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31/07/2015, 14:30
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Prof. Hantao Ji (Princeton University)10/08/2015, 09:55Despite its disruptive influences on the large-scale structures of space and solar plasmas, the crucial topological changes and associated dissipation during magnetic reconnection take place only near an X-line within thin singular layers on the electron scales. While ion dissipation layers have been frequently detected, the existence of election layers near the X-line and the...Go to contribution page
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Prof. Paolo Ricci (CRPP, EPFL)10/08/2015, 11:10The methodology used to assess the reliability of numerical simulation codes constitutes the Verification and Validation (V&V) procedure. V&V is composed by two separate tasks: the verification process, which is a mathematical issue targeted to assess that the physical model is correctly solved by the numerical code, and the validation, which determines the consistency of the...Go to contribution page
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Dr Andrey Divin (St. Petersburg State University)10/08/2015, 11:35Electron diffusion region (EDR) is regarded as the key region of collisionless magnetic reconnection. Electrons are unmagnetized inside the EDR, and magnetic field lines are detached from plasma, allowing fast conversion of magnetic energy into energy of plasma. Large-scale kinetic simulations are required for understanding the EDR structure. In this study, two- dimensional...Go to contribution page
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Mr Ivo Furno (EPFL-CRPP)10/08/2015, 12:00Suprathermal ions with energies greater than the background plasma species are frequently observed during magnetic reconnection in astrophysical and laboratory plasmas. Understanding the interaction between turbulence and suprathermal ions is a fundamental problem to shed light on the physics governing many plasma phenomena, from particle dropouts during impulsive solar energetic...Go to contribution page
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Dr Sergio Servidio (University of Calabria)10/08/2015, 14:00Systematic analysis of numerical simulations of two-dimensional magnetohydrodynamic (2D MHD) turbulence reveals the presence of a large number of X-type neutral points, where magnetic reconnection locally occurs [1]. The associated reconnection rates are distributed over a wide range of values and scales, exhibiting a good agreement with existing theories of magnetic reconnection....Go to contribution page
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Ms Cecilia Norgren (Swedish Institute of Space Physics)10/08/2015, 14:25Lower hybrid waves in magnetic reconnection regions Lower hybrid waves are strong plasma waves that are often excited within thin boundaries that form in the vicinity of magnetic reconnection regions. These waves can be excited by sharp gradients in the density that can form along the separatrices or at the front of reconnection jets. The wave length scale is on the order of the...Go to contribution page
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Dr Narita Yasuhito (Austrian Academy of Sciences)10/08/2015, 14:50A wave-driven scenario of magnetic reconnection is presented, the whistler-wave hypothesis, to explain the triggering mechanism of the reconnection in space and astrophysical plasmas. Magnetic reconnection releases a huge amount of energy on a short time scale, and is believed to be in operation in the phenomena of auroral substorms, flares, and coronal mass ejections. The...Go to contribution page
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Dr Huishan Fu (Beihang University)10/08/2015, 15:45In this study, we apply a new method—the first-order Taylor expansion (FOTE)—to find magnetic nulls and reconstruct magnetic field topology, in order to use it with the data from the forth-coming MMS mission. We compare this method with the previously used Poincare index (PI), and find that they are generally consistent, except that the PI method can only find a null inside the...Go to contribution page
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Elin Eriksson (Swedish Institute of Space Physics, Uppsala, Sweden and Uppsala University, Department of Physics and Astronomy, Uppsala, Sweden)10/08/2015, 16:10Regions with vanishing magnetic field, also referred to as magnetic nulls, are of high interest in plasma physics. Near magnetic nulls particles become unmagnetized and can by interacting with electric fields be accelerated up to high energies. Magnetic nulls have been observed and studied before using in-situ observations for selected events. Here we present the first...Go to contribution page
