69 resources related to Magnetic reconnection
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The Pulsed Power Conference is held on a biannual basis and serves as the principal forum forthe exchange of information on pulsed power technology and engineering.
IEEE International Conference on Plasma Science (ICOPS) is an annual conference coordinated by the Plasma Science and Application Committee (PSAC) of the IEEE Nuclear & Plasma Sciences Society.
SoutheastCon is the annual Region 3 conference that brings together engineering professionals, students, and volunteers for a weekend of technical presentations, meetings, student competitions, and volunteer education.
Energy conversion and conditioning technologies, power electronics, adjustable speed drives and their applications, power electronics for smarter grid, energy efficiency,technologies for sustainable energy systems, converters and power supplies
The international IEEE Aerospace Conference is organized to promote interdisciplinaryunderstanding of aerospace systems, their underlying science, and technology
Physics, medicine, astronomy—these and other hard sciences share a common need for efficient algorithms, system software, and computer architecture to address large computational problems. And yet, useful advances in computational techniques that could benefit many researchers are rarely shared. To meet that need, Computing in Science & Engineering (CiSE) presents scientific and computational contributions in a clear and accessible format. ...
Research, development, design, application, construction, installation, and operation of electric power generating facilities (along with their conventional, nuclear, or renewable sources) for the safe, reliable, and economic generation of electrical energy for general industrial, commercial, public, and domestic consumption, and electromechanical energy conversion for the use of electrical energy
Science and technology related to the basic physics and engineering of magnetism, magnetic materials, applied magnetics, magnetic devices, and magnetic data storage. The Transactions publishes scholarly articles of archival value as well as tutorial expositions and critical reviews of classical subjects and topics of current interest.
Plasma science and engineering, including: magnetofluid dynamics and thermionics; plasma dynamics; gaseous electronics and arc technology; controlled thermonuclear fusion; electron, ion, and plasma sources; space plasmas; high-current relativistic electron beams; laser-plasma interactions; diagnostics; plasma chemistry and colloidal and solid-state plasmas.
Fundamental technologies used in the control and conversion of electric power. Topics include dc-to- dc converter design, direct off-line switching power supplies, inverters, controlled rectifiers, control techniques, modeling, analysis and simulation techniques, the application of power circuit components (power semiconductors, magnetics, capacitors), and thermal performance of electronic power systems.
IEEE Transactions on Plasma Science, 2000
Coronal mass ejections (CMEs) appear to originate preferentially in regions of the Sun's corona that are sigmoidal, i.e., have sinuous S or reverse-S shapes. Yohkoh solar X-ray images have been studied before and after a modest number of Earth-directed (halo) CMEs. These images tend to show sigmoidal shapes before the eruptions and arcades, cusps, and transient coronal holes after. Using ...
2016 IEEE International Conference on Plasma Science (ICOPS), 2016
Summary form only given. The experimental research of fusion DD reaction was provided on the dense plasma focus (DPF) device at the current above 1 MA and the total neutron yield at the level of 1010. The multiframe interferometry and X-ray diagnostics imaged the evolution of toroidal and plasmoidal structures, formed by closed currents with poloidal and toroidal components. The ...
IEEE Transactions on Plasma Science, 2005
The evolution of the collisionless tearing mode instability is studied using an electromagnetic gyrokinetic /spl delta/f particle-in-cell simulation model. Drift-kinetic electrons are used. High resolution, small box (less than 10 ion gyroradii) simulations have been well benchmarked with eigenmode analysis and their nonlinear evolution agrees well with theory. In this regime, the ion response is not important and can be ...
IEEE Transactions on Plasma Science, 2000
Geomagnetic storms have been studied for more than a century and substorms for nearly four decades. The space era which began in the late 1950s has ushered new discoveries and given new practical importance to this scientific discipline as we continue to amass technological assets in space. Geomagnetic storms and substorms pose hazards to our venture into the final frontier, ...
2004 Asia-Pacific Radio Science Conference, 2004. Proceedings., 2004
Fast magnetic reconnection and the related magnetic loop (plasmoid) are studied on the basis of MHD (magnetohydrodynamic) simulations. When the upstream magnetic field region is of sufficiently low beta, and the magnetic diffusion region is strongly localized, the reconnection jet can be supersonic, leading to the formation of a fast shock in front of the downstream magnetic loop (plasmoid), and ...
