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Electron pitch angle distributions (PADs) are crucial to revealing electron acceleration and heating in geospace. The electron PADs in the Earth's magnetotail have been widely studied by statistical or case analysis. However, the statistical features of electron PADs in tailward flows are still unclear. We survey data from the Magnetospheric Multiscale (MMS) satellite to statistically investigate electron PADs in tailward flows in the Earth's magnetotail for the first time. We find that for most (66.3%) tailward flows, electrons with energy from 0.1 to 30 keV are mainly field‐aligned. The PADs of suprathermal (>2 keV) electrons in a part of tailward flows (26.3%) are mostly isotropic. Additionally, the perpendicular‐dominated PADs of suprathermal electrons only exist in a few (7.4%) tailward flows. According to the different dominant PADs of suprathermal electrons, the tailward flows are classified into three types: field‐aligned‐dominated type, isotropic‐dominated type and perpendicular‐dominated type flows. The dependence of electron PADs on plasma environmental parameters is investigated in these three types of flows. For field‐aligned‐dominated type flows, the field‐aligned anisotropy decreases toward the central plasma sheet (CPS) and with the increase of the energy. In addition, it is found that the field‐aligned anisotropy in the field‐aligned‐dominated tailward flows reduces noticeably when the |Vix| exceeds 800 km/s. In isotropic‐dominated type flows, the field‐aligned anisotropy of electrons with energy ≥10 keV also shows a slight decreasing trend toward the CPS. For perpendicular‐dominated type flows, the perpendicular anisotropy exhibits two non‐monotonic processes, initially increasing and then decreasing with the increase of distance from the CPS; while becomes more evident for higher energy electrons. Our statistical results indicate that in tailward flows, electron anisotropy depends on the distance from the CPS, energy and plasma flow velocity. Tailward flows are associated with the transport of plasma toward the distant tail, and the statistical analysis of electron PADs in these flows can improve our understanding of the related electron dynamics in the magnetotail. Key Points: Statistically features of field‐aligned‐dominated, isotropic‐dominated and perpendicular‐dominated type tailward flows are revealedFor the field‐aligned‐dominated type flows, the field‐aligned anisotropy decreases toward the central plasma sheet and with the increase of the energyThe perpendicular pitch‐angle anisotropy in the perpendicular‐dominated type flows is more evident for higher energy electrons [ABSTRACT FROM AUTHOR]

Energy conversion between the fields and the particles occurs through various physical processes within space environments. Magnetic reconnection stands out as one such process capable of rapidly and massively releasing energy. The high‐speed outflow jets produced by reconnection can induce turbulence characterized by intermittent structures. In this study, we investigate the impact of guide field on the energy conversion associated with the magnetic topologies within these structures during reconnection. Utilizing both particle‐in‐cell simulations and observations from the Magnetospheric Multiscale mission, our findings suggest that a larger guide field present during reconnection leads to increased energy conversion as well as the generation of O‐type topology structures within the turbulent outflow. Our results provide significant evidence on the relationships between energy conversion and magnetic topologies within turbulent outflow of reconnection and the guide field conditions. Plain Language Summary: In space environments, various physical processes involve the conversion of energy between magnetic fields and particles. One such process is magnetic reconnection, which can rapidly release a large amount of energy. During magnetic reconnection, high‐speed outflow jets are generated, leading to the formation of turbulent structures. In our study, we investigate how the presence of a guide field affects the energy conversion process and the resulting magnetic topologies within these turbulent structures during reconnection events. Using both particle‐in‐cell simulations and observations from the Magnetospheric Multiscale mission, we explore the impact of guide fields on energy conversion and magnetic topologies. Our findings indicate that a larger guide field present during reconnection leads to increased energy conversion and the generation of specific magnetic topology structures known as O‐type topologies within the turbulent outflow. These results provide significant insights into the complex relationships between energy conversion processes, magnetic topologies, and guide field conditions during magnetic reconnection events in space. Understanding these relationships is crucial for advancing our knowledge of fundamental physical processes occurring in space environments. Key Points: Magnetic topology in the turbulent reconnection outflow is investigated through both Magnetospheric Multiscale (MMS) observations and particle‐in‐cell (PIC) simulationsA larger guide field can promote the generation of O‐type topology in the turbulent outflow of the reconnectionHigher energy conversion is contributed by those O‐type topologies in the presence of a larger guide field [ABSTRACT FROM AUTHOR]

