Searcharxiv⌕ Search

arXiv subjects

Mahendra K. Verma

Publications and source records attributed to Mahendra K. Verma.

125 records · Page 7Linked to original sources

Comment on "On two-dimensional magnetohydrodynamic turbulence" [Phys. Plasmas, 8, 3282 (2001)]

Biskamp and Schwarz [Phys. Plasmas, 8, 3282 (2001)] have reported that the energy spectrum of two-dimensional magnetohydrodynamic turbulence is proportional to $k^{-3/2}$, which is a prediction of Iroshnikov-Kraichnan phenomenology. In this comment we report some earlier results which conclusively show that for two-dimensional magnetohydrodynamic turbulence, Kolmogorov-like phenomenology (spectral index 5/3) is better model than Iroshnikov-Kraichnan phenomenology; these results are based on energy flux analysis.

nlin.CD↗

On Generation of magnetic field in astrophysical bodies

In this letter we compute energy transfer rates from velocity field to magnetic field in MHD turbulence using field-theoretic method. The striking result of our field theoretic calculation is that there is a large energy transfer rate from the large-scale velocity field to the large-scale magnetic field. We claim that the growth of large-scale magnetic energy is primarily due to this transfer. We reached the above conclusion without any linear approximation like that in $α$-dynamo.

nlin.CD↗

Energy transfer in two-dimensional magnetohydrodynamic turbulence: formalism and numerical results

The basic entity of nonlinear interaction in Navier-Stokes and the Magnetohydrodynamic (MHD) equations is a wavenumber triad ({\bf k,p,q}) satisfying ${\bf k+p+q=0}$. The expression for the combined energy transfer from two of these wavenumbers to the third wavenumber is known. In this paper we introduce the idea of an effective energy transfer between a pair of modes by the mediation of the third mode, and find an expression for it. Then we apply this formalism to compute the energy transfer in the quasi-steady-state of two-dimensional MHD turbulence with large-scale kinetic forcing. The computation of energy fluxes and the energy transfer between different wavenumber shells is done using the data generated by the pseudo-spectral direct numerical simulation. The picture of energy flux that emerges is quite complex---there is a forward cascade of magnetic energy, an inverse cascade of kinetic energy, a flux of energy from the kinetic to the magnetic field, and a reverse flux which transfers the energy back to the kinetic from the magnetic. The energy transfer between different wavenumber shells is also complex---local and nonlocal transfers often possess opposing features, i.e., energy transfer between some wavenumber shells occurs from kinetic to magnetic, and between other wavenumber shells this transfer is reversed. The net transfer of energy is from kinetic to magnetic. The results obtained from the studies of flux and shell-to-shell energy transfer are consistent with each other.

nlin.CD↗

Calculation of renormalized viscosity and resistivity in magnetohydrodynamic turbulence

A self-consistent renormalization (RG) scheme has been applied to nonhelical magnetohydrodynamic turbulence with normalized cross helicity $σ_c =0$ and $σ_c \to 1$. Kolmogorov's 5/3 powerlaw is assumed in order to compute the renormalized parameters. It has been shown that the RG fixed point is stable for $d \ge d_c \approx 2.2$. The renormalized viscosity $ν^*$ and resistivity $η^*$ have been calculated, and they are found to be positive for all parameter regimes. For $σ_c=0$ and large Alfvén ratio (ratio of kinetic and magnetic energies) $r_A$, $ν^*=0.36$ and $η^*=0.85$. As $r_A$ is decreased, $ν^*$ increases and $η^*$ decreases, untill $r_A \approx 0.25$ where both $ν^*$ and $η^*$ are approximately zero. For large $d$, both $ν^*$ and $η^*$ vary as $d^{-1/2}$. The renormalized parameters for the case $σ_c \to 1$ are also reported.

nlin.CD↗

Field theoretic calculation of renormalized-viscosity, renormalized-resistivity, and energy fluxes of magnetohydrodynamic turbulence

A self-consistent renormalization (RG) scheme has been applied to nonhelical magnetohydrodynamic turbulence with zero cross helicity. Kolmogorov's 5/3 powerlaw has been shown to be a consistent solution for $d \ge d_c \approx 2.2$. For Kolmogorov's solution, both renormalized viscosity and resistivity are positive for the whole range of parameters. Various cascade rate and Kolmogorov's constant for MHD turbulence have been calculated by solving the flux equation to the first order in perturbation series. We find that the magnetic energy cascades forward. The Kolmogorov's constant for $d=3$ does not vary significantly with $r_A$ and is found to be close to the constant for fluid turbulence.