A Discussion on Hard Drives
Perpendicular magnetic anisotropy: From ultralow power spintronics to cancer therapy
Magnetic Nanowires: Revolutionizing Hard Drives, RAM, and Cancer Treatment
HYUNSOO YANG - IEEE Magnetics Distinguished Lecture
Spin Dynamics in Inhomogeneously Magnetized Systems - Teruo Ono: IEEE Magnetics Society Distinguished Lecture 2016
Magnetic Shield Implementation - EMC Society Demo
35 Years of Magnetic Heterostructures
High Magnetic Field Science and its Application in the US - ASC-2014 Plenary series - 10 of 13 - Friday 2014/8/15
IEEE Magnetics 2014 Distinguished Lectures - JONATHAN COKER
Magmites: Wireless Resonant Magnetic Microrobots
ISEC 2013 Special Gordon Donaldson Session: Remembering Gordon Donaldson - 6 of 7 - A high sensitive magnetometer system for natural magnetic field measurements
HARI SRIKANTH - IEEE Magnetics Distinguished Lecture
IEEE Magnetics 2014 Distinguished Lectures - Tim St Pierre
Magnetic Materials and Magnetic Devices - Josep Fontcuberta: IEEE Magnetics Distinguished Lecture 2016
ASC-2014 SQUIDs 50th Anniversary: 4 of 6 - Keiji Enpuku
Towards Logic-in-Memory circuits using 3D-integrated Nanomagnetic Logic - Fabrizio Riente: 2016 International Conference on Rebooting Computing
IMS 2015: Robert H. Caverly - Aspects of Magnetic Resonance Imaging
Nanoscale Magnetism with Picosecond Time Resolution and High Sensitivity - Hendrik Ohldag - IEEE Magnetics Distinguished Lecture
ISEC 2013 Special Gordon Donaldson Session: Remembering Gordon Donaldson - 5 of 7 - SQUID Instrumentation for Early Cancer Diagnostics
Coronal mass ejections (CMEs) appear to originate preferentially in regions of the Sun's corona that are sigmoidal, i.e., have sinuous S or reverse-S shapes. Yohkoh solar X-ray images have been studied before and after a modest number of Earth-directed (halo) CMEs. These images tend to show sigmoidal shapes before the eruptions and arcades, cusps, and transient coronal holes after. Using such structures as proxies, it has been shown that there is a relationship between sigmoidal shape and tendency to erupt. Regions in the Sun's corona appear sigmoidal because their magnetic fields are twisted. Some of this twist may originate deep inside the Sun. However, it is significantly modulated by the Coriolis force and turbulent convection as this flux buoys up through the Sun's convection zone. As the result of these phenomena, and perhaps subsequent magnetic reconnection, magnetic flux ropes form. These flux ropes manifest themselves as sigmoids in the corona. Although there are fundamental reasons to expect such flux ropes to be unstable, the physics is not as simple as might first appear, and there exist various explanations for instability. Many gaps need to be filled in before the relationship between sigmoids and CMEs is well enough understood to be a useful predictive tool.
Summary form only given. The experimental research of fusion DD reaction was provided on the dense plasma focus (DPF) device at the current above 1 MA and the total neutron yield at the level of 1010. The multiframe interferometry and X-ray diagnostics imaged the evolution of toroidal and plasmoidal structures, formed by closed currents with poloidal and toroidal components. The spontaneous evolution starts by the dominant toroidal current, continues by increase of the poloidal component and finished by the dominant poloidal one. The transformations are realized by reconnection of magnetic lines, similarly as in tokamak and astrophysical1 or in laser produced fusion plasmas 2. The ordered structures in DPF are similar to the field reverse and spheromak-like configurations with confined plasma in which the pressure of the pinching current is equaled by the pressures of the compressed plasma and repulsive component of magnetic field. The neutron production of fusion neutrons correlates with the formation and decay of plasmoids. We present the estimation of the radial distribution of the poloidal and toroidal current, its filamentary form3 and the possible acceleration mechanism of fast particles at the release of the part of magnetic energy during reconnection.
The evolution of the collisionless tearing mode instability is studied using an electromagnetic gyrokinetic /spl delta/f particle-in-cell simulation model. Drift-kinetic electrons are used. High resolution, small box (less than 10 ion gyroradii) simulations have been well benchmarked with eigenmode analysis and their nonlinear evolution agrees well with theory. In this regime, the ion response is not important and can be either fixed, adiabatic or fully gyrokinetic. Here, results are presented with larger box sizes (64 ion gyroradii radially) where the ion gyrokinetic response is important and cannot be neglected. In these larger box simulations, the instability exhibits an odd parity, different than the even tearing parity.
Geomagnetic storms have been studied for more than a century and substorms for nearly four decades. The space era which began in the late 1950s has ushered new discoveries and given new practical importance to this scientific discipline as we continue to amass technological assets in space. Geomagnetic storms and substorms pose hazards to our venture into the final frontier, much like adverse atmospheric weather does to our outdoor activity. This tutorial provides an overview of the main characteristics of these space phenomena and a brief review of the present theories concerning their initiation. For geomagnetic storms, the two prevailing views on their cause are discussed. One considers a storm to be the accumulated effects of a series of substorms while the other considers it to be the result of strong and prolonged enhancement of the global magnetospheric electric field. A synergistic model combining elements from both views is proposed as the likely explanation for the cause of geomagnetic storms. For substorms, there are generally four categories of models. The first proposes some plasma instabilities or externally-imposed reduction in the magnetospheric electric field at the near-Earth region. The second calls for magnetic reconnection occurring in the mid-tail environment. The third focuses on coupling the ionosphere to the magnetosphere while the fourth invokes abstract descriptions in nonlinear dynamics to address some statistical characteristics of substorms. An evaluation of observations and these models suggests that substorm onset may not be uniquely attributed to a single physical process.
