114 research outputs found
Uniqueness of the compactly supported weak solutions of the relativistic Vlasov-Darwin system
We use optimal transportation techniques to show uniqueness of the compactly
supported weak solutions of the relativistic Vlasov-Darwin system. Our proof
extends the method used by Loeper in J. Math. Pures Appl. 86, 68-79 (2006) to
obtain uniqueness results for the Vlasov-Poisson system.Comment: AMS-LaTeX, 21 page
Emission heights of coronal bright points on Fe XII radiance map
We study the emission heights of the coronal bright points (BPs) above the
photosphere in the bipolar magnetic loops that are apparently associated with
them. As BPs are seen in projection against the disk their true emission
heights are unknown. The correlation of the BP locations on the Fe XII radiance
map from EIT with the magnetic field features (in particular neutral lines) was
investigated in detail. The coronal magnetic field was determined by an
extrapolation of the photospheric field to different altitudes above the disk.
It was found that most BPs sit on or near a photospheric neutral line, but that
the emission occurs at a height of about 5 Mm. Some BPs, while being seen in
projection, still seem to coincide with neutral lines, although their emission
takes place at heights of more than 10 Mm. Such coincidences almost disappear
for emissions above 20 Mm. We also projected the upper segments of the 3-D
magnetic field lines above different heights, respectively, on to the x-y
plane. The shape of each BP was compared with the respective field-line segment
nearby. This comparison suggests that most coronal BPs are actually located on
the top of their associated magnetic loops. Finally, we calculated for each
selected BP region the correlation coefficient between the Fe XII intensity
enhancement and the horizontal component of the extrapolated magnetic field
vector at the same x-y position in planes of different heights, respectively.
We found that for almost all the BP regions we studied the correlation
coefficient, with increasing height, increases to a maximal value and then
decreases again. The height corresponding to this maximum was defined as the
correlation height, which for most bright points was found to range below 20
Mm.Comment: 7 pages, 4 figures, 1 tabl
Segmentation of Loops from Coronal EUV Images
We present a procedure which extracts bright loop features from solar EUV
images. In terms of image intensities, these features are elongated ridge-like
intensity maxima. To discriminate the maxima, we need information about the
spatial derivatives of the image intensity. Commonly, the derivative estimates
are strongly affected by image noise. We therefore use a regularized estimation
of the derivative which is then used to interpolate a discrete vector field of
ridge points ``ridgels'' which are positioned on the ridge center and have the
intrinsic orientation of the local ridge direction. A scheme is proposed to
connect ridgels to smooth, spline-represented curves which fit the observed
loops. Finally, a half-automated user interface allows one to merge or split,
eliminate or select loop fits obtained form the above procedure. In this paper
we apply our tool to one of the first EUV images observed by the SECCHI
instrument onboard the recently launched STEREO spacecraft. We compare the
extracted loops with projected field lines computed from
almost-simultaneously-taken magnetograms measured by the SOHO/MDI Doppler
imager. The field lines were calculated using a linear force-free field model.
This comparison allows one to verify faint and spurious loop connections
produced by our segmentation tool and it also helps to prove the quality of the
magnetic-field model where well-identified loop structures comply with
field-line projections. We also discuss further potential applications of our
tool such as loop oscillations and stereoscopy.Comment: 13 pages, 9 figures, Solar Physics, online firs
Flat galaxies with dark matter halos - existence and stability
We consider a model for a flat, disk-like galaxy surrounded by a halo of dark
matter, namely a Vlasov-Poisson type system with two particle species, the
stars which are restricted to the galactic plane and the dark matter particles.
These constituents interact only through the gravitational potential which
stars and dark matter create collectively. Using a variational approach we
prove the existence of steady state solutions and their nonlinear stability
under suitably restricted perturbations.Comment: 39 page
Evolution of turbulent spots in a parallel shear flow
The evolution of turbulent spots in a parallel shear flow is studied by means
of full three-dimensional numerical simulations. The flow is bounded by free
surfaces and driven by a volume force. Three regions in the spanwise spot
cross-section can be identified: a turbulent interior, an interface layer with
prominent streamwise streaks and vortices and a laminar exterior region with a
large scale flow induced by the presence of the spot. The lift-up of streamwise
streaks which is caused by non-normal amplification is clearly detected in the
region adjacent to the spot interface. The spot can be characterized by an
exponentially decaying front that moves with a speed different from that of the
cross-stream outflow or the spanwise phase velocity of the streamwise roll
pattern. Growth of the spots seems to be intimately connected to the large
scale outside flow, for a turbulent ribbon extending across the box in
downstream direction does not show the large scale flow and does not grow.
Quantitatively, the large scale flow induces a linear instability in the
neighborhood of the spot, but the associated front velocity is too small to
explain the spot spreading.Comment: 10 pages, 10 Postscript figure
How to use magnetic field information for coronal loop identification?