While Mars lacks a global intrinsic magnetic field, it does exhibit crustal magnetic anomalies (mostly in its Southern Hemisphere). These crustal magnetic anomalies directly interact with solar wind, which forms a mini‐magnetosphere and a region denoted the mini‐magnetopause. Using magnetic field and plasma measurements from the Mars Atmosphere and Volatile Evolution, we report a novel case of magnetic reconnection at the Martian mini‐magnetopause. In this process, protons and oxygen ions from the Martian atmosphere were accelerated during reconnection and likely escaped along the outflow direction. Magnetic reconnection may occur between the interplanetary magnetic field and crustal magnetic fields at the Martian mini‐magnetopause, which contributes to planetary ion escape, solar wind entering the mini‐magnetosphere and the evolution of magnetic topology in the dayside Martian mini‐magnetosphere. Plain Language Summary: While Mars lacks a global intrinsic magnetic field, it does exhibit crustal magnetic anomalies. The solar wind from the sun accompanied by interplanetary magnetic field (IMF) directly interacts with this crustal magnetic field, similar to what occurs on Earth, albeit at a smaller scale. The boundary between the crustal field on Mars and the IMF is called the mini‐magnetopause. Magnetic reconnection is a fundamental process in astrophysical and space plasmas that can change the topology of magnetic field and effectively convert magnetic energy into thermal and kinetic energy. Using magnetic field and plasma measurements from the Mars Atmosphere and Volatile Evolution missions, we report direction observations of magnetic reconnection at the Martian mini‐magnetopause. Through magnetic reconnection at the mini‐magnetopause, the IMF reconnects with the magnetic field from the crustal field, forming new magnetic field lines that channel solar wind to enter the Martian atmosphere and planetary plasmas to escape. Key Points: Magnetic reconnection at the Martian mini‐magnetopause is reported for the first timeProton and oxygen ions from the mini‐magnetosphere are accelerated during magnetic reconnectionMagnetic reconnection at the mini‐magnetopause could cause solar wind to enter the mini‐magnetosphere [ABSTRACT FROM AUTHOR]

Using high‐resolution data from the Magnetospheric Multiscale mission, an electron‐only reconnection current sheet is found between two successive dipolarization fronts (DFs). The electron‐only reconnection occurs between the northward component of the magnetic field of the flux pileup region (FPR) of the first DF (DF1) and the southward component of the magnetic dip of the second DF (DF2). The faster DF2 compresses the FPR of DF1, which constitutes an anti‐parallel topology and reduces the thickness of the current sheet. Further analysis shows that the current sheet is unstable to the electron tearing instability, which may power the onset of the reconnection. Our results suggest that these two DFs may merge into one by the reconnection, which sheds light on the evolution of DFs during their earthward propagation. Plain Language Summary: Magnetic reconnection, releasing magnetic energy and energizing plasmas, are believed to be responsible for the explosive phenomena in space. Though reconnection has been investigated for decades, the onset of reconnection is elusive. Dipolarization fronts (DFs), important carriers in the transportation of mass, magnetic flux, and energy in the magnetotail, can be generated by reconnections and will integrate into the geomagnetic field at last. The generation of DFs and dynamics at DFs are thoroughly probed by simulations and observations. However, the evolution of DFs during their earthward propagation is rarely inspected. In this work, we present an observation of an electron‐only reconnection between two successive DFs. The latter DF compresses the former DF and reduces the thickness of the current sheet between them. Inside the reconnection current sheet, electron tearing instability is unstable, which may power the reconnection. By reconnection, these two DFs may merge. Our observations can improve our understanding of the evolution of DFs in the magnetotail. Key Points: An electron‐only reconnection current sheet is found between two dipolarization frontsThe current sheet is unstable to the electron tearing instabilityDF2 compresses DF1 and thins the current sheet, which may initiate electron tearing instability and trigger the reconnection [ABSTRACT FROM AUTHOR]