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Dr Vyacheslav Olshevsky (KU Leuven)10/08/2015, 16:35Fully kinetic electromagnetic particle-in-cell code iPic3D is used to model magnetic reconnection in the variety of plasma configurations. We apply Poincare index technique to locate and identify the topological characteristics of the magnetic null points in different three- dimensional simulations. The relevance of magnetic nulls to energy dissipation, turbulence and plasma...Go to contribution page
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Prof. Klaus Galsgaard (Niels Bohr Institute - University of Copenhagen)11/08/2015, 09:00Magnetic flux emergence is a very important process in renewing the magnetic field of the solar corona. As new magnetic flux emergence from below the photosphere and reaches in to the corona, the situation for magnetic reconnection are setup in the battle for space between the old coronal magnetic field and the new emerging magnetic field. Numerical MHD experiments investigate this...Go to contribution page
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Dr Rumi Nakamura (IWF/OEAW)11/08/2015, 09:30In the Earth's magnetotail, there are two preferred sites for the magnetic reconnection. One is in the distant tail usually beyond the lunar orbit, and is considered to be semi-permanently present. The other is in the near tail at a distance of a few tens of Earth radius (Re), where the magnetic reconnection initially involves closed-field lines in the plasma sheet and hence...Go to contribution page
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Dr Daniel Graham (Swedish Institute of Space Physics)11/08/2015, 10:15Magnetic reconnection enables the accelerating and heating of electrons, leading to the formation of electron distributions, which can be unstable to a variety of instabilities. For instance, magnetic reconnection can accelerate electrons to form beams and counter-streaming electron populations, as well as loss cone distributions. Additionally, at Earth’s magnetopause...Go to contribution page
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Maria Hamrin (Umeå University)11/08/2015, 11:10In the vicinity of magnetic reconnection, magnetic energy is transferred into kinetic energy. Such a region hence corresponds to a electrical load and it should manifest itself as large and positive values of the power density, E.J>>0, where E and J are the electric field and the current density, respectively. From simple theoretical arguments we find that an event with...Go to contribution page
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Heli Hietala (Imperial College London, UK)11/08/2015, 11:35Magnetic reconnection redistributes energy by releasing magnetic energy into plasma kinetic energy - high speed bulk flows, heating, and particle acceleration. A significant portion of the energy released by magnetotail reconnection appears to go into ion heating, and the heating is anisotropic with the plasma temperature parallel to the magnetic field generally increasing more...Go to contribution page
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Dr Keizo Fujimoto (National Astronomical Observatory of Japan)11/08/2015, 12:00Understanding the wave properties in magnetic reconnection is very important in collisionless plasmas. The waves can transport the momentum and energy between the different species, resulting in the anomalous magnetic dissipation, particle heating, and the formation of non-thermal particles. Observations in the Earth’s magnetosphere and laboratory experiment have shown...Go to contribution page
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Dr Jonathan Eastwood (Imperial College London)11/08/2015, 14:00Magnetic reconnection is one of the most important processes at work in space plasma environments, controlling energy storage, transport and release. In particular, it is crucial to the physics of the solar wind - magnetosphere interaction because it can explosively release stored energy, transforming it into different forms in the reconnection outflow. Magnetotail reconnection...Go to contribution page
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Dr Sergio Toledo Redondo (Swedish Institute of Space Physics)11/08/2015, 14:25Recent studies show that cold ions (energies up to tens of eV) of ionospheric origin are present in the magnetosphere and often reach the magnetopause, participating in magnetic reconnection. At low latitudes they are abundant and even dominate over the hot magnetospheric ions. Owing to their smaller gyroradius, they remain magnetized down to smaller scales than the hot ions and...Go to contribution page
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Prof. Quanming Lu (University of Science and Technology of China)11/08/2015, 14:50A large scale two-dimensional (2-D) particle-in-cell (PIC) simulation is performed in this paper to investigate electron acceleration in the dipolarization front (DF) region during magnetic reconnection. It is found that the DF is mainly driven by an ion outflow which also generates a positive potential region behind the DF. The DF propagates with an almost constant speed and...Go to contribution page
