&lt;title&gt;Adaptive optics in ophthalmology&lt;/title&gt;

Iroshnikov, N. G.; Larichev, A. V.

doi:10.1117/12.714172

Cited by 34 publications

(56 citation statements)

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“…Magnetoplasma turbulence evolves under the action of non-linear interactions in that larger eddies transfer their energy to smaller ones through a forward cascade. According to Kolmogorov (1941), Iroshnikov (1963) and Kraichnan (1965), the cascade of spectral energy is mediated by a local interaction amongst the neighbouring Fourier modes that continues until the energy in the smallest turbulent eddies is dissipated due to the finite Reynolds number. This leads to the damping of small-scale motions as well.…”

Section: N O N -L I N E a R S I M U L At I O N Smentioning

confidence: 99%

“…For instance, the assumption of isotropy breaks down in the presence the mean or largescale magnetic field. Along the direction of this large-scale magnetic field, Alfvén waves suppress the parallel cascade (Iroshnikov 1963;Kraichnan 1965). The resulting inertial range MHD spectrum is therefore thought to be flattened from k −5/3 to k −3/2 (Iroshnikov 1963;Kraichnan 1965).…”

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confidence: 99%

“…Along the direction of this large-scale magnetic field, Alfvén waves suppress the parallel cascade (Iroshnikov 1963;Kraichnan 1965). The resulting inertial range MHD spectrum is therefore thought to be flattened from k −5/3 to k −3/2 (Iroshnikov 1963;Kraichnan 1965). Within the paradigm of incompressible MHD turbulence, Goldreich & Sridhar (1995) proposed that parallel (k ) and perpendicular (k ⊥ ) modes are correlated by k ∝ k 2/3 ⊥ and energy in the perpendicular modes follows a Kolmogorov-like spec-trum when linear (along B 0 ) and non-linear (across B 0 ) frequencies balance.…”

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confidence: 99%

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The turbulent density spectrum in the solar wind plasma

Shaikh¹,

Zank²

2009

Monthly Notices of the Royal Astronomical Society

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The density fluctuation spectrum in the solar wind reveals a Kolmogorov‐like scaling with a spectral slope of −5/3 in wavenumber space. The energy transfer process in the magnetized solar wind, characterized typically by magnetohydrodynamic turbulence, over extended length‐scales remains an unresolved paradox of modern turbulence theories, raising the question of how a compressible magnetofluid exhibits a turbulent spectrum that is a characteristic of an incompressible hydrodynamic fluid. To address these questions, we have undertaken three‐dimensional time‐dependent numerical simulations of a compressible magnetohydrodynamic fluid describing super‐Alfvénic, supersonic and strongly magnetized plasma fluid. It is shown that a Kolmogorov‐like density spectrum can develop by plasma motions that are dominated by Alfvénic cascades whereas compressive modes are dissipated.

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Section: N O N -L I N E a R S I M U L At I O N Smentioning

confidence: 99%

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confidence: 99%

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confidence: 99%

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The turbulent density spectrum in the solar wind plasma

Shaikh¹,

Zank²

2009

Monthly Notices of the Royal Astronomical Society

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“…The Iroshnikov-Kraichnan's (IK) phenomenology [13,14] couples the two previous timescales without introducing a distinction between the perpendicular and the parallel direction; assuming isotropy we get the famous The former time is similar to the eddy-turnover time in Navier-Stokes turbulence and may be associated to the distortion of wave packets whereas the latter may be seen as the duration of interaction between two counter-propagating linear plane Alfvén waves.…”

Section: Iroshnikov-kraichnan Spectrummentioning

confidence: 99%

Solar Wind Turbulence: New Questions and Possible Solutions

Galtier¹

2010

AIP Conference Proceedings

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Anomalous scaling and the role of intermittency in solar wind MHD turbulence: new insights AIP Conf. Proc. 932, 75 (2007);Abstract. The interplanetary medium provides a vast natural laboratory for studying many fundamental questions about astrophysical plasmas. In this paper I make a short review on what we know about turbulent fluctuations which behave differently at low (f < 1 Hz) and high (f > Hz) frequencies. Particular attention is made about anisotropy at low frequency and its MHD modeling as well as the origin of a second inertial range at high frequencies characterized by steep power law spectra which cannot be associated with MHD fluctuations.

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“…For example, the weak, isotropic, incompressible phenomenology of Iroshnikov and Kraichnan ͑IK͒, 17,18 where the dominant process is Alfvén wave collisions, gives a =4 or p ± = p /4. The parameter a is anomalous in that it no longer follows from a dimensional analysis in the sense of K41.…”

Section: Introductionmentioning

confidence: 99%

Intermittency, dissipation, and scaling in two-dimensional magnetohydrodynamic turbulence

2007

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Direct numerical simulations (DNS) provide a means to test phenomenological models for the scaling properties of intermittent MHD turbulence. The well-known model of She and Leveque, when generalized to MHD, is in good agreement with the DNS in three dimensions, however, it does not coincide with DNS in two dimensions (2D). This is resolved here using the results of recent DNS of driven MHD turbulence in 2D which directly determine the scaling of the rate of dissipation. Specifically, a simple modification to generalized refined similarity is proposed that captures the results of the 2D MHD simulations. This leads to a new generalization of She and Leveque in MHD that is coincident with the DNS results in 2D. A key feature of this model is that the most intensely dissipating structures, which are responsible for the intermittency, are thread-like in 2D, independent of whether the underlying phenomenology of the cascade is Kolmogorov or Iroshnikov Kraichnan.

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<title>Adaptive optics in ophthalmology</title>

Cited by 34 publications

References 0 publications

The turbulent density spectrum in the solar wind plasma

The turbulent density spectrum in the solar wind plasma

Solar Wind Turbulence: New Questions and Possible Solutions

Intermittency, dissipation, and scaling in two-dimensional magnetohydrodynamic turbulence

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