nlin.CD↗

Energy transfer in two-dimensional magnetohydrodynamic turbulence

In an earlier paper (physics/0006012) we had developed a method for computing the effective energy transfer between any two Fourier modes in fluid or magnetohydrodynamic (MHD) flows. This method is applied to a pseudo-spectral, direct numerical simulation (DNS) study of energy transfer in the quasi-steady state of 2-D MHD turbulence with large scale kinetic forcing. Two aspects of energy transfer are studied: the energy fluxes, and the energy transfer between different wavenumber regions ({\it shells}). The picture of energy fluxes that emerges is quite complex - there is a forward cascade of magnetic energy, an inverse cascade of kinetic energy, a flux of energy from the kinetic to the magnetic field, and a reverse flux which transfers the energy back to the kinetic from the magnetic. The energy transfer between different wave number shells is also complex - local and nonlocal transfers often possess opposing features, i.e., energy transfer between some wave number shells occurs from kinetic to magnetic, and between other wave number shells this transfer is reversed. The net transfer of energy is from kinetic to magnetic. The results obtained from the flux studies and the shell-to-shell energy transfer studies are consistent with each other.

chao-dyn↗

A new approach to study energy transfer in turbulence

The unit of nonlinear interaction in Navier-Stokes and the Magnetohydrodynamic (MHD) equations is a wavenumber triad ({\bf k,p,q}) satisfying ${\bf k+p+q=0}$. The expression for the combined energy transfer from two of these wavenumbers to the third wavenumber is known. In this paper we introduce the idea of an effective energy transfer between a pair of modes through the mediation of the third mode and then find an expression for it. In fluid turbulence, energy transfer takes place between a pair of velocity modes, whereas in MHD turbulence energy transfer takes places between (1) a pair of velocity modes, (2) a pair of magnetic modes, and (3) between a velocity and a magnetic mode in a triad. In this paper we have obtained the expression for each of these transfers. We also show how the effective mode-to-mode energy transfer rate can be utilised to study energy cascades and shell-to-shell energy transfer rates.

physics.flu-dyn↗

Intermittency exponents and energy spectrum of the Burgers and KPZ equations with correlated noise

We numerically calculate the energy spectrum, intermittency exponents, and probability density $P(u')$ of the one-dimensional Burgers and KPZ equations with correlated noise. We have used pseudo-spectral method for our analysis. When $σ$ of the noise variance of the Burgers equation (variance $\propto k^{-2 σ}$) exceeds 3/2, large shocks appear in the velocity profile leading to $<|u(k)|^2> \propto k^{-2}$, and structure function $<|u(x+r,t)-u(x,t)|^q> \propto r$ suggesting that the Burgers equation is intermittent for this range of $σ$. For $-1 \le σ\le 0$, the profile is dominated by noise, and the spectrum $<|h(k)|^{2}>$ of the corresponding KPZ equation is in close agreement with Medina et al.'s renormalization group predictions. In the intermediate range $0 < σ<3/2$, both noise and well-developed shocks are seen, consequently the exponents slowly vary from RG regime to a shock-dominated regime. The probability density $P(h)$ and $P(u)$ are gaussian for all $σ$, while $P(u')$ is gaussian for $σ=-1$, but steadily becomes nongaussian for larger $σ$; for negative $u'$, $P(u') \propto \exp(-a x)$ for $σ=0$, and approximately $\propto u'^{-5/2}$ for $σ> 1/2$. We have also calculated the energy cascade rates for all $σ$ and found a constant flux for all $σ\ge 1/2$.

chao-dyn↗

Probing Physics of Magnetohydrodynamic Turbulence Using Direct Numerical Simulation

The energy spectrum and the nolinear cascade rates of MHD turbulence is not clearly understood. We have addressed this problem using direct numerical simulation and analytical calculations. Our numerical simulations indicate that Kolmogorov-like phenomenology with $k^{-5/3}$ energy spectrum, rather than Kraichnan's $k^{-3/2}$, appears to be applicable in MHD turbulence. Here, we also construct a self-consistent renomalization group procedure in which the mean magnetic field gets renormalized, which in turns yields $k^{-5/3}$ energy spectrum. The numerical simulations also show that the fluid energy is transferred to magnetic energy. This result could shed light on the generation magnetic field as in dynamo mechanism.