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Dr Philip Pritchett (University of California, Los Angeles)11/08/2015, 15:45Magnetic reconnection is widely accepted as the driver of dynamics in the Earth’s magnetotail despite the difficulty in understanding how reconnection can be initiated in a current sheet with curved magnetic field lines associated with a small normal B_z component. In particular, reconnection is the favored mechanism for explaining the generation of bursty bulk flows and...Go to contribution page
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Dr Yuri Khotyaintsev (Swedish Institute of Space Physics)11/08/2015, 16:10We use multi-spacecraft observations by Cluster and MMS in the magnetotail and 3D PIC simulations to investigate conversion of electromagnetic energy at the front of a fast plasma jet. Such plasma jet can be produced as a result of magnetic reconnection. Jet fronts are known to have a sharp increase of magnetic field (referred to as dipolarization fronts in the magnetospheric...Go to contribution page
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Dr Mikhail Sitnov (JHU/APL)11/08/2015, 16:25Magnetic reconnection in the Earth’s magnetotail has important features that distinguish it from similar processes in other space plasma regions, laboratory plasmas and in the simplest theoretical models. First, the very possibility of spontaneous reconnection has been questioned because of the stabilizing effect of electrons magnetized by the north-south (Bz) magnetic field...Go to contribution page
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Prof. Merav Opher (Boston University)12/08/2015, 09:00
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Dr Kenichi Nishikawa (Univerisyt of Alabama in Huntsville)12/08/2015, 09:30We investigated particle acceleration and shock structure associated with an unmagnetized relativistic jet propagating into an unmagnetized plasma. Strong magnetic fields generated in the trailing shock contribute to the electron’s transverse deflection and acceleration. Kinetic Kelvin- Helmholtz instability (kKHI) is also responsible to create strong DC and AC magnetic fields....Go to contribution page
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Prof. Nikolai Pogorelov (Department of Space Science, University of Alabama in Huntsville)12/08/2015, 09:55Recent simulations of the solar wind (SW) interaction with the local interstellar medium (LISM) performed by our team showed that the heliopause is the subject of various hydrodynamic instabilities which allow for an efficient, but spotty, mixing of the SW and LISM plasmas. The analysis of the coupling between the heliospheric and interstellar magnetic fields (HMF and ISMF) shows...Go to contribution page
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Dr Jiayong Zhong (Department of Astronomy, Beijing Normal University)12/08/2015, 11:10Laser driven magnetic reconnection (LDMR) is constructed with self- generated B fields has been experimentally and theoretically studied extensively, where more than Mega-Gauss strong B fields are spontaneously generated in high-power laser-plasma interactions, which located on the target surface and produced by non- parallel temperature and density gradients of expanding...Go to contribution page
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Prof. Axel Brandenburg (Nordita)12/08/2015, 11:35Using direct numerical simulations of three-dimensional hydromagnetic turbulence, either with helical or non-helical forcing, we show that the ratio of kinetic-to-magnetic energy dissipation always increases with the magnetic Prandtl number, i.e., the ratio of kinematic viscosity to magnetic diffusivity. This dependence can be approximated by a power law, but the exponent is not...Go to contribution page
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Prof. Igor Rogachevskii (Ben-Gurion University of the Negev and Nordita)12/08/2015, 12:00We study different regimes of magnetic reconnection during formation of bipolar structures using direct numerical simulations of the equations of magnetohydrodynamics with external random forcing and in the presence of gravity. The domain is divided into two parts: a lower layer with the helical forcing and an upper layer with the non-helical forcing with a smooth transition in...Go to contribution page
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Dr Li-Jen Chen (NASA Goddard Space Flight Center)12/08/2015, 14:00The electron diffusion region (EDR) holds the ultimate mystery of how magnetic reconnection can occur in a collisionless plasma, and is the target region of the first science priority for the newly launched Magnetospheric Multi-scale (MMS) mission. Processes of elctron acceleration, mixing and heating in the EDR can be understood by analyzing the electron distribution functions with...Go to contribution page
