Two-fluid turbulence including electron inertia

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We present a full two-fluid magnetohydrodynamic (MHD) description for a completely ionized hydrogen plasma, retaining the effects of the Hall current, electron pressure, and electron inertia. According to this description, each plasma species introduces a new spatial scale: the ion inertial length λ...

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Autor principal: Andrés, Nahuel
Otros Autores: Gonzalez, C., Martin, L., Dmitruk, P., Gómez, D.
Formato: Capítulo de libro
Lenguaje:Inglés
Publicado: American Institute of Physics Inc. 2014
Acceso en línea:Registro en Scopus
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100 1 |a Andrés, Nahuel 
245 1 0 |a Two-fluid turbulence including electron inertia 
260 |b American Institute of Physics Inc.  |c 2014 
270 1 0 |m Andrés, N.; Instituto de Astronomía Y Física del Espacio, CC. 67, suc. 28, Argentina 
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506 |2 openaire  |e Política editorial 
520 3 |a We present a full two-fluid magnetohydrodynamic (MHD) description for a completely ionized hydrogen plasma, retaining the effects of the Hall current, electron pressure, and electron inertia. According to this description, each plasma species introduces a new spatial scale: the ion inertial length λi and the electron inertial length λe, which are not present in the traditional MHD description. In the present paper, we seek for possible changes in the energy power spectrum in fully developed turbulent regimes, using numerical simulations of the two-fluid equations in two-and-a-half dimensions. We have been able to reproduce different scaling laws in different spectral ranges, as it has been observed in the solar wind for the magnetic energy spectrum. At the smallest wavenumbers where plain MHD is valid, we obtain an inertial range following a Kolmogorov k-5/3 law. For intermediate wavenumbers such that λi -1 蠐 k 蠐 λe -1, the spectrum is modified to a k-7/3 power-law, as has also been obtained for Hall-MHD neglecting electron inertia terms. When electron inertia is retained, a new spectral region given by k > λe -1 arises. The power spectrum for magnetic energy in this region is given by a k-11/3 power law. Finally, when the terms of electron inertia are retained, we study the self-consistent electric field. Our results are discussed and compared with those obtained in the solar wind observations and previous simulations. © 2014 AIP Publishing LLC.  |l eng 
593 |a Instituto de Astronomía Y Física del Espacio, CC. 67, suc. 28, Buenos Aires, 1428, Argentina 
593 |a Departamento de Física, Facultad de Ciencias Exactas Y Naturales, Universidad de Buenos Aires, Buenos Aires, 1428, Argentina 
690 1 0 |a ELECTRIC FIELDS 
690 1 0 |a ELECTRONS 
690 1 0 |a MAGNETOPLASMA 
690 1 0 |a POWER SPECTRUM 
690 1 0 |a SOLAR WIND 
690 1 0 |a TURBULENT FLOW 
690 1 0 |a ELECTRON INERTIA 
690 1 0 |a ELECTRON PRESSURES 
690 1 0 |a INERTIAL RANGES 
690 1 0 |a ION INERTIAL LENGTH 
690 1 0 |a IONIZED HYDROGEN PLASMAS 
690 1 0 |a MAGNETIC ENERGIES 
690 1 0 |a SPECTRAL REGION 
690 1 0 |a TURBULENT REGIME 
690 1 0 |a MAGNETOHYDRODYNAMICS 
700 1 |a Gonzalez, C. 
700 1 |a Martin, L. 
700 1 |a Dmitruk, P. 
700 1 |a Gómez, D. 
773 0 |d American Institute of Physics Inc., 2014  |g v. 21  |k n. 12  |p Phys. Plasmas  |x 1070664X  |w (AR-BaUEN)CENRE-6479  |t Physics of Plasmas 
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