Identifying how different wave modes interaction with each other is an important topic in space physics. Using measurements from the Magnetospheric Multiscale (MMS) mission, we report an event in the Earth's magnetosheath where ultra‐low‐frequency (ULF) waves, whistler waves, and quasi‐electrostatic whistler harmonics were observed simultaneously. Specifically, our analyses show that the parallel components of ULF waves modulate the electron butterfly distributions which provide the free energy to the excitation of the observed whistler waves. Meanwhile, quasi‐electrostatic waves sharing frequencies that are nearly integral multiples of the frequency of the observed whistlers are identified as nonlinear harmonics of whistler waves. The close correlations between the whistler waves and the electric field harmonics, as well as the high bicoherence indexes within the frequency ranges of the whistlers and harmonics, suggest the significant nonlinear couplings between the whistler waves and quasi‐electrostatic whistler harmonics. Our work provides new insights to the interactions between waves at different frequency bands. Key Points: Ultra‐low‐frequency (ULF) waves, whistler waves, and quasi‐electrostatic whistler harmonics are observed simultaneously in the magnetosheath plasmaULF waves modulate the electron butterfly shaped distributions which provide free energy for the excitation of the observed whistler wavesQuasi‐electrostatic waves are identified as the whistler harmonics, and may be generated by the wave‐wave nonlinear coupling [ABSTRACT FROM AUTHOR]

Heavy particles are extensively detected in the space environment, especially in the solar wind and interplanetary magnetosphere. Various physical processes can be affected by the physical dynamics of heavy particles. One of the processes is magnetic reconnection, which converts the energy from the magnetic field to the particles. In the present study, we investigate the impact of heavy particles with increasing mass (i.e., mass-loading effect) on energy conversion rate during magnetic reconnection. The declined reconnection rate and energy conversion rates by this effect are captured as reported previously. After considering three major regions in reconnection, it reveals that the mass-loading effect decreases more energy conversion rate of positive species at the separatrix, affects the heavier species less in the inner electron diffusion region (EDR), and propels the formation of a non-zero electric field at reconnection front (RF). Our results provide a more comprehensive understanding of the magnetic reconnection with complicated plasma components. [ABSTRACT FROM AUTHOR]

Dipolarization fronts (DFs) are widely believed to host energy conversion processes. However, which mechanism is responsible for the energy conversion is still obscure. Using data from the Magnetospheric Multiscale mission, a current sheet is observed at a DF. This current sheet is caused by interchange instability bending the edge of the DF. Inside the current sheet, Hall electromagnetic field, super Alfvénic electron jets, demagnetization of ions and electrons, strong energy conversion, and steady ion flow and temperature are observed, indicating an electron‐only reconnection at the DF. The duskward plasma flow, which may be deflected by the DF, compresses the bent edges of the DF. As a result, the width of the current sheet between two adjacent bent edges of the DF reduces, and then reconnection begins. Our observations give direct evidence that magnetic reconnection results in energy conversion at a DF. Plain Language Summary: Magnetic reconnection is an explosive phenomenon in space, which can rapidly convert energy from magnetic field to particles. Dipolarization fronts are essential carriers of mass and energy from the magnetotail to the Earth. Strong energy conversion, considered to be even more significant than magnetic reconnection, is usually observed at dipolarization fronts. However, the specific mechanism responsible for the energy conversion at a dipolarization front is elusive. Using data from the Magnetospheric Multiscale mission, we present direct evidence of magnetic reconnection at a dipolarization front, leading to strong energy conversion. The reconnection occurs in the current sheet at the dipolarization front. The duskward diverted flow compresses the bent dipolarization front induced by interchange instability, resulting in reconnection. Key Points: A current sheet with strong energy conversion is found at a DFThe strong energy conversion at this DF is mainly caused by the magnetic reconnectionThe duskward diverted flow compresses the bent DF caused by interchange instability, leading to the reconnection [ABSTRACT FROM AUTHOR]

Magnetic reconnection is the physical process that converts the energy from the fields to the plasmas in space, astrophysical and laboratory plasmas. The Reconnection front (RF) is the structure generated in the reconnection outflow region and participates in the energy release budget. Here, we first report a novel crater structure of magnetic field behind the RF, which is well supported by both the in‐situ observations from the Magnetospheric Multiscale mission and kinetic particle‐in‐cell simulations. The theoretical explanations from the simulations suggests that the formation of the crater structure is possibly due to that high‐speed outflow electron jet from inner electron diffusion region constantly strikes the RF. From another perspective, the crater structure is the continuous impact of the electron jet. Our results can establish a new understanding of the RF and energy conversion during magnetic reconnection. Plain Language Summary: Magnetic reconnection is a natural process in space environments, astrophysical settings, and laboratories, where energy from magnetic fields is transformed into the energy of various particles. One crucial structure in this process is called the reconnection front (RF), which plays a big role in how energy is released. In our study, we have discovered something interesting: a unique crater‐like structure behind the RF. We found evidence for this in observations from the Magnetospheric Multiscale mission and computer simulations that study the behavior of particles in magnetic reconnection. Our simulations suggest that this crater shape happens because electrons have the high‐speed outflow and form current jets. It is like the electrons poured out from the inner electron diffusion region, hitting a speed bump. Another way to think about it is that this crater is formed by the continuous impact of fast‐outflowing electron jets. Understanding this crater structure helps us better grasp how the RF works and how energy changes during magnetic reconnection. Our research finds and tries to explain a new piece of the puzzle in understanding the mysteries of space and plasmas in the magnetic reconnection process. Key Points: A novel crater structure is first verified behind the Reconnection front (RF) by both Magnetospheric Multiscale observations and particle‐in‐cell simulationsThe formation of the crater structure appears to be associated with the high‐speed electron jets from inner electron diffusion regionA possible scenario that electron outflow constantly strikes the RF and then causes the formation of the crater structure [ABSTRACT FROM AUTHOR]

