Finite dissipation and intermittency in magnetohydrodynamics

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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Autores principales: Mininni, P.D., Pouquet, A.
Formato: JOUR
Materias:
Analysis of data
Equipartition
Fast reconnection
Grid resolution
Initial conditions
Initial velocities
Intermittency
MHD flow
Numerical simulation
Solar environment
Structure functions
Taylor-Reynolds number
Computer simulation languages
Fluid dynamics
Magnetohydrodynamics
Reynolds number
Solar wind
Magnetic fields
Acceso en línea:http://hdl.handle.net/20.500.12110/paper_15393755_v80_n2_p_Mininni
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Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA) de Universidad de Buenos Aires
id todo:paper_15393755_v80_n2_p_Mininni
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spelling todo:paper_15393755_v80_n2_p_Mininni2023-10-03T16:22:28Z Finite dissipation and intermittency in magnetohydrodynamics Mininni, P.D. Pouquet, A. Analysis of data Equipartition Fast reconnection Grid resolution Initial conditions Initial velocities Intermittency MHD flow Numerical simulation Solar environment Structure functions Taylor-Reynolds number Computer simulation languages Fluid dynamics Magnetohydrodynamics Reynolds number Solar wind Magnetic fields 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. Fil:Mininni, P.D. Universidad de Buenos Aires. Facultad de Ciencias Exactas y Naturales; Argentina. JOUR info:eu-repo/semantics/openAccess http://creativecommons.org/licenses/by/2.5/ar http://hdl.handle.net/20.500.12110/paper_15393755_v80_n2_p_Mininni
institution Universidad de Buenos Aires
institution_str I-28
repository_str R-134
collection Biblioteca Digital - Facultad de Ciencias Exactas y Naturales (UBA)
topic Analysis of data
Equipartition
Fast reconnection
Grid resolution
Initial conditions
Initial velocities
Intermittency
MHD flow
Numerical simulation
Solar environment
Structure functions
Taylor-Reynolds number
Computer simulation languages
Fluid dynamics
Magnetohydrodynamics
Reynolds number
Solar wind
Magnetic fields
spellingShingle Analysis of data
Equipartition
Fast reconnection
Grid resolution
Initial conditions
Initial velocities
Intermittency
MHD flow
Numerical simulation
Solar environment
Structure functions
Taylor-Reynolds number
Computer simulation languages
Fluid dynamics
Magnetohydrodynamics
Reynolds number
Solar wind
Magnetic fields
Mininni, P.D.
Pouquet, A.
Finite dissipation and intermittency in magnetohydrodynamics
topic_facet Analysis of data
Equipartition
Fast reconnection
Grid resolution
Initial conditions
Initial velocities
Intermittency
MHD flow
Numerical simulation
Solar environment
Structure functions
Taylor-Reynolds number
Computer simulation languages
Fluid dynamics
Magnetohydrodynamics
Reynolds number
Solar wind
Magnetic fields
description 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.
format JOUR
author Mininni, P.D.
Pouquet, A.
author_facet Mininni, P.D.
Pouquet, A.
author_sort Mininni, P.D.
title Finite dissipation and intermittency in magnetohydrodynamics
title_short Finite dissipation and intermittency in magnetohydrodynamics
title_full Finite dissipation and intermittency in magnetohydrodynamics
title_fullStr Finite dissipation and intermittency in magnetohydrodynamics
title_full_unstemmed Finite dissipation and intermittency in magnetohydrodynamics
title_sort finite dissipation and intermittency in magnetohydrodynamics
url http://hdl.handle.net/20.500.12110/paper_15393755_v80_n2_p_Mininni
work_keys_str_mv AT mininnipd finitedissipationandintermittencyinmagnetohydrodynamics
AT pouqueta finitedissipationandintermittencyinmagnetohydrodynamics
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