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Dr Rongsheng Wang (Institute of Geology and Geophysics, Chinese Academy of Sciences)12/08/2015, 14:25One long outstanding issue in the study of magnetic reconnection is exactly where and how electrons are energized, although the observations have demonstrated that a substantial part of magnetic energy is converted into energetic electrons in reconnection. Here, we present the first evidence of electron acceleration by parallel electric field (up to -20 mV/m) carried by the...Go to contribution page
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Dr Maria Elena Innocenti (University of Leuven, Belgium)12/08/2015, 14:50We describe here the first observation of switch-off of the in plane tangential component of the magnetic field in Particle In Cell (PIC) simulations of magnetic reconnection, a situation reminding of Petschek’s switch-off. Switch-off is obtained through a slow shock / rotational discontinuity compound structure. Two external slow shocks located in correspondence of the...Go to contribution page
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Paul Cassak (West Virginia University)12/08/2015, 15:45Magnetic reconnection at the dayside magnetopause is a crucial facet of solar wind-magnetospheric coupling, as it drives magnetospheric convection and is necessary for magnetic energy storage in the magnetotail. Many fundamental questions about dayside reconnection remain insufficiently answered quantitatively and even qualitatively, such as the location and local efficiency of...Go to contribution page
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Prof. Martin Goldman (University of Colorado at Boulder)12/08/2015, 16:10The primary goal of the current NASA-MMS mission is to "identify and study diffusion regions during magnetic reconnection in Earth's magnetopause and magnetotail. Yet the term diffusion region is often misunderstood and can be ambiguous. Different conditions for a region to be a "diffusion region" are interpreted theoretically, related to each other and applied to 2D PIC...Go to contribution page
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Prof. Joerg Buechner (Max-Planck-Institut fuer Sonnensystemforschung)13/08/2015, 09:00Magnetic reconnection is a multi-scale phenomenon which in collisionless plasmas involves electron and ion kinetic processes as well as macro-scale plasma flows. Only numerical simulation approaches allow to bridge the huge scale- gaps between the relevant particle and flow dynamics. We review the different approaches taken so far to cope with the arising difficulties and draw...Go to contribution page
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Prof. Masahiro Hoshino (The University of Tokyo)13/08/2015, 09:30Nonthermal particles are ubiquitous in space and astrophysical plasmas, and explosive phenomena such as supernova remnant shocks, solar flares, and terrestrial substroms have demonstrated evidence for the production of high-energy particles. Yet the particle acceleration mechanism remains an unresolved issue. After the innovative idea of the stochastic acceleration by Enrico...Go to contribution page
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Dr Antonella Greco (Physics Department, University of Calabria, Italy)13/08/2015, 10:15The intermittent properties of the turbulent field at different scales down towards electron scales have been studied using CLUSTER magnetic field data in solar wind. We found that turbulence, in some cases, orginizes itself in unidimensional current sheets well descibed by an Harris equilibrium on electron scales. These structures could be those structures that numerical...Go to contribution page
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Dr Nobumitsu Yokoi (Institute of Industrial Science, University of Tokyo)13/08/2015, 11:10Turbulence modeling provides a powerful tool for investigating realistic turbulence with large-scale inhomogeneities. An attempt to study fast reconnection with the aid of self-consistent turbulence model is introduced. Turbulence related to magnetic reconnection is not homogeneous-isotropic at all. Its statistical properties depend on the large-scale configurations of the...Go to contribution page
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Prof. Alexander Lazarian (University of Wisconsin, Madison, USA)13/08/2015, 11:35Turbulence is a natural state of high Reynolds flows and is ubiquitous in astrophysical systems. In most cases turbulence is externally driven, but one also expects the outflows induced by reconnection to get turbulent. High resolution numerical resolution reconnection simulations in 3D also show the transition to the turbulent state. Therefore it is essential to understand how...Go to contribution page