Electron vortices are usually embedded within different magnetic structures in space plasmas. The effects, including the nonideal electric field, energy dissipation and magnetic field, of electron vortices on these magnetic structures are still unclear. Utilizing the unprecedented high‐resolution data from the Magnetospheric Multiscale mission in the terrestrial magnetosheath, we statistically investigate these effects on magnetic structures. Both nonideal electric fields and energy dissipation have no obvious correlations with the scales of electron vortices. However, compared to the scales, stronger correlations are found between the vorticities of electron vortices and nonideal electric fields, and energy dissipation, respectively. Most of electron vortices have positive contributions to magnetic fields of magnetic structures, such as strengthening the decrease (or increase) of Bt for current sheets and magnetic holes (or flux ropes and magnetic peaks). Our results reveal that the electron vortices play an important role in the evolution of magnetic structures. Plain Language Summary: The magnetosheath exhibits various dynamical features such as heating and compression of the plasma, kinetic instabilities, particle beams and kinetic structures due to the highly dynamical environment in near‐Earth space. The electron vortices as the structure that manifests the in suit observations, including bipolar variations of electron velocity and large electron vorticity, have been revealed widely in the magnetosheath. However, the specific effects of electron vortices embedded within the magnetic structures on these magnetic structures are still unknown, especially in a statistical view. Thanks to the unprecedented high‐time resolution data of the Magnetospheric Multiscale mission in the magnetosheath, we investigated the effects, including the nonideal electric fields, energy dissipation and magnetic fields, of electron vortices on these magnetic structures. We find that the nonideal electric fields, energy dissipation inside the electron vortices is more significant than outside for most of magnetic structures, and more than half of electron vortices have positive effects on generating the measured magnetic field of these magnetic structures, which is helpful for understanding the subsequent evolution and interaction between them. Key Points: The effects of nonideal electric field, energy dissipation and magnetic field of electron vortices on magnetic structures have been studiedThe nonideal electric fields and energy dissipation are more correlated with the vorticities of electron vortices compared to their scalesMost of electron vortices have positive contributions to magnetic fields of magnetic structures [ABSTRACT FROM AUTHOR]

Magnetic reconnection is a fundamental physical process of rapidly converting magnetic energy into particles. The electron diffusion region (EDR) is the crucial region during magnetic reconnection. The outer EDR, which also plays a crucial role in magnetic reconnection, is responsible for energy conversion. In the outer EDR, the electrons are decelerated and return the energy to the magnetic field on the pileup region behind the reconnection front. In the present study, we used the fully kinetic particle‐in‐cell simulation and revealed that part of decelerated electrons in the outer EDR could even move back to the inner EDR. This phenomenon is caused by the dominant contribution from the magnetic tension force, and it suggests a magnetic Marangoni effect in space plasma, similar to the Marangoni effect in fluids. Our results potentially propose a brand‐new physical process and a novel mechanism in the EDR during magnetic reconnection. Plain Language Summary: Plasma's energy can be changed through various approaches in the universe, and magnetic reconnection is one of those approaches to convert energy from the magnetic field to the plasma. In the reconnection site, the inner electron diffusion region (EDR) is an essential area where the energy is released, and the electron's energy is enhanced significantly. Meanwhile, in the outer EDR, the electrons are decelerated by the electric field, thus their energy decreases. However, part of those electrons can move backward to the inner EDR, and how this phenomenon comes up has no further investigation. In this study, we use numerical simulations to reveal the possible mechanism of this kind of electron's motion. It is found that the electron deceleration is caused by the magnetic tensor force. The electrons with specific conditions have the possibility to move backward. Those backflow electrons have a second chance to be accelerated again in the inner EDR. Such electron motion in plasma physics is not a kind of gyro movement but might indicate a so‐called magnetic Marangoni effect similar to the Marangoni effect in fluid physics. Our findings propose a novel mechanism associated with electron acceleration in the EDR during magnetic reconnection. Key Points: The magnetic tension force causes the deceleration of the electrons in the outer electron diffusion region (EDR) during magnetic reconnectionPartial electrons are decelerated and even move back to the inner EDR, and they are accelerated again and attain higher energyThe electron backflow motion in the outer EDR indicates a magnetic Marangoni effect in space plasma [ABSTRACT FROM AUTHOR]

