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Intermittency in Hall-magnetohydrodynamics with a strong guide field
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10.1063/1.4807378
/content/aip/journal/pop/20/5/10.1063/1.4807378
http://aip.metastore.ingenta.com/content/aip/journal/pop/20/5/10.1063/1.4807378

Figures

Image of FIG. 1.
FIG. 1.

(a) Perpendicular energy spectrum for runs A (solid), B (dot), C (dash), and D (dash-dot). Note how the spectrum becomes steeper in the HMHD simulations for wavenumbers larger than the inverse ion skin depth (respectively, 32, 16, and 8 for runs B, C, and D). The slope indicates Kolmogorov scaling as a reference. (b) Perpendicular energy spectrum compensated by for the same runs.

Image of FIG. 2.
FIG. 2.

Axisymmetric structure functions for the longitudinal magnetic field up to six order for (a) run A ( ), and (b) run D ( ). The order of the structure function is indicated as follows:  = 1 (solid), 2 (dot), 3 (dash), 4 (dash-dot), 5 (dash-triple-dot), and 6 (long dash).

Image of FIG. 3.
FIG. 3.

Scaling exponents (with error bars) as a function of the order up to sixth order, for the velocity (crosses), and for the magnetic field (diamonds), (a) for run A ( ), and (b) for run D ( ). Linear scaling of the exponents with (corresponding to non-intermittent scaling with the second order exponent consistent with the scaling of the energy spectrum in Fig. 1 ) is indicated in both cases by the straight line.

Image of FIG. 4.
FIG. 4.

Fourth order structure function of longitudinal magnetic field increments for runs A ( , solid line), B ( , dashed line), C ( , dashed-dotted line), and D ( , dotted line).

Image of FIG. 5.
FIG. 5.

PDFs for magnetic field increments, for  = 1.6 (solid), 0.8 (dot), 0.4 (dash-dot), 0.2 (dash-triple-dot), and 0.1 (long dashes), and for runs A, B, C, and D from top to bottom, respectively. In all the figures, a dashed curve indicates a Gaussian PDF with unit variance.

Image of FIG. 6.
FIG. 6.

PDFs for velocity field increments, for  = 1.6 (solid), 0.8 (dot), 0.4 (dash-dot), 0.2 (dash-triple-dot), and 0.1 (long dashes), and for runs A, B, C, and D from top to bottom, respectively. In all the figures, a dashed curve indicates a Gaussian PDF with unit variance.

Image of FIG. 7.
FIG. 7.

(a) Velocity field scaling exponents (with error bars) as a function of the order up to sixth order, for runs D (stars), D2 (crosses), and D3 (diamonds) all with . Linear scaling of the exponents is indicated as a reference. (b) Same for the magnetic field scaling exponents.

Image of FIG. 8.
FIG. 8.

(a) PDFs of velocity field increments for  = 0.1 and , for runs D (solid line), D2 (dotted line), and D3 (dashed-dotted line). The three PDFs are practically indistinguishable. The dashed line shows a Gaussian distribution as a reference. (b) Same for magnetic field increments.

Tables

Generic image for table
Table I.

Skewness () and kurtosis () for the -derivatives of and , for all runs with spatial resolution and with different amplitudes of the Hall effect . and are, respectively, the skewness and kurtosis of the magnetic field spatial derivatives, while and are the corresponding quantities for the velocity field derivatives.

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/content/aip/journal/pop/20/5/10.1063/1.4807378
2013-05-23
2014-04-17
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752b84549af89a08dbdd7fdb8b9568b5 journal.articlezxybnytfddd
Scitation: Intermittency in Hall-magnetohydrodynamics with a strong guide field
http://aip.metastore.ingenta.com/content/aip/journal/pop/20/5/10.1063/1.4807378
10.1063/1.4807378
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