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Alexandros Chasapis (Laboratoire des Physiques des Plasmas)13/08/2015, 12:00We present an in situ study of thin current sheets and associated electron heating in turbulent space plasma. We use Cluster observations made in the turbulent plasma downstream of the Earth's quasi-parallel shock and we analyze the properties of ion-scale current sheets. Intermittent structures were identified using the Partial Variance of Increments method. We studied the...Go to contribution page
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Dr Laila Andersson (LASP)13/08/2015, 14:00How plasma stored in the Magnetotail is returned back to Earth has great implication of the Earth magnetosphere responds to changes in the solar wind. In the magnetotail both oxygen and protons are impacted by fast tail changes such as magnetic reconnection and cross tail oscillations. The Cluster mission observations of the magnetotail flows shows that at low speeds protons and oxygen...Go to contribution page
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Mr Magic Zazralt (Niels Bohr Institute)13/08/2015, 14:25Theoretical atmosphere models provide the basis for a variety of applications for astronomy. In one-dimensional (1D) atmosphere models, convection is usually treated with the mixing-length theory. However, this theory is by far not flawless and the superadiabatic regime is poorly rendered. Due to the increasing computational power, we are now capable to compute large grids of...Go to contribution page
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Ilja Honkonen (NASA/GSFC)13/08/2015, 14:50Due to its multi-scale nature, magnetic reconnection is difficult to model numerically using a full electromagnetic description of plasma in a system whose size is orders of magnitude larger than the smallest relevant spatial scales. In the context of Earth's magnetosphere reconnection has been modeled using a magnetohydrodynamic description of plasma for decades while kinetic...Go to contribution page
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Prof. Minna Palmroth (Finnish Meteorological Institute, Helsinki, Finland)13/08/2015, 15:45Vlasiator (http://vlasiator.fmi.fi) is a newly developed, global hybrid- Vlasov simulation, which solves the six-dimensional phase space utilising the Vlasov equation for protons, while electrons are treated as a charge-neutralising fluid. The outcome of the simulation is a global reproduction of ion-scale physics where the generation of physical features can be followed in time...Go to contribution page
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Dr Stefano Markidis (KTH)13/08/2015, 16:10We present the first 3D global simulation of Ganymede’s magnetosphere in a unified framework coupling the fluid and kinetic models. An MHD model describes the global interaction of solar wind with Ganymede’s magnetosphere over the whole simulation domain. A kinetic model is used only in the selected space regions, where kinetic effects dominate and MHD description fails. In...Go to contribution page
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Dr Stefan Eriksson (University of Colorado)14/08/2015, 09:00Hall currents generate a characteristic quadrupole out-of-plane magnetic field at a single X-line for a weak background guide-field and relatively symmetric conditions of plasma density and magnetic field strength across a reconnecting current sheet. This is observed as a bipolar perturbation of the out-of-plane magnetic field (BM) across the exhaust region as, e.g., reported...Go to contribution page
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Dr Vadim Roytershteyn14/08/2015, 09:30Recent simulations have revealed complex details of magnetic reconnection than on the first glance bring into question many established concepts in magnetic reconnection. As an example, it is not clear whether the concept of the diffusion region, a theoretical construct deeply ingrained into all things reconnection, can be usefully extended to 3D reconnection. At the same...Go to contribution page
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Prof. Viggo Hansteen (Institute of Theoretical Astrophysics, University of Oslo)14/08/2015, 10:15We have performed three-dimensional (3d) magnetohydrodynamic simulations of magnetic flux emergence in a model that spans the convection zone and into the outer solar atmosphere with the Bifrost code. This is a ``realistic'' model, in the sense that the parameters and physical effects that control the atmosphere can be used to produce diagnostics that can be directly compared...Go to contribution page