In Saturn's magnetosphere, the plasma temperature increases with radial distance, requiring a heating mechanism to counteract the adiabatic cooling effect of expanding plasma. To explore potential heating source, we perform a statistical study about intermittent structures and intermittent heating in Saturn's magnetosphere based on the observations from the Cassini spacecraft. Partial Variance of Increments (PVI) technique is used to measure the intermittency of magnetic field and identify the intermittent structures. It is found that the electron temperature has a rising trend as the increase of magnetic field intermittency, implying the occurrence of electron heating in the intermittent structures. Additionally, the turbulence heating rate also exhibits an increasing trend as the increase of probability density of intermittent structures. Our results evidence the effect of intermittent heating in the Saturn's magnetosphere, and suggest that intermittent structures with high magnetic field intermittency play an important role in turbulence heating. Plain Language Summary: In Saturn's magnetosphere, the plasma temperature increases with radial distance, requiring a heating mechanism to counteract the adiabatic cooling effect of expanding plasma. Intermittent structure, which has been widely investigated in solar wind turbulence to explain the solar wind plasma heating, have never been considered in Saturn's magnetosphere. In this work, we investigate the intermittent structures and intermittent heating in Saturn's magnetosphere based on the observations from the Cassini spacecraft. We identify a positive correlation between electron temperature and magnetic field intermittency, as well as a positive correlation between turbulence heating rate and the probability density of intermittent structures. These results suggest that intermittent structures contribute to turbulent heating in Saturn's magnetosphere. Key Points: Intermittent structures are identified in Saturn's magnetosphere based on partial variance of increment techniqueElectron temperature has a rising trend as the intermittency increases, indicating the occurrence of intermittent electron heatingTurbulence heating rate increases as intermittent density rises, implying a contribution of intermittent structure to turbulence heating [ABSTRACT FROM AUTHOR]

With high‐resolution data from Magnetospheric Multiscale (MMS) mission, an ion‐scale flux rope (FR) with a heavily tilted axis is observed in the tailward outflow of a magnetic reconnection in the terrestrial magnetotail. Combined with the field‐aligned electron distribution and positions of MMS when the X‐line and FR are observed, the tilted axis is inferred to be caused by the extension of the X‐line in the dawn‐dusk direction. J · E′ is negative and electrons are losing energy in the FR. An ion‐scale electron vortex embedded in the plane perpendicular to the axis is observed inside FR. The induced magnetic field generated by the electron vortex has the same direction as the axial component, which can contribute to the axial component and increase the magnetic flux of the FR. Such electron vortex FRs may be an essential carrier of magnetic flux from near‐Earth X‐line to distant X‐line or interplanetary space. Plain Language Summary: Magnetic reconnection is an efficient energy and magnetic flux release process in the magnetotail. It is well known that dipolarization front is an important carrier of magnetic flux to Earth. However, how the magnetic flux transports at the tailward side is rarely concerned. In this work, we present an observation of an electron vortex flux rope as a new possible candidate. The embedded electron vortex generates an induced magnetic field with the same direction as the axial component of the flux rope, which is self‐consistent and can contribute to the enhancement of the magnetic flux carried by the flux rope by converting energy from electrons to the magnetic field. Our observations can contribute to understand the dynamics of the magnetotail. Key Points: An ion‐scale flux rope with an electron vortex embedded is observed in the tailward outflow of a magnetic reconnection eventThe tilted axis of the flux rope is due to the extension of the X‐line in the dawn‐dusk directionThe electron vortex flux rope may be an essential carrier of magnetic flux to distant tail or interplanetary space [ABSTRACT FROM AUTHOR]

