61 research outputs found
MHD Turbulence: A Biased Review
This review puts the developments of the last few years in the context of the
canonical time line (Kolmogorov to Iroshnikov-Kraichnan to Goldreich-Sridhar to
Boldyrev). It is argued that Beresnyak's objection that Boldyrev's alignment
theory violates the RMHD rescaling symmetry can be reconciled with alignment if
the latter is understood as an intermittency effect. Boldyrev's scalings,
recovered in this interpretation, are thus an example of a physical theory of
intermittency in a turbulent system. Emergence of aligned structures brings in
reconnection physics, so the theory of MHD turbulence intertwines with the
physics of tearing and current-sheet disruption. Recent work on this by
Loureiro, Mallet et al. is reviewed and it is argued that we finally have a
reasonably complete picture of MHD cascade all the way to the dissipation
scale. This picture appears to reconcile Beresnyak's Kolmogorov scaling of the
dissipation cutoff with Boldyrev's aligned cascade. These ideas also enable
some progress in understanding saturated MHD dynamo, argued to be controlled by
reconnection and to contain, at small scales, a tearing-mediated cascade
similar to its strong-mean-field counterpart. On the margins of this core
narrative, standard weak-MHD-turbulence theory is argued to require adjustment
- and a scheme for it is proposed - to take account of the part that a
spontaneously emergent 2D condensate plays in mediating the Alfven-wave
cascade. This completes the picture of the MHD cascade at large scales. A
number of outstanding issues are surveyed, concerning imbalanced MHD turbulence
(for which a new theory is proposed), residual energy, subviscous and decaying
regimes of MHD turbulence (where reconnection again features prominently).
Finally, it is argued that the natural direction of research is now away from
MHD and into kinetic territory.Comment: 188 pages, 49 figures; (re)submitted to JPP; this version is
substantially modified from v1, especially secs 7.3, 8.2, 11, 12.4, 13.4 and
appendices B.3, C.5, C.
Thermal disequilibration of ions and electrons by collisionless plasma turbulence
Does overall thermal equilibrium exist between ions and electrons in a weakly
collisional, magnetised, turbulent plasma---and, if not, how is thermal energy
partitioned between ions and electrons? This is a fundamental question in
plasma physics, the answer to which is also crucial for predicting the
properties of far-distant astronomical objects such as accretion discs around
black holes. In the context of discs, this question was posed nearly two
decades ago and has since generated a sizeable literature. Here we provide the
answer for the case in which energy is injected into the plasma via Alfv\'enic
turbulence: collisionless turbulent heating typically acts to disequilibrate
the ion and electron temperatures. Numerical simulations using a hybrid
fluid-gyrokinetic model indicate that the ion-electron heating-rate ratio is an
increasing function of the thermal-to-magnetic energy ratio,
: it ranges from at to at
least for . This energy partition is
approximately insensitive to the ion-to-electron temperature ratio
. Thus, in the absence of other equilibrating
mechanisms, a collisionless plasma system heated via Alfv\'enic turbulence will
tend towards a nonequilibrium state in which one of the species is
significantly hotter than the other, viz., hotter ions at high
, hotter electrons at low . Spectra of
electromagnetic fields and the ion distribution function in 5D phase space
exhibit an interesting new magnetically dominated regime at high and
a tendency for the ion heating to be mediated by nonlinear phase mixing
("entropy cascade") when and by linear phase mixing
(Landau damping) when $\beta_\mathrm{i}\gg1
Firehose and Mirror Instabilities in a Collisionless Shearing Plasma
Hybrid-kinetic numerical simulations of firehose and mirror instabilities in
a collisionless plasma are performed in which pressure anisotropy is driven as
the magnetic field is changed by a persistent linear shear . For a
decreasing field, it is found that mostly oblique firehose fluctuations grow at
ion Larmor scales and saturate with energies ; the pressure
anisotropy is pinned at the stability threshold by particle scattering off
microscale fluctuations. In contrast, nonlinear mirror fluctuations are large
compared to the ion Larmor scale and grow secularly in time; marginality is
maintained by an increasing population of resonant particles trapped in
magnetic mirrors. After one shear time, saturated order-unity magnetic mirrors
are formed and particles scatter off their sharp edges. Both instabilities
drive sub-ion-Larmor--scale fluctuations, which appear to be
kinetic-Alfv\'{e}n-wave turbulence. Our results impact theories of momentum and
heat transport in astrophysical and space plasmas, in which the stretching of a
magnetic field by shear is a generic process.Comment: 5 pages, 8 figures, accepted for publication in Physical Review
Letter
Fluidization of collisionless plasma turbulence
In a collisionless, magnetized plasma, particles may stream freely along
magnetic-field lines, leading to phase "mixing" of their distribution function
and consequently to smoothing out of any "compressive" fluctuations (of
density, pressure, etc.,). This rapid mixing underlies Landau damping of these
fluctuations in a quiescent plasma-one of the most fundamental physical
phenomena that make plasma different from a conventional fluid. Nevertheless,
broad power-law spectra of compressive fluctuations are observed in turbulent
astrophysical plasmas (most vividly, in the solar wind) under conditions
conducive to strong Landau damping. Elsewhere in nature, such spectra are
normally associated with fluid turbulence, where energy cannot be dissipated in
the inertial scale range and is therefore cascaded from large scales to small.