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Dr Daniel Kagan (Tel Aviv University)14/08/2015, 11:10We investigate the beaming of particles and the resulting synchrotron radiation in relativistic reconnection with background magnetizations of 4, 40, and 400 via 2D particle-in-cell simulations. First, we verify that the overall rate of energy conversion and the characteristics of radiation are similar at all magnetizations even for configurations including low-density background plasmas,...Go to contribution page
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Mr fabien widmer (Max-Planck-Institut für Sonnensystemforschung, Göttingen, Germany)14/08/2015, 11:35Magnetic reconnection is a very efficient process to convert magnetic energy into kinetic plasma energy. Unfortunately, models of reconnection such as Sweet Parker, do not agree with the time scale observed during the impulsive phase of a Solar flares, providing only small reconnection rates. One possible approach for reaching fast reconnection observed is by considering small...Go to contribution page
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Sanni Hoilijoki (Finnish Meteorological Institute)14/08/2015, 12:00The global hybrid-Vlasov simulation Vlasiator (http://vlasiator.fmi.fi), developed at the Finnish Meteorological Institute, describes ions as velocity distributions functions propagated by solving the Vlasov equation and treats electrons as charge-neutralizing fluid. We present results from a new 5- dimensional simulation describing the Earth's magnetosphere in two dimensions in...Go to contribution page
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Dr Gian Luca Delzanno (Los Alamos National Laboratory)14/08/2015, 14:00The Vlasov-Maxwell equations are a fundamental model for the microscopic evolution of magnetized, collisionless plasmas. Because of the wide disparity of spatial and temporal scales typical of plasmas, their numerical solution is extremely challenging and is a very active area of research. There are three main numerical approaches to the solution of the...Go to contribution page
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Yann Pfau-Kempf (Finnish Meteorological Institute, Helsinki, Finland)14/08/2015, 14:25The Finnish Meteorological Institute's hybrid-Vlasov model Vlasiator (http://vlasiator.fmi.fi), which couples kinetic ion physics through Vlasov's equation with charge-neutralising fluid electrons, is used to model self-consistently the solar wind-magnetosphere interaction in two spatial and three velocity dimensions. Recent simulations in the polar plane include southward IMF in...Go to contribution page
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Mr Rishi Mistry (Imperial College London)14/08/2015, 14:50Magnetic reconnection at the magnetopause and magnetotail affect many magnetospheric dynamics including the onset of magnetospheric sub-storms and space weather effects, and the balance of energy in the magnetosphere. In these environments, however, asymmetric boundary conditions and imprecise knowledge of the motion of reconnection exhausts relative to spacecraft affect the...Go to contribution page
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Dr Jane Pratt (University of Exeter Astrophysics)14/08/2015, 15:45When a fusion plasma is above a critical value of beta, neoclassical tearing modes are destabilized. The resulting magnetic islands can grow to large size, allowing fast escape of the plasma from the fusion machine. The primary tactic for preventing tearing modes and reducing the size of magnetic islands in fusion machines is to apply current inside the magnetic islands. In...Go to contribution page
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Dr nicolas aunai (CNRS/LPP)14/08/2015, 16:10Collisionless magnetic reconnection is enabled by electron scale mechanisms and its dynamic is mainly controlled by ion scale processes. Whenever the to plasmas on both sides of the current sheet have different properties, a lot of well-known processes and their associated signatures are vastly changed. In this presentation, I will explain how one can highlight the regions of...Go to contribution page
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14/08/2015, 16:35
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Ms Elisabet Liljeblad (Space and Plasma Physics, The Royal Institute of Technology, KTH, Stockholm)Workshop, August 10-14PosterThe low-latitude boundary layer is a region where a constant transfer of mass and energy takes place. The layer has been studied extensively on Earth, but so far no comprehensive study on the layer on Mercury exists. This study aims for a systematic analysis on Mercury magnetopause crossings during year 2011 to identify and analyse the LLBL and its properties, including thickness,...Go to contribution page