The Kolmogorov scaling in the inertial range of scales is a distinct characteristic of fully developed turbulence, and studying it offers valuable insights into the evolution of turbulence. In this work, we perform a statistical survey of the power spectra with the Kolmogorov scaling in Saturn's magnetosphere using Cassini measurements. Two cases study show that both magnetic‐field and electron density spectra exhibit f−5/3 at the MHD scales. The statistical analysis reveals a wide‐ranging and abundant presence of Kolmogorov spectra throughout magnetosphere, observed across all local times. Interestingly, the occurrence rate of these Kolmogorov‐like events within Saturn's magnetosphere surpasses that observed in the planetary magnetosheath. The measurements of magnetic compressibility for the Kolmogorov‐like events show the dominance of incompressible Alfvénic turbulence (44.64%) with respect to magnetosonic‐like one (6.94%). In addition, the source and evolution of the turbulent fluctuations are further discussed. Plain Language Summary: Turbulence is ubiquitous in space and astrophysical plasmas, such as the solar wind, planetary magnetospheres, and the interstellar medium. Plasma turbulence has been widely studied in the solar wind and planetary magnetosheaths, but much less in the planetary magnetospheres. In the solar wind, power spectral density of the magnetic field fluctuations generally follows the so‐called Kolmogorov spectrum f−5/3 at the magnetohydrodynamic (MHD) scales, which suggests a fully developed turbulent state. In this study, we have discovered the widespread presence of Kolmogorov spectra in the Saturn's magnetosphere. The spatial distribution and nature of turbulent fluctuation for the Kolmogorov‐like events are also investigated in detail. Key Points: Magnetic field and electron density spectra have Kolmogorov scaling of f−5/3 at MHD scales in Saturn's magnetosphereThe spatial distribution of the Kolmogorov spectra within Saturn's magnetosphere reveals the extensive occurrence of Kolmogorov‐like eventsThe fluctuations for Kolmogorov‐like events are dominated by Alfvénic modes (44.64%) with respect to magnetosonic‐like one (6.94%) [ABSTRACT FROM AUTHOR]

Neuromorphic computing devices, which emulate biological neural networks, are crucial in realizing artificial intelligence for information processing and decision-making. Different types of neuromorphic computing devices with varying resistance levels have been developed, such as oxide-based memristors caused by ion diffusion, phase transition-based devices caused by threshold switching, progressive crystallization/amorphization, and spintronics-based devices caused by magnetic domain switching. However, these devices face significant challenges, including disruptions in the reading process, limited scalability in integrated circuits, and non-linearity in weight change. To address these challenges, alternative approaches are required. In this study, we introduce a multi-layer-multi-terminal neuromorphic computing device based on the asymmetric temperature gradient. Our device exhibits a wide range of synaptic functions, including potentiation, depression, and both anti-symmetric and symmetric spike-timing-dependent plasticity. The thermal driving strategy offers an energy-efficient platform for future neuromorphic computing devices to achieve artificial intelligence. [ABSTRACT FROM AUTHOR]

BACKGROUND/OBJECTIVES: The prevalence of metabolic syndrome (MetS) and obesity has increased worldwide, as well as in Taiwan, particularly in women aged>40 years. The purpose of this study was to elucidate the effects of a calorie- restriction diet (CR) supplemented with protein and n-3 polyunsaturated fatty acids (PUFAs) on women with MetS. SUBJECTS/METHODS: A total of 143 eligible female participants were recruited and assigned to four dietary interventions such as 1500-kcal CR, calorie-restriction meal-replacement diet (CRMR), calorie-restriction diet with fish oil supplementation (CRF) and calorie-restriction meal-replacement diet with fish oil supplementation (CRMRF). The changes in anthropometric measures, metabolic profiles, inflammatory response and the Z-score of severity of MetS were evaluated. RESULTS: Among 143 female MetS patients enrolled, 136 patients completed the 12-week study. After the 12-week dietary interventions, we observed reductions in body weight (BW), body mass index (BMI) and waist circumference (WC) in all groups. BMI and triglyceride (TG) levels decreased significantly in the CRMR, CRF and CRMRF groups, but not in the CR group. The homeostasis model assessment of insulin resistance (HOMA-IR) had significantly improved in all four groups, and the levels of interleukin-6 (IL-6) and C-reactive protein (CRP) had significantly decreased in the CRF and CRMRF groups. Following the interventions, the changes in waist circumference (WC), mean arterial pressure (MAP), fasting blood glucose (FBG), TGs, HOMA-IR, CRP and IL-6 significantly correlated with the reductions in Z-score of MetS severity. CONCLUSIONS: Our study results indicate that a calorie-restriction dietary intervention combined with various macronutrients can reduce the severity of MetS in women and increase recovery from MetS by almost twofold in comparison with a CR alone. European Journal of Clinical Nutrition (2015) 69, 322-328;doi:10.1038/ejcn.2014.196; published online 24 September 2014, INTRODUCTION The prevalence of metabolic syndrome (MetS) has increased worldwide, in parallel with an increase in the rates of obesity. (1) Such trends have also occurred in Taiwan, particularly in [...]