By direct numerical simulations and theoretical arguments, it is shown here
that turbulence of compressive fluctuations in collisionless plasmas strongly
resembles one in a collisional fluid and does have broad power-law spectra.
This "fluidization" of collisionless plasmas occurs because phase mixing is
strongly suppressed on average by "stochastic echoes", arising due to nonlinear
advection of the particle distribution by turbulent motions. Besides resolving
the long-standing puzzle of observed compressive fluctuations in the solar
wind, our results suggest a conceptual shift for understanding kinetic plasma
turbulence generally: rather than being a system where Landau damping plays the
role of dissipation, a collisionless plasma is effectively dissipationless
except at very small scales. The universality of "fluid" turbulence physics is
thus reaffirmed even for a kinetic, collisionless system
Magneto-immutable turbulence in weakly collisional plasmas
We propose that pressure anisotropy causes weakly collisional turbulent
plasmas to self-organize so as to resist changes in magnetic-field strength. We
term this effect "magneto-immutability" by analogy with incompressibility
(resistance to changes in pressure). The effect is important when the pressure
anisotropy becomes comparable to the magnetic pressure, suggesting that in
collisionless, weakly magnetized (high-) plasmas its dynamical relevance
is similar to that of incompressibility. Simulations of magnetized turbulence
using the weakly collisional Braginskii model show that magneto-immutable
turbulence is surprisingly similar, in most statistical measures, to critically
balanced MHD turbulence. However, in order to minimize magnetic-field
variation, the flow direction becomes more constrained than in MHD, and the
turbulence is more strongly dominated by magnetic energy (a nonzero "residual
energy"). These effects represent key differences between pressure-anisotropic
and fluid turbulence, and should be observable in the turbulent
solar wind.Comment: Accepted for publication in J. Plasma Phy
Weak Alfvén-wave turbulence revisited
Weak Alfvénic turbulence in a periodic domain is considered as a mixed state of Alfvén waves interacting with the two-dimensional (2D) condensate. Unlike in standard treatments, no spectral continuity between the two is assumed, and, indeed, none is found. If the 2D modes are not directly forced, k−2 and k−1 spectra are found for the Alfvén waves and the 2D modes, respectively, with the latter less energetic than the former. The wave number at which their energies become comparable marks the transition to strong turbulence. For imbalanced energy injection, the spectra are similar, and the Elsasser ratio scales as the ratio of the energy fluxes in the counterpropagating Alfvén waves. If the 2D modes are forced, a 2D inverse cascade dominates the dynamics at the largest scales, but at small enough scales, the same weak and then strong regimes as described above are achieved
Reconnection-controlled decay of magnetohydrodynamic turbulence and the role of invariants
We present a new theoretical picture of magnetically dominated, decaying
turbulence in the absence of a mean magnetic field. We demonstrate that such
turbulence is governed by the reconnection of magnetic structures, and not by
ideal dynamics, as has previously been assumed. We obtain predictions for the
magnetic-energy decay laws by proposing that turbulence decays on reconnection
timescales, while respecting the conservation of certain integral invariants
representing topological constraints satisfied by the reconnecting magnetic
field. As is well known, the magnetic helicity is such an invariant for
initially helical field configurations, but does not constrain non-helical
decay, where the volume-averaged magnetic-helicity density vanishes. For such a
decay, we propose a new integral invariant, analogous to the Loitsyansky and
Saffman invariants of hydrodynamic turbulence, that expresses the conservation
of the random (scaling as ) magnetic helicity contained
in any sufficiently large volume. Our treatment leads to novel predictions for
the magnetic-energy decay laws: in particular, while we expect the canonical
power law for helical turbulence when reconnection is fast (i.e.,
plasmoid-dominated or stochastic), we find a shallower decay in the
slow `Sweet-Parker' reconnection regime, in better agreement with existing
numerical simulations. For non-helical fields, for which there currently exists
no definitive theory, we predict power laws of and in
the fast- and slow-reconnection regimes, respectively. We formulate a general
principle of decay of turbulent systems subject to conservation of Saffman-like
invariants, and propose how it may be applied to MHD turbulence with a strong
mean magnetic field and to isotropic MHD turbulence with initial equipartition
between the magnetic and kinetic energies.Comment: 30 pages, 15 figures, accepted by Phys. Rev.
Cosmic-void observations reconciled with primordial magnetogenesis
It has been suggested that the weak magnetic field hosted by the intergalactic medium in cosmic voids could be a relic from the early Universe. However, accepted models of turbulent magnetohydrodynamic decay predict that the present-day strength of fields originally generated at the electroweak phase transition (EWPT) without parity violation would be too low to explain the observed scattering of γ-rays from TeV blazars. Here, we propose that the decay is mediated by magnetic reconnection and conserves the mean square fluctuation level of magnetic helicity. We find that the relic fields would be stronger by several orders of magnitude under this theory than was indicated by previous treatments, which restores the consistency of the EWPT-relic hypothesis with the observational constraints. Moreover, efficient EWPT magnetogenesis would produce relics at the strength required to resolve the Hubble tension via magnetic effects at recombination and seed galaxy-cluster fields close to their present-day strength
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