables that list state and national totals. The NCES Web site at http://nces.ed.gov/pubsearch provides free downloads of NCES publications and edited raw data files from the surveys. The NCES Electronic Catalog on the site offers out-of-print publications and data files.

This section of the "Library and Book Trade Almanac," 54th edition focuses on the formal library statistics program initiated by the U.S. National Center for Education Statistics (NCES) that included surveys on academic libraries, school library media centers, public libraries and state libraries in 1989. The Academic Libraries Survey conducted by the NCES provides descriptive statistics from more than 3,000 libraries in the 50 states, the District of Columbia, and the outlying areas of the U.S.

Hot Flow Anomalies (HFAs) are transients observed at planetary bow shocks, formed by the shock interaction with a convected interplanetary current sheet. The primary interpretation relies on reflected ions channeled upstream along the current sheet. The short duration of HFAs has made direct observations of this process difficult. We employ high resolution measurements by NASA's Magnetospheric Multiscale Mission to probe the ion microphysics within a HFA. Magnetospheric Multiscale Mission data reveal a smoothly varying internal density and pressure, which increase toward the trailing edge of the HFA, sweeping up particles trapped within the current sheet. We find remnants of reflected or other backstreaming ions traveling along the current sheet, but most of these are not fast enough to out‐run the incident current sheet convection. Despite the high level of internal turbulence, incident and backstreaming ions appear to couple gyro‐kinetically in a coherent manner. Shock waves in space are responsible for energizing particles and diverting supersonic flows around planets and other obstacles. Explosive events known as Hot Flow Anomalies (HFAs) arise when a rapid change in the interplanetary magnetic field arrives at the bow shock formed by, for example, the supersonic solar windplasma flow from the Sun impinging on the Earth's magnetic environment. HFAs are known to produce impacts all the way to ground level, but the physics responsible for their formation occur too rapidly to be resolved by previous satellite missions. This paper employs NASA's fleet of four Magnetospheric Multiscale satellites to reveal for the first time clear, discreet populations of ions that interact coherently to produce the extreme heating and deflection. MMS observations reveal distinct ion velocity‐space populations within a Hot Flow Anomaly (HFA)The HFA interior varies smoothly in density with a swept‐up pressure excess toward the trailing edgeThe HFA interior displays coherent kinematic coupling between antisunward and sunward backstreaming ions