60 research outputs found
Crescent-shaped electron velocity distribution functions formed at the edges of plasma jets interacting with a tangential discontinuity
In this paper we discuss numerical simulations that illustrate a physical
mechanism leading to the formation of crescent-shaped electron velocity
distribution functions at the edges of a high-speed plasma jet impacting on a
thin, steep and impenetrable tangential discontinuity with no magnetic shear.
We use three-dimensional particle-in-cell simulations to compute the velocity
distribution function of electrons in different areas of the plasma jet and
at different phases of the interaction with the discontinuity. The simulation
set-up corresponds to an idealized, yet relevant, magnetic configuration
likely to be observed at the frontside magnetopause under the northward
interplanetary magnetic field. The combined effect of the gradient-B drift
and the remote sensing of large Larmor radius electrons leads to the
formation of crescent-shaped electron velocity distribution functions. We
provide examples of such distributions measured by a virtual satellite
launched into the simulation domain.</p
Turbulence-generated proton-scale structures in the terrestrial magnetosheath
Recent results of numerical magnetohydrodynamic simulations suggest that in
collisionless space plasmas turbulence can spontaneously generate thin current
sheets. These coherent structures can partially explain intermittency and the
non-homogenous distribution of localized plasma heating in turbulence. In this
Letter Cluster multi-point observations are used to investigate the
distribution of magnetic field discontinuities and the associated small-scale
current sheets in the terrestrial magnetosheath downstream of a quasi-parallel
bow shock. It is shown experimentally, for the first time, that the strongest
turbulence generated current sheets occupy the long tails of probability
distribution functions (PDFs) associated with extremal values of magnetic field
partial derivatives. During the analyzed one hour long time interval, about a
hundred strong discontinuities, possibly proton-scale current sheets were
observed.Comment: 10 pages, 5 figures in The Astrophysical Journal Letters, Volume 819,
Number 1, 201
Sheared magnetospheric plasma flows and discrete auroral arcs: a quasi-static coupling model
We consider sheared flows in magnetospheric boundary layers of tangential discontinuity type, forming a structure that is embedded in a large-scale convergent perpendicular electric field. We construct a kinetic model that couples the magnetospheric structure with the topside ionosphere. The contribution of magnetospheric electrons and ionospheric electrons and ions is taken into account into the current-voltage relationship derived for an electric potential monotonically decreasing with the altitude. The solution of the current continuity equation gives the distribution of the ionospheric potential consistent with the given magnetospheric electric potential. The model shows that a sheared magnetospheric flow generates current sheets corresponding to upward field-aligned currents, field-aligned potential drops and narrow bands of precipitating energy, as in discrete auroral arcs. Higher velocity magnetospheric sheared flows have the tendency to produce brighter and slightly broader arcs. An increase in arc luminosity is also associated with enhancements of magnetospheric plasma density, in which case the structures are narrower. Finally, the model predicts that an increase of the electron temperature of the magnetospheric flowing plasma corresponds to slightly wider arcs but does not modify their luminosity
Multi-point observations of intermittency in the cusp regions
International audienceIn this paper we investigate the statistical properties of magnetic field fluctuations measured by the four Cluster spacecraft in the cusp and close to the interface with the magnetospheric lobes, magnetopause and magnetosheath. At lower altitudes along the outbound orbit of 26 February 2001, the magnetic field fluctuations recorded by all four spacecraft are random and their Probability Distribution Functions (PDFs) are Gaussian at all scales. The flatness parameter, F ? related to the kurtosis of the time series, is equal to 3. At higher altitudes, in the cusp and its vicinity, closer to the interface with the magnetopause and magnetosheath, the PDFs from all Cluster satellites are non-Gaussian and show a clear intermittent behavior at scales smaller than ?G? 61 s (or 170 km). The flatness parameter increases to values greater than 3 for scales smaller than ?G. A Haar wavelet transform enables the identification of the "events" that produce sudden variations of the magnetic field and of the scales that have most of the power. The LIM parameter (i.e. normalized wavelet power) indicates that events for scales below 65 s are non-uniformly distributed throughout the cusp passage. PDFs, flatness and wavelet analysis show that at coarse-grained scales larger than ?G the intermittency is absent in the cusp. Fluctuations of the magnetic energy observed during the same orbit in the magnetosheath show PDFs that tend toward a Gaussian at scales smaller than ?G found in the cusp. The flatness analysis confirms the decreasing of ?G from cusp to magnetosheath. Our analysis reveals the turbulent cusp as a transition region from a non-intermittent turbulent state inside the magnetosphere to an intermittent turbulent state in the magnetosheath that has statistical properties resembling the solar wind turbulence. The observed turbulent fluctuations in the cusp suggests a phenomenon of nonlinear interactions of plasma coherent structures as in contemporary models of space plasma turbulence
Polar cap arcs from the magnetosphere to the ionosphere: kinetic modelling and observations by Cluster and TIMED
On 1 April 2004 the GUVI imager onboard the TIMED spacecraft spots an
isolated and elongated polar cap arc. About 20 min later, the Cluster
satellites detect an isolated upflowing ion beam above the polar cap.