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Dr Daniel Kagan (Tel Aviv University)Workshop, August 10-14PosterWe investigate the acceleration of particles beyond the synchrotron burnoff limit of the background magnetic field in relativistic magnetic reconnection by analysing the effects of radiative cooling on test particles incident on a large reconnection region in a 2D particle-in-cell simulation. We find that the trajectories of the particles are not significantly affected by cooling while...Go to contribution page
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Mr Jeremy Dargent (CNRS/LPP/IRAP)Workshop, August 10-14PosterTangential current layers are ubiquitous in the Universe.They appear in magnetized collisionless plasmas as a result of the Frozen-in law and the conservation of field line connectivity. However, there are few steady kinetic descriptions of them and most of these describe symmetric layers. The BAS model (Belmont et al. 20132) is a semi- analytical model which provides a steady ion...Go to contribution page
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Dr Alessandro Retinò (Laboratoire de Physique des Plasmas, Palaiseau, France)Workshop, August 10-14InvitedThe microphysics of magnetic reconnection (i.e. the physics at proton scales and below) is one of the most important aspects of reconnection and the target of the recently launched NASA/MMS mission. Among different open issues related to the microphysics, understanding the mechanisms of particle heating and acceleration is one of the most important. The Earth’s magnetopause is an...Go to contribution page
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Dr Mikhail Belyaev (Theoretical Astrophysics Center UC Berkeley Astronomy Department)Workshop, August 10-14OralWe perform 2.5D axisymmetric simulations of the pulsar magnetosphere (aligned dipole rotator) using the charge conservative, relativistic, electromagnetic particle in cell code PICsar. Particle in cell codes are a powerful tool to use for studying the pulsar magnetosphere, because they can handle the force- free and vacuum limits and provide a self-consistent treatment of...Go to contribution page
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Dr YongCun Zhang (State Key Laboratory of Space Weather, Center for Space Science and Applied Research,Chinese Academy of Sciences)Workshop, August 10-14PosterWe report first results of magnetic curvature distribution in the diffusion region of a unique magnetic reconnection event. This event is exceptional since all four Cluster spacecraft is crossing the diffusion region. Magnetic curvature analysis shows that magnetic field lines are sharply curved with high curvature in the inner outflow regions between the two Hall regions and display...Go to contribution page
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John Dorelli (NASA-GSFC)Workshop, August 10-14InvitedRecent high resolution global magnetohydrodynamics (MHD) simulations of Earth's magnetosphere [Komar et al., 2013, Glocer et al., 2015] suggest that dayside magnetopause reconnection occurs at topological separators that extend across the entire dayside -- stretching from one polar cusp to the other -- for both northward and southward Interplanetary Magnetic Field (IMF) conditions....Go to contribution page
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Mr Xuehan Guo (The University of Tokyo)Workshop, August 10-14PosterMagnetic reconnection plays a fundamental role in magnetized plasmas because it permits magnetic configurations to changes the magnetic field line topology releasing magnetic stress and energy. Localized electron heating of magnetic reconnection was studied under strong guide- field using two merging spherical tokamak plasmas in Univ. Tokyo Spherical Tokamak (UTST) experiment. Our new...Go to contribution page
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Mr Chris Elenbaas (University of Amsterdam)Workshop, August 10-14PosterTransient giant gamma-ray flares comprise the most extreme radiation events to have been observed from magnetars. Developing on (sub)millisecond timescales and expelling vast amounts of energy within a mere fraction of a second, the initial phase of these extraordinary bursts present a significant challenge for candidate trigger mechanisms. Here we revise and critically analyse the...Go to contribution page
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Dr Huishan Fu (Beihang University)Workshop, August 10-14PosterA magnetic reconnection event detected by Cluster is analyzed using three methods: single-spacecraft inference, multi-spacecraft timing, and the first-order Taylor expansion (FOTE). Using single-spacecraft method, we find that the structure is a reconnection X-line; while using timing and FOTE analyses, we find it is a magnetic island (O-line). We conclude that the best and fast way to...Go to contribution page
