5,102 research outputs found
The Madison plasma dynamo experiment: a facility for studying laboratory plasma astrophysics
The Madison plasma dynamo experiment (MPDX) is a novel, versatile, basic
plasma research device designed to investigate flow driven magnetohydrodynamic
(MHD) instabilities and other high- phenomena with astrophysically
relevant parameters. A 3 m diameter vacuum vessel is lined with 36 rings of
alternately oriented 4000 G samarium cobalt magnets which create an
axisymmetric multicusp that contains 14 m of nearly magnetic field
free plasma that is well confined and highly ionized . At present, 8
lanthanum hexaboride (LaB) cathodes and 10 molybdenum anodes are inserted
into the vessel and biased up to 500 V, drawing 40 A each cathode, ionizing a
low pressure Ar or He fill gas and heating it. Up to 100 kW of electron
cyclotron heating (ECH) power is planned for additional electron heating. The
LaB cathodes are positioned in the magnetized edge to drive toroidal
rotation through torques that propagate into the
unmagnetized core plasma. Dynamo studies on MPDX require a high magnetic
Reynolds number , and an adjustable fluid Reynolds number , in the regime where the kinetic energy of the flow exceeds the magnetic
energy (vv). Initial results from MPDX are presented
along with a 0-dimensional power and particle balance model to predict the
viscosity and resistivity to achieve dynamo action.Comment: 14 pages, 13 figure
Efficient solution of 3D electromagnetic eddy-current problems within the finite volume framework of OpenFOAM
Eddy-current problems occur in a wide range of industrial and metallurgical
applications where conducting material is processed inductively. Motivated by
realising coupled multi-physics simulations, we present a new method for the
solution of such problems in the finite volume framework of foam-extend, an
extended version of the very popular OpenFOAM software. The numerical procedure
involves a semi-coupled multi-mesh approach to solve Maxwell's equations for
non-magnetic materials by means of the Coulomb gauged magnetic vector potential
and the electric scalar potential. The concept is further extended on the basis
of the impressed and reduced magnetic vector potential and its usage in
accordance with Biot-Savart's law to achieve a very efficient overall modelling
even for complex three-dimensional geometries. Moreover, we present a special
discretisation scheme to account for possible discontinuities in the electrical
conductivity. To complement our numerical method, an extensive validation is
completing the paper, which provides insight into the behaviour and the
potential of our approach.Comment: 47 pages, improved figures, updated references, fixed typos, reverse
phase shift, consistent use of inner produc
GMC Collisions As Triggers of Star Formation. IV. The Role of Ambipolar Diffusion
We investigate the role of ambipolar diffusion (AD) in collisions between
magnetized giant molecular clouds (GMCs), which may be an important mechanism
for triggering star cluster formation. Three dimensional simulations of GMC
collisions are performed using a version of the Enzo magnetohydrodynamics code
that has been extended to include AD. The resistivities are calculated using
the 31-species chemical model of Wu et al. (2015). We find that in the
weak-field, case, AD has only a modest effect on the
dynamical evolution during the collision. However, for the stronger-field,
case involving near-critical clouds, AD results in formation
of dense cores in regions where collapse is otherwise inhibited. The overall
efficiency of formation of cores with in
these simulations is increases from about 0.2% to 2% once AD is included,
comparable to observed values in star-forming GMCs. The gas around these cores
typically has relatively slow infall at speeds that are a modest fraction of
the free-fall speed.Comment: 15 pages, 15 figures, Accepted to Ap
GMC Collisions As Triggers of Star Formation. IV. The Role of Ambipolar Diffusion
We investigate the role of ambipolar diffusion (AD) in collisions between
magnetized giant molecular clouds (GMCs), which may be an important mechanism
for triggering star cluster formation. Three dimensional simulations of GMC
collisions are performed using a version of the Enzo magnetohydrodynamics code
that has been extended to include AD. The resistivities are calculated using
the 31-species chemical model of Wu et al. (2015). We find that in the
weak-field, case, AD has only a modest effect on the
dynamical evolution during the collision. However, for the stronger-field,
case involving near-critical clouds, AD results in formation
of dense cores in regions where collapse is otherwise inhibited. The overall
efficiency of formation of cores with in
these simulations is increases from about 0.2% to 2% once AD is included,
comparable to observed values in star-forming GMCs. The gas around these cores
typically has relatively slow infall at speeds that are a modest fraction of
the free-fall speed.Comment: 15 pages, 15 figures, Accepted to Ap
Collisionless Magnetic Reconnection in Space Plasmas
Magnetic reconnection requires the violation of the frozen-in condition which
ties gyrating charged particles to the magnetic field inhibiting diffusion.
Ongoing reconnection has been identified in near-Earth space as being
responsible for the excitation of substorms, magnetic storms, generation of
field aligned currents and their consequences, the wealth of auroral phenomena.
Its theoretical understanding is now on the verge of being completed.
Reconnection takes place in thin current sheets. Analytical concepts proceeded
gradually down to the microscopic scale, the scale of the electron skin depth
or inertial length, recognizing that current layers that thin do preferentially
undergo spontaneous reconnection. Thick current layers start reconnecting when
being forced by plasma inflow to thin. For almost half a century the physical
mechanism of reconnection has remained a mystery. Spacecraft in situ
observations in combination with sophisticated numerical simulations in two and
three dimensions recently clarified the mist, finding that reconnection
produces a specific structure of the current layer inside the electron inertial
(also called electron diffusion) region around the reconnection site, the X
line. Onset of reconnection is attributed to pseudo-viscous contributions of
the electron pressure tensor aided by electron inertia and drag, creating a
complicated structured electron current sheet, electric fields, and an electron
exhaust extended along the current layer. We review the general background
theory and recent developments in numerical simulation on collisionless
reconnection. It is impossible to cover the entire field of reconnection in a
short space-limited review. The presentation necessarily remains cursory,
determined by our taste, preferences, and knowledge. Only a small amount of
observations is included in order to support the few selected numerical
simulations.Comment: Review pape
Magnetic field, temperature and velocity distribution measurements in an electromagnetic induction pump using a small ferrite core coil system
International audienceIn this paper technique of local AC magnetic field, temperature and velocity measurements in the gap between electromagnetic induction pump (EMIP) channel and inductor using a single ferrite core coil is discussed. Described method has several important advantages: high signal/noise ratio due to ferrite core, small size of a sensor, three parameter measurement, non-intrusiveness, low cost etc. However, some significant limitations should be also considered: saturation of ferrite core with relatively low fields and temperature dependence on magnetic permeability characteristic of ferrite material. Finally, this perspective measurement method was tested in University of Latvia (UL) and implemented in measurement system of TESLA-EMP loop in Institute of Physics of University of Latvia (IPUL). Some relevant results of these experiments are presented
- …