Finite dissipation and intermittency in magnetohydrodynamics

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We present an analysis of data stemming from numerical simulations of decaying magnetohydrodynamic (MHD) turbulence up to grid resolution of 15363 points and up to Taylor Reynolds number of ∼1200. The initial conditions are such that the initial velocity and magnetic fields are helical and in equipa...

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Autor principal: Mininni, P.D
Otros Autores: Pouquet, A.
Formato: Capítulo de libro
Lenguaje:Inglés
Publicado: 2009
Acceso en línea:Registro en Scopus
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Biblioteca Central Dr. Luis F. Leloir (FCEN) de Universidad de Buenos Aires
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100 1 |a Mininni, P.D. 
245 1 0 |a Finite dissipation and intermittency in magnetohydrodynamics 
260 |c 2009 
270 1 0 |m Mininni, P. D.; Departamento de Física, Facultad de Ciencias Exactas y Naturales, Ciudad Universitaria, 1428 Buenos Aires, Argentina 
506 |2 openaire  |e Política editorial 
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520 3 |a We present an analysis of data stemming from numerical simulations of decaying magnetohydrodynamic (MHD) turbulence up to grid resolution of 15363 points and up to Taylor Reynolds number of ∼1200. The initial conditions are such that the initial velocity and magnetic fields are helical and in equipartition, while their correlation is negligible. Analyzing the data at the peak of dissipation, we show that the dissipation in MHD seems to asymptote to a constant as the Reynolds number increases, thereby strengthening the possibility of fast reconnection events in the solar environment for very large Reynolds numbers. Furthermore, intermittency of MHD flows, as determined by the spectrum of anomalous exponents of structure functions of the velocity and the magnetic field, is stronger than that of fluids, confirming earlier results; however, we also find that there is a measurable difference between the exponents of the velocity and those of the magnetic field, reminiscent of recent solar wind observations. Finally, we discuss the spectral scaling laws that arise in this flow. © 2009 The American Physical Society.  |l eng 
593 |a Departamento de Física, Facultad de Ciencias Exactas y Naturales, Ciudad Universitaria, 1428 Buenos Aires, Argentina 
593 |a NCAR, P.O. Box 3000, Boulder, CO 80307-3000, United States 
690 1 0 |a ANALYSIS OF DATA 
690 1 0 |a EQUIPARTITION 
690 1 0 |a FAST RECONNECTION 
690 1 0 |a GRID RESOLUTION 
690 1 0 |a INITIAL CONDITIONS 
690 1 0 |a INITIAL VELOCITIES 
690 1 0 |a INTERMITTENCY 
690 1 0 |a MHD FLOW 
690 1 0 |a NUMERICAL SIMULATION 
690 1 0 |a SOLAR ENVIRONMENT 
690 1 0 |a STRUCTURE FUNCTIONS 
690 1 0 |a TAYLOR-REYNOLDS NUMBER 
690 1 0 |a COMPUTER SIMULATION LANGUAGES 
690 1 0 |a FLUID DYNAMICS 
690 1 0 |a MAGNETOHYDRODYNAMICS 
690 1 0 |a REYNOLDS NUMBER 
690 1 0 |a SOLAR WIND 
690 1 0 |a MAGNETIC FIELDS 
700 1 |a Pouquet, A. 
773 0 |d 2009  |g v. 80  |k n. 2  |p Phys. Rev. E Stat. Nonlinear Soft Matter Phys.  |x 15393755  |t Physical Review E - Statistical, Nonlinear, and Soft Matter Physics 
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856 4 0 |u https://doi.org/10.1103/PhysRevE.80.025401  |y DOI 
856 4 0 |u https://hdl.handle.net/20.500.12110/paper_15393755_v80_n2_p_Mininni  |y Handle 
856 4 0 |u https://bibliotecadigital.exactas.uba.ar/collection/paper/document/paper_15393755_v80_n2_p_Mininni  |y Registro en la Biblioteca Digital 
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962 |a info:eu-repo/semantics/article  |a info:ar-repo/semantics/artículo  |b info:eu-repo/semantics/publishedVersion 
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