Intense electromagnetic energy conversion and local magnetic flux transport occur at reconnection fronts (RFs) formed by magnetic reconnection. Tailward RFs (TRFs), characterized by sharply enhanced negative magnetic field normal components accompanied by tailward plasma flows, are the tailward propagating dipolarization fronts in the Earth's magnetotail. So far RFs and TRFs are observed merely at magnetized planets. Using data from Mars Atmosphere and Volatile EvolutioN, we report, for the first time, the observations of TRF embedded in a current sheet (possibly diffusion region of magnetic reconnection) in the Martian magnetotail. At the TRF, O+ and O2+ are accelerated in tailward direction; behind the TRF, the perpendicular electron fluxes enhance at the energy of 251–905 eV, which should be caused by betatron acceleration. The energized plasmas indicate that the electromagnetic energy converts to plasma kinetic energy around the TRF. Our observations suggest that RFs could occur in the planetary magnetotail without the global intrinsic dipole magnetic field. Plain Language Summary: Magnetic reconnection is a process that the anti‐parallel magnetic field lines break and reconnect, accompanied by explosive energy conversion. Without a global dipole magnetic field, Mars has interesting flexible magnetic fields in the magnetotail, which can be varied corresponding to the upstream interplanetary magnetic field. Magnetic reconnection occurs during the interplanetary magnetic field and Martian solar‐wind‐induced magnetosphere. Tailward reconnection fronts, characterized by sharply enhanced negative magnetic field normal components usually accompanied by tailward plasma flows, are generally formed by magnetic reconnection. Intense electromagnetic energy conversion occurs at reconnection fronts, consistent with local magnetic flux transport and global magnetotail flux reduction in the magnetotail. Utilizing measurements from the Mars Atmosphere and Volatile EvolutioN orbiter, for the first time we report the observations of tailward reconnection fronts in the near‐Mars magnetotail, which is unexpected for a planet without an intrinsic dipole magnetic field. Besides, ion acceleration and electron acceleration are found around the tailward reconnection fronts. Our work offers a new perspective and shows the importance of magnetic reconnection on the evolution of the near‐Mars magnetotail. Key Points: A tailward reconnection front is observed in the near‐Mars magnetotail for the first timeHeavy ion acceleration and electron acceleration are detected around the tailward reconnection frontReconnection fronts could occur in the planetary magnetotail without the global intrinsic dipole magnetic field [ABSTRACT FROM AUTHOR]

The topology of the magnetic and velocity fields at the kinetic scales are investigated in the context of nearly incompressible magnetosheath plasma turbulence. Using the unprecedented high‐resolution data from the Magnetospheric MultiScale mission, the joint probability distribution functions of geometrical invariants characterizing the magnetic and velocity fields gradient tensor at the kinetic scales are computed. The topological features of the magnetic and velocity field gradient tensors and their symmetric component tensors present axisymmetric distribution patterns, indicating that the structure of the plasma turbulence at the kinetic scales are different from those in hydrodynamic and magnetohydrodynamic turbulence. Moreover, a strong correlation between the straining and rotational parts of the magnetic and velocity field gradient tensors was found, which manifests the dominance of sheet‐like structures at the kinetic‐scales dissipation in incompressible plasma turbulence. Plain Language Summary: The terrestrial magnetosheath provides an excellent laboratory to study space plasma turbulence. Thanks to the unprecedented high time resolution data of the Magnetospheric Multiscale mission, the kinetic‐scales structures and dynamic of incompressible magnetosheath plasma turbulence can be investigated. By means of a universal topological classification method in fluid dynamics area, we construct the topological features of both magnetic and velocity field in incompressible plasma turbulence at dissipation scales. Our results show that the distribution of velocity‐field topological structures is different from the other turbulence system, such as hydrodynamic and magnetohydrodynamic turbulence. In addition, we verify that the sheet‐like structures dominate the kinetic‐scales dissipation in the incompressible plasma turbulence. Key Points: The kinetic‐scales topological features in incompressible magnetosheath plasma turbulence are investigatedDistribution patterns different from hydrodynamic and magnetohydrodynamic turbulence of velocity‐field topological characteristics are identifiedSheet‐like structures dominate dissipation‐scale dynamics in the incompressible plasma turbulence [ABSTRACT FROM AUTHOR]