The structure of the solar corona is dominated by the magnetic field because
the magnetic pressure is about four orders of magnitude higher than the plasma
pressure. Due to the high conductivity the emitting coronal plasma (visible
e.g. in SOHO/EIT) outlines the magnetic field lines. The gradient of the
emitting plasma structures is significantly lower parallel to the magnetic
field lines than in the perpendicular direction. Consequently information
regarding the coronal magnetic field can be used for the interpretation of
coronal plasma structures. We extrapolate the coronal magnetic field from
photospheric magnetic field measurements into the corona. The extrapolation
method depends on assumptions regarding coronal currents, e.g. potential fields
(current free) or force-free fields (current parallel to magnetic field). As a
next step we project the reconstructed 3D magnetic field lines on an EIT-image
and compare with the emitting plasma structures. Coronal loops are identified
as closed magnetic field lines with a high emissivity in EIT and a small
gradient of the emissivity along the magnetic field.Comment: 14 pages, 3 figure
A novel type of intermittency in a nonlinear dynamo in a compressible flow
The transition to intermittent mean--field dynamos is studied using numerical
simulations of isotropic magnetohydrodynamic turbulence driven by a helical
flow. The low-Prandtl number regime is investigated by keeping the kinematic
viscosity fixed while the magnetic diffusivity is varied. Just below the
critical parameter value for the onset of dynamo action, a transient
mean--field with low magnetic energy is observed. After the transition to a
sustained dynamo, the system is shown to evolve through different types of
intermittency until a large--scale coherent field with small--scale turbulent
fluctuations is formed. Prior to this coherent field stage, a new type of
intermittency is detected, where the magnetic field randomly alternates between
phases of coherent and incoherent large--scale spatial structures. The
relevance of these findings to the understanding of the physics of mean--field
dynamo and the physical mechanisms behind intermittent behavior observed in
stellar magnetic field variability are discussed.Comment: 19 pages, 13 figure
Signature of mass supply to quiet coronal loops
Aims. The physical implication of large blue shift of Ne viii in the quiet
Sun region is investigated in this paper. Methods. We compare the significant
Ne viii blue shifts, which are visible as large blue patches on the
Doppler-shift map of a middlelatitude quiet-Sun region observed by SUMER, with
the coronal magnetic-field structures as reconstructed from a simultaneous
photospheric magnetogram by means of a force-free-field extrapolation. Results.
We show for the first time that coronal funnels also exist in the quiet Sun.
The region studied contains several small funnels that originate from network
lanes, expand with height and finally merge into a single wide open-field
region. However, the large blue shifts of the Ne viii line are not generally
associated with funnels. A comparison between the projections of coronal loops
onto the solar x-y-plane and the Ne viii dopplergram indicates that there are
some loops that reveal large Ne viii blue shifts in both legs, and some loops
with upflow in one and downflow in the other leg. Conclusions. Our results
suggest that strong plasma outflow, which can be traced by large Ne viii blue
shift, is not necessarily associated with the solar wind originating in coronal
funnels but appears to be a signature of mass supply to coronal loops. Under
the assumption that the measured Doppler shift of the Ne viii line represents
the real outflow velocity of the neon ions being markers of the proton flow, we
estimate the mass supply rate to coronal loops to be about 10\^{34} s\^{-1}.Comment: 5 pages, 4 figure
Turbulence and passive scalar transport in a free-slip surface
We consider the two-dimensional (2D) flow in a flat free-slip surface that
bounds a three-dimensional (3D) volume in which the flow is turbulent. The
equations of motion for the two-dimensional flow in the surface are neither
compressible nor incompressible but strongly influenced by the 3D flow
underneath the surface. The velocity correlation functions in the 2D surface
and in the 3D volume scale with the same exponents. In the viscous subrange the
amplitudes are the same, but in the inertial subrange the 2D one is reduced to
2/3 of the 3D amplitude. The surface flow is more strongly intermittent than
the 3D volume flow. Geometric scaling theory is used to derive a relation
between the scaling of the velocity field and the density fluctuations of a
passive scalar advected on the surface.Comment: 11 pages, 10 Postscript figure
Neurodegeneration and Epilepsy in a Zebrafish Model of CLN3 Disease (Batten Disease)
The neuronal ceroid lipofuscinoses are a group of lysosomal storage disorders that comprise the most common, genetically heterogeneous, fatal neurodegenerative disorders of children. They are characterised by childhood onset, visual failure, epileptic seizures, psychomotor retardation and dementia. CLN3 disease, also known as Batten disease, is caused by autosomal recessive mutations in the CLN3 gene, 80–85% of which are a ~1 kb deletion. Currently no treatments exist, and after much suffering, the disease inevitably results in premature death. The aim of this study was to generate a zebrafish model of CLN3 disease using antisense morpholino injection, and characterise the pathological and functional consequences of Cln3 deficiency, thereby providing a tool for future drug discovery. The model was shown to faithfully recapitulate the pathological signs of CLN3 disease, including reduced survival, neuronal loss, retinopathy, axonopathy, loss of motor function, lysosomal storage of subunit c of mitochondrial ATP synthase, and epileptic seizures, albeit with an earlier onset and faster progression than the human disease. Our study provides proof of principle that the advantages of the zebrafish over other model systems can be utilised to further our understanding of the pathogenesis of CLN3 disease and accelerate drug discovery
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