Fast magnetic reconnection and the related magnetic loop (plasmoid) are studied on the basis of MHD (magnetohydrodynamic) simulations. When the upstream magnetic field region is of sufficiently low beta, and the magnetic diffusion region is strongly localized, the reconnection jet can be supersonic, leading to the formation of a fast shock in front of the downstream magnetic loop (plasmoid), and hence strong plasma heating (compression) in the magnetic loop. According to MHD simulations, this reconnection process is basically established by two steps of plasma acceleration, slow shock acceleration and adiabatic expansion acceleration. On the other hand, when the beta value is higher, subsonic reconnection occurs. In that case, fast shock does not appear and, hence, plasma heating and compression become weak. It is first shown how that is the difference between supersonic and subsonic magnetic reconnections. Second, showing the compression ratio obtained from the MHD simulations, the positive feedback enhancement of the plasma compression (heating) is caused only in the supersonic case.
The radio emission of the Sun in 3-mm range observations are the important source of the information about dynamics of evolution of solar active regions. The solar flares observations allow investigation the physical processes accompanying these phenomena. Their variety determines uniqueness of each solar flare. Solar flares are the result of abundant magnetic field annihilation during magnetic lines reconnection. Abundant magnetic field energy accumulation occurs at the vortex motion of the magnetized plasma of photosphere due to pressing a magnetic field and the stretching of magnetic tubes. The magnetic lines of a various direction approach results in appearance of the high-power current layers between them for compensation a tangential gap. Current layers dissipate at reconnection of magnetic lines. It causes flare high- temperature heating of plasma in the field of magnetic reconnection. Thus there are an acceleration of free electrons up to high energy and electromagnetic energy radiation by them in broad frequency band.
Summary form only given. Observational evidence suggests the presence of a plasma double layer (DL) above the surface of the Sun. Such a DL, together with a single charge layer (SL) directly below it, provides a straight-forward explanation for the existence of the temperature minimum in the lower corona, the X-ray emissions observed above sunspots, and the variations observed in the intensity of the solar wind. This plasma sheath is arguably a generic feature, in varying degree, surrounding all stars. Thus, this mechanism would affect stellar physics and plasma cosmology at their most fundamental level. These three charge layers constitute a pnp junction transistor-like mechanism. The action produced by this morphology controls (varies) and even cuts-off the solar wind. Acceleration of solar wind ions within the DL causes the observed temperature inversion. The failure of the invention of magnetic reconnection to explain these several observed solar phenomena is clear. A three-layer charge density structure, similar to the SL, DL anode tufting combination that is familiar to plasma engineers is a hypothesis that offers a reasonable explanation without the invention of "new science".
In this paper, using Cluster multi-spacecrafts observation data during January to April of each year from 2001 to 2006, we have studied the solar wind penetration events into the Earth's high-latitude magnetosphere. When the IMF is northward, although the formation of the entry layers depends on the direction of IMF, we pointed out that it mainly depends on the IMF Bx component and the influences of IMF By component could be weak.
Students attending the Center for Integrated Space Weather Modeling (CISM) summer school [Simpson, 2004; Gross et al., 2009] not only ask questions of the lecturers but also submit written questions at the end of each lecture sessions. Over the last decade we have collected approximately 3000 of these submitted questions about space weather and associated physical processes. This article addresses questions commonly asked about magnetic reconnection. Some of the questions are about points that are unclear, while others illuminate how students process new or reprocess previous information and sometimes form common misconceptions about reconnection. Some of these issues arise when students apply conceptual plasma approximations (e.g., “frozen-in- flux” or “particles trapped on field lines”) and apply them inappropriately. Another source of student misconceptions is the use of the term reconnection by researchers to describe both the process that reconnects the magnetic field at the reconnection point and also the results of field reconfiguration—accelerated and heated plasmas, high-energy particles, and X-rays emissions. Students may also interpret the standard schematic drawing of X-point reconnection literally, believing that reconnection is confined to a plane, and they often misinterpret the relevant length scales. In addition, student questions indicate that they treat field lines, rather than the fields themselves, as physical objects. The questions below are composite questions gleaned from review of the actual questions that students asked during more than a decade of summer schools. Along with identifying the questions, the aim of this article is to document the responses and provide a few useful references for instructors and students. Rather than a scholarly review of the subject, this manuscript provides succinct answers to common questions about magnetic reconnection.
This paper reviews the basic principles and techniques involved in formulating particle-in-cell (PIC) simulation models which can be used to address medium- and large-scale problems in magnetosphere electrodynamics. The limitations imposed by the underlying kinetic physics of a plasma are emphasized, and representative algorithms are described for full particle and hybrid (particle ions, fluid electrons) models. Issues related to the choice of initial and boundary conditions and the implementation of PIC models on massively parallel computers are discussed. Explicit examples involving the diffusion region in collisionless reconnection, plasma sheet convection, and large scale structure in magnetic reconnection are presented to illustrate the current capabilities of PIC models.
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