The research and utilization of germplasm resources serves as an important basis for breeding good varieties of the medicinal orchid Dendrobium officinale. In this study, ISSR and SCoT molecular markers were used to study the genetic diversity and genetic relationships of 24 D. officinale germplasms. Ten ISSR primers and 12 SCoT primers amplified 81 and 96 gene loci, of which 81 and 95 loci were polymorphic, respectively. ISSR markers gave a genetic diversity index (H) of 0.3388, Shannon information index (I) of 0.5097, and genetic distance ranging from 0.1749 to 0.9605, with an average of 0.4414; SCoT markers gave an H of 0.3330, I of 0.5043, and genetic distance ranging from 0.1823 to 0.7577, with an average of 0.4331. The results of the UPGMA cluster analysis, PCoA, genetic structure analysis, genetic distance, and geographical distance analysis of the two molecular markers were quite different. Further analysis of ISSR + SCoT showed that the combination of the two markers was complementary, and could better reveal the genetic diversity and genetic relationships of D. officinale. The DNA fingerprints of 24 samples of D. officinale were constructed based on ISSR and SCoT markers. This study provides reliable theoretical support for variety classification, breeding, and germplasm identification of D. officinale. [ABSTRACT FROM AUTHOR]

The present paper deals mainly with the distribution features, briefly describes the geology in the three geothermal fields of different types in Beijing, Yangbajing of Xizang (Tibet), and Dengwu of Guangdong, and finally gives on account of the development and utilization of geothermal resources. Up to now, more, than 2,500 geothermal water points (including hot springs, hot-water wells, and hot water in mines) have been found. Four major geothermal zones and three basic types of geothermal resources can be preliminarily divided. In China, geothermal resources have been used for the purposes of power generating, industry and agriculture, medical treatment, etc. This article contains a sketch map showing the distribution of geothermal water in China. Cet article porte sur les caractéristiques de répartition, les types essentiels et les conditions de formation des ressources géothermiques, explique brièvement la géologie de trois types différents de champs géothermiques : Pékin, Yanbajin de Xiang (Tibet) et de Dengwu de Guangdong et enfin présente l'exploitation et l'utilisation des ressources géothermiques. Jusqu'à présent, on a découvert plus de 2500 points d'eaux géothermiques (y compris sources thermales, puits des eaux thermales et les eaux thermales apparues dans les mines). lis sont subdivisés en quatre zones géothermiques principales et trois types essentiels de ressources géothermiques. Les ressources géothermiques ont trouvé leur utilisation dans la production de l'électricité, dans l'industrie, l'agriculture et le traitement médical, etc. On trouve dans cet article une esquisse de répartition des ressources géothermiques de la Chine.

Magnetic reconnection can efficiently heat and accelerate the electrons through various approaches and mechanisms. The electron diffusion region (EDR), especially the inner EDR, is one of the energization areas for the electrons during the reconnection. How the electrons' energy changes when passing the inner EDR is not well understood. In this study, we investigate the electron energy change from the individual perspective using the full kinetic particle-in-cell simulation. It is revealed that the electron energy gain rate is related to both traveling time and path in the inner EDR. The energy from the magnetic field tends to be allocated to the electron perpendicular part and the random thermal part. Our results promote the understanding of the function of the inner EDR during magnetic reconnection. [ABSTRACT FROM AUTHOR]

We report one sort of weak physical unclonable functions (PUFs) composed of 14-nm nFinFETs with entropy of the random-trap-fluctuation (RTF). After the positive-bias-temperature-instability (PBTI) stress at high temperatures (85 °C ~ 150 °C), the generation of abundant random traps at the interface of gate-dielectric layers and channel efficiently improves cryptographic parameters of nFinFET-PUFs. Results show that bit-error-rates of the MOSAIC plots reduce to 1.4%; average values/standard-deviation of the inter- and intra- Hamming-distance reach 50.28%/1.7% and 0.38%/0.42%, respectively. This work provides an implacable technique to boost characteristics of weak PUFs through combinations of device-reliability and cryptography. [ABSTRACT FROM AUTHOR]