2,026 research outputs found
Fast reconnection in relativistic plasmas: the magnetohydrodynamics tearing instability revisited
Fast reconnection operating in magnetically dominated plasmas is often
invoked in models for magnetar giant flares, for magnetic dissipation in pulsar
winds, or to explain the gamma-ray flares observed in the Crab nebula, hence
its investigation is of paramount importance in high-energy astrophysics. Here
we study, by means of two dimensional numerical simulations, the linear phase
and the subsequent nonlinear evolution of the tearing instability within the
framework of relativistic resistive magnetohydrodynamics, as appropriate in
situations where the Alfven velocity approaches the speed of light. It is found
that the linear phase of the instability closely matches the analysis in
classical MHD, where the growth rate scales with the Lundquist number S as
S^-1/2, with the only exception of an enhanced inertial term due to the thermal
and magnetic energy contributions. In addition, when thin current sheets of
inverse aspect ratio scaling as S^-1/3 are considered, the so-called "ideal"
tearing regime is retrieved, with modes growing independently on S and
extremely fast, on only a few light crossing times of the sheet length. The
overall growth of fluctuations is seen to solely depend on the value of the
background Alfven velocity. In the fully nonlinear stage we observe an inverse
cascade towards the fundamental mode, with Petschek-type supersonic jets
propagating at the external Alfven speed from the X-point, and a fast
reconnection rate at the predicted value R~(ln S)^-1.Comment: 14 pages, 9 figures, accepted for publication (MNRAS
Activation of MHD reconnection on ideal timescales
Magnetic reconnection in laboratory, space and astrophysical plasmas is often
invoked to explain explosive energy release and particle acceleration. However,
the timescales involved in classical models within the macroscopic MHD regime
are far too slow to match the observations. Here we revisit the tearing
instability by performing visco-resistive two-dimensional numerical simulations
of the evolution of thin current sheets, for a variety of initial
configurations and of values of the Lunquist number , up to . Results
confirm that when the critical aspect ratio of is reached in the
reconnecting current sheets, the instability proceeds on ideal (Alfv\'enic)
macroscopic timescales, as required to explain observations. Moreover, the same
scaling is seen to apply also to the local, secondary reconnection events
triggered during the nonlinear phase of the tearing instability, thus
accelerating the cascading process to increasingly smaller spatial and temporal
scales. The process appears to be robust, as the predicted scaling is measured
both in inviscid simulations and when using a Prandtl number in the
viscous regime.Comment: Accepted for publication in Plasma Physics and Controlled Fusio
Coupling the Yoccoz-Birkeland population model with price dynamics: Chaotic livestock commodities market cycles
We propose a new model for the time evolution of livestock commodities prices which exhibits endogenous deterministic stochastic behaviour. The model is based on the Yoccoz\u2013Birkeland integral equation, a model first developed for studying the time-evolution of single species with high average fertility, a relatively short mating season and density-dependent reproduction rates. This equation is then coupled with a differential equation describing the price of a livestock commodity driven by the unbalance between its demand and supply. At its birth the cattle population is split into two parts: reproducing females and cattle for butchery. The relative amount of the two is determined by the spot price of the meat. We prove the existence of an attractor (theorem A) and of a non-trivial periodic solution (theorem B) and we investigate numerically the properties of the attractor: the strange attractor existing for the original Yoccoz\u2013Birkeland model is persistent but its chaotic behaviour depends also on the time evolution of the price in an essential way
Can Gravity Distinguish Between Dirac and Majorana Neutrinos?
We show that spin-gravity interaction can distinguish between Dirac and
Majorana neutrino wave packets propagating in a Lense-Thirring background.
Using time-independent perturbation theory and gravitational phase to generate
a perturbation Hamiltonian with spin-gravity coupling, we show that the
associated matrix element for the Majorana neutrino differs significantly from
its Dirac counterpart. This difference can be demonstrated through significant
gravitational corrections to the neutrino oscillation length for a two-flavour
system, as shown explicitly for SN1987A.Comment: 4 pages, 2 figures; minor changes of text; typo corrected; accepted
in Physical Review Letter
Thin shell quantization in Weyl spacetime
We study the problem of quantization of thin shells in a Weyl-Dirac theory by deriving a Wheeler-DeWitt equation from the dynamics. Solutions are found which have interpretations in both cosmology and particle physics
Massive Scalar Particles in a Modified Schwarzschild Geometry
Massive, spinless bosons have vanishing probability of reaching the sphere r=2M from the region r>2M when the original Schwarzschild metric is modified by maximal acceleration corrections
What’s in a child’s ear? The first case of otomyiasis by Sarcophaga argyrostoma (Diptera, Sarcophagidae) and review of the literature
A synthetic glycopeptide of human myelin oligodendrocyte glycoprotein to detect antibody responses in multiple sclerosis and other neurological diseases.
Scale dependence and cross-scale transfer of kinetic energy in compressible hydrodynamic turbulence at moderate Reynolds numbers
We investigate properties of the scale dependence and cross-scale transfer of
kinetic energy in compressible three-dimensional hydrodynamic turbulence, by
means of two direct numerical simulations of decaying turbulence with initial
Mach numbers M = 1/3 and M = 1, and with moderate Reynolds numbers, R_lambda ~
100. The turbulent dynamics is analyzed using compressible and incompressible
versions of the dynamic spectral transfer (ST) and the Karman-Howarth-Monin
(KHM) equations. We find that the nonlinear coupling leads to a flux of the
kinetic energy to small scales where it is dissipated; at the same time, the
reversible pressure-dilatation mechanism causes oscillatory exchanges between
the kinetic and internal energies with an average zero net energy transfer.
While the incompressible KHM and ST equations are not generally valid in the
simulations, their compressible counterparts are well satisfied and describe,
in a quantitatively similar way, the decay of the kinetic energy on large
scales, the cross-scale energy transfer/cascade, the pressure dilatation, and
the dissipation. There exists a simple relationship between the KHM and ST
results through the inverse proportionality between the wave vector k and the
spatial separation length l as k l ~ 3^1/2. For a given time the dissipation
and pressure-dilatation terms are strong on large scales in the KHM approach
whereas the ST terms become dominant on small scales; this is owing to the
complementary cumulative behavior of the two methods. The effect of pressure
dilatation is weak when averaged over a period of its oscillations and may lead
to a transfer of the kinetic energy from large to small scales without a net
exchange between the kinetic and internal energies. Our results suggest that
for large-enough systems there exists an inertial range for the kinetic energy
cascade ...Comment: 14 pages, 10 figure
Field distribution and activity of chlorinated solvents degrading bacteria by combining CARD-FISH and real time PCR
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