Cluster observations show that the ions are accelerated upward by a
quasi-stationary electric field. The field-aligned potential drop is
estimated to about 700 V and the upflowing ions are accompanied by a tenuous
population of isotropic protons with a temperature of about 500 eV.
<br><br>
The magnetic footpoints of the ion outflows observed by Cluster are situated
in the prolongation of the polar cap arc observed by TIMED GUVI. The
upflowing ion beam and the polar cap arc may be different signatures of the
same phenomenon, as suggested by a recent statistical study of polar cap ion
beams using Cluster data.
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We use Cluster observations at high altitude as input to a quasi-stationary
magnetosphere-ionosphere (MI) coupling model. Using a Knight-type
current-voltage relationship and the current continuity at the topside
ionosphere, the model computes the energy spectrum of precipitating
electrons at the top of the ionosphere corresponding to the generator
electric field observed by Cluster. The MI coupling model provides a
field-aligned potential drop in agreement with Cluster observations of
upflowing ions and a spatial scale of the polar cap arc consistent with the
optical observations by TIMED. The computed energy spectrum of the
precipitating electrons is used as input to the Trans4 ionospheric transport
code. This 1-D model, based on Boltzmann's kinetic formalism, takes into
account ionospheric processes such as photoionization and electron/proton
precipitation, and computes the optical and UV emissions due to
precipitating electrons. The emission rates provided by the Trans4 code are
compared to the optical observations by TIMED. They are similar in size and
intensity. Data and modelling results are consistent with the scenario of
quasi-static acceleration of electrons that generate a polar cap arc as they
precipitate in the ionosphere. The detailed observations of the acceleration
region by Cluster and the large scale image of the polar cap arc provided by
TIMED are two different features of the same phenomenon. Combined together,
they bring new light on the configuration of the high-latitude magnetosphere
during prolonged periods of Northward IMF. Possible implications of the
modelling results for optical observations of polar cap arcs are also
discussed
Evolution of Intermittency in the Slow and Fast Solar Wind beyond the Ecliptic Plane
We study intermittency as a departure from self-similarity of the solar wind magnetic turbulence and investigate the evolution with the heliocentric distance and latitude. We use data from the Ulysses spacecraft measured during two solar minima (1997-1998 and 2007-2008) and one solar maximum (1999-2001). In particular, by modeling a multifractal spectrum, we revealed the intermittent character of turbulence in the small-scale fluctuations of the magnetic field embedded in the slow and fast solar wind. Generally, at small distances from the Sun, in both the slow and fast solar wind, we observe the high degree of multifractality (intermittency) that decreases somewhat slowly with distance and slowly with latitude. The obtained results seem to suggest that generally intermittency in the solar wind has a solar origin. However, the fast and slow streams, shocks, and other nonlinear interactions can only be considered as the drivers of the intermittent turbulence. It seems that analysis shows that turbulence beyond the ecliptic plane evolves too slowly to maintain the intermittency with the distance and latitude. Moreover, we confirm that the multifractality and intermittency are at a lower level than in the ecliptic, as well as the existence of symmetry with respect to the ecliptic plane, suggesting that there are similar turbulent properties observed in the two hemispheres
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