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Dr Shiyong Huang (Laboratoire de Physique des Plasmas, CNRS-Ecole Polytechnique-UPMC, Palaiseau, France)Workshop, August 10-14PosterMagnetic reconnection is a fundamental physical process that enables the rapid transfer of magnetic energy into plasma kinetic and thermal energy in the laboratory, astrophysical and space plasma. Flux ropes have been suggested to play important role in controlling the micro-scale physics of magnetic reconnection and electron acceleration. In this presentation, we report the...Go to contribution page
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Dr Yi-Hsin Liu (NASA-GSFC)Workshop, August 10-14OralAt Earth's magnetopause, reconnection proceeds asymmetrically between magnetosheath plasmas, namely solar wind plasmas compressed by Earth's bow shock, and magnetospheric plasmas. In an asymmetric configuration, it is unclear if there is a simple principle to determine the orientation of the x-line. Using fully kinetic simulations, we study this issue and a spatially localized...Go to contribution page
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Mr Bart Ripperda (KU Leuven)Workshop, August 10-14PosterParticle acceleration due to interacting tilt and kink instabilities in repelling current channels B. Ripperda, R. Keppens Centre for mathematical Plasma-Astrophysics, Department of Mathematics, KU Leuven We present a numerical study where we use a combination of resistive magnetohydrodynamic (MHD) and test-particle methods to analyze particle acceleration in two repelling current...Go to contribution page
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Prof. Nagendra Singh (University of Alabama in Huntsville)Workshop, August 10-14OralWe study the evolution of an electron current layer (ECL) through its several stages by means of three-dimensional particle-in-cell (PIC) simulations with ion to electron mass ratio M/me =400. An ECL evolves through the following stages: (i) Electrostatic (ES) current-driven instability (CDI) soon after its formation with half width w about 2 electron skin depth (de), (ii)...Go to contribution page
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Prof. Mats André (Swedish Institute of Space Physics, Uppsala)Workshop, August 10-14PosterMagnetospheric ions with energies less than tens of eV originate from the ionosphere. The low energy indicates the origin of the plasma but also severely complicates detection of the positive ions onboard sunlit spacecraft at higher altitudes, which often become positively charged to several tens of volts. We discuss some methods to observe low-energy ions, including a recently...Go to contribution page
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Mr Boris Gudiksen (Inst for theoretical astrophysics, University of Oslo)Workshop, August 10-14PosterThe solar atmosphere shows signs of almost continuous reconnection events happening, producing energy releases over a large range in energy. The reconnection events are fast, efficient but so far not explained in detail. We observe the effects of reconnection both in low and high plasma beta environments. Observational data on accelerated particles, radiation in a wide range of...Go to contribution page
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Dr Suleiman Baraka (Al Aqsa University, Gaza Palestine. + IAP-UPMC, Paris, France)Workshop, August 10-14PosterWe apply three IMF orientations along with an artificial depression in the solar dynamic pressure to study their impacts on the cusp dynamics and orientation. PIC EM Relativistic code was used to investigate the problem in hand. Particles and fields updates are carefully studied at both northern and southern cusps. The size, position and shape of the both cusps under the said conditions...Go to contribution page
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Dr A. Vaivads (Swedish Institute of Space Physics, Uppsala)Workshop, August 10-14PosterThe acceleration of energetic electrons inside magnetic pile-up regions of plasma jets in the Earth magnetotail is studied in details for one case observed by Cluster. The case has been selected based on high observed fluxes of electrons, Cluster being in the burst mode and Cluster separation being around 1000 km that is optimal for studies of ion scale physics. We show that...Go to contribution page
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Dr Maria Elena Innocenti (Center for mathematical Plasma Astrophysics, Department of Mathematics, K.U. Leuven (University of Leuven), Celestijnenlaan 200B, B-3001 Leuven, Belgium)Workshop, August 10-14PosterMagnetic reconnection is an intrinsically multi-scale phenomenon. At least at a first approximation, it is possible to pinpoint areas where processes occur at different spatial and temporal scales, such as the inflow region, the Ion Diffusion Region and the Electron Diffusion Region (EDR). This can be used to lower the computational cost of Particle In Cell, realistic mass ratio...Go to contribution page
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