chao-dyn↗

Initial Condition Sensitivity of Global Quantities in Magnetohydrodynamic Turbulence

In this paper we study the effect of subtle changes in initial conditions on the evolution of global quantities in two-dimensional Magnetohydrodynamic (MHD) turbulence. We find that a change in the initial phases of complex Fourier modes of the Elsässer variables, while keeping the initial values of total energy, cross helicity and Alfvén ratio unchanged, has a significant effect on the evolution of cross helicity. On the contrary, the total energy and Alfvén ratio are insensitive to the initial phases. Our simulations are based on direct numerical simulation using the pseudo-spectral method.

chao-dyn↗

Mean magnetic field renormalization and Kolmogorov's energy spectrum in MHD turbulence

In this paper we construct a self-consistent renormalization group procedure for MHD turbulence in which small wavenumber modes are averaged out, and effective mean magnetic field at large wavenumbers is obtained. In this scheme the mean magnetic field scales as $k^{-1/3}$, while the energy spectrum scales as $k^{-5/3}$ similar to that in fluid turbulence. We also deduce from the formalism that the magnitude of cascade rate decreases as the strength of the mean magnetic field is increased.

chao-dyn↗

Anomalous Viscosity, Resistivity, and Thermal Diffusivity of the Solar Wind Plasma

In this paper we have estimated typical anomalous viscosity, resistivity, and thermal difffusivity of the solar wind plasma. Since the solar wind is collsionless plasma, we have assumed that the dissipation in the solar wind occurs at proton gyro radius through wave-particle interactions. Using this dissipation length-scale and the dissipation rates calculated using MHD turbulence phenomenology [{\it Verma et al.}, 1995a], we estimate the viscosity and proton thermal diffusivity. The resistivity and electron's thermal diffusivity have also been estimated. We find that all our transport quantities are several orders of magnitude higher than those calculated earlier using classical transport theories of {\it Braginskii}. In this paper we have also estimated the eddy turbulent viscosity.

chao-dyn↗

Direct Interaction Approximation of Magnetohydrodynamic Turbulence

In this paper we apply Kraichnan's direct interaction approximation, which is a one loop perturbation expansion, to magnetohydrodynamic turbulence. By substituting the energy spectra both from kolmogorov-like MHD turbulence phenomenology and a generalization of Dobrowolny et al.'s model we obtain Kolmogorov's and Kraichnan's constant for MHD turbulence. We find that the constants depend of the Alfvén ratio and normalized cross helicity; the dependence has been studied here. We also demonstrate the inverse cascade of magnetic energy for Kolmogorov-like models. Our results are in general agreement with the earlier simulation results except for large normalized cross helicity.

chao-dyn↗

Turbulent Heating in the Solar Wind and in the Solar Corona

In this paper we calculate the turbulent heating rates in the solar wind using the Kolmogorov-like MHD turbulence phenomenology with Kolmogorov's constants calculated by {\it Verma and Bhattacharjee }[1995b,c]. We find that the turbulent heating can not account for the total heating of the nonAlfvénic streams in the solar wind. We show that dissipation due to thermal conduction is also a potential heating source. Regarding the Alfvénic streams, the predicted turbulent heating rates using the constants of {\it Verma and Bhattacharjee }[1995c] are higher than the observed heating rates; the predicted dissipation rates are probably overestimates because Alfvénic streams have not reached steady-state. We also compare the predicted turbulent heating rates in the solar corona with the observations; the Kolmogorov-like phenomenology predicts dissipation rates comparable to the observed heating rates in the corona [{\it Hollweg, }% 1984], but Dobrowoly et al.'s generalized Kraichnan model yields heating rates much less than that required.

chao-dyn↗

Computation of Kolmogorov's Constant in Magnetohydrodynamic Turbulence

In this paper we calculate Kolmogorov's constant for magnetohydrodynamic turbulence to one loop order in perturbation theory using the direct interaction approximation technique of Kraichnan. We have computed the constants for various $E^u(k)/E^b(k)$, i.e., fluid to magnetic energy ratios when the normalized cross helicity is zero. We find that $K$ increases from 1.47 to 4.12 as we go from fully fluid case $(E^b=0)$ to a situation when $% E^u/E^b=0.5$, then it decreases to 3.55 in a fully magnetic limit $(E^u=0)$. When $E^u/E^b=1$, we find that $K=3.43$.

chao-dyn↗