Aspects of the theory of incompressible MHD turbulence with crosshelicity and applications to the solar wind
Abstract
Solar wind observations have shown that the normalized crosshelicity {sigma}{sub c}, the ratio of the crosshelicity spectrum to the energy spectrum, is approximately constant, independent of wavenumber, throughout the inertial range. This means that the correlation between velocity and magnetic field fluctuations is the same at every scale, that the ratio of the two Elsasser energies (w{sup +}/w{sup }){sup 2} is the same at every scale, and that the ratio of the energy cascade times of the two Elsasser energies {tau}{sup +}/{tau}{sup } is the same at every scale. In the case when the magnetic Prandtl number is unity, it can be shown from the equations of incompressible MHD that if {sigma}{sub c} is a constant, then the cascade times of the two Elsasser energies are equal so that {tau}{sup +}/{tau}{sup } = 1. This is an important constraint for turbulence theories. Using this result, the Goldreich and Sridhar theory and the Boldyrev theory are generalized to MHD turbulence with nonvanishing crosshelicity in such a way that the scaling laws of the original two theories are unchanged. The derivation and some of the important properties of these more general theories shall be presented. Solar wind measurements in support of thesemore »
 Authors:

 Los Alamos National Laboratory
 Publication Date:
 Research Org.:
 Los Alamos National Lab. (LANL), Los Alamos, NM (United States)
 Sponsoring Org.:
 USDOE
 OSTI Identifier:
 1043539
 Report Number(s):
 LAUR1008027; LAUR108027
TRN: US201214%%81
 DOE Contract Number:
 AC5206NA25396
 Resource Type:
 Conference
 Resource Relation:
 Conference: 2010 AGU Fall Meeting ; December 13, 2010 ; San Francisco, CA
 Country of Publication:
 United States
 Language:
 English
 Subject:
 32 ENERGY CONSERVATION, CONSUMPTION, AND UTILIZATION; 79 ASTROPHYSICS, COSMOLOGY AND ASTRONOMY; HELICITY; MAGNETIC FIELDS; MAGNETOHYDRODYNAMICS; MEETINGS; PRANDTL NUMBER; SCALING LAWS; SOLAR WIND; TURBULENCE; WASTE HEAT UTILIZATION
Citation Formats
Podesta, John J. Aspects of the theory of incompressible MHD turbulence with crosshelicity and applications to the solar wind. United States: N. p., 2010.
Web.
Podesta, John J. Aspects of the theory of incompressible MHD turbulence with crosshelicity and applications to the solar wind. United States.
Podesta, John J. Fri .
"Aspects of the theory of incompressible MHD turbulence with crosshelicity and applications to the solar wind". United States. https://www.osti.gov/servlets/purl/1043539.
@article{osti_1043539,
title = {Aspects of the theory of incompressible MHD turbulence with crosshelicity and applications to the solar wind},
author = {Podesta, John J},
abstractNote = {Solar wind observations have shown that the normalized crosshelicity {sigma}{sub c}, the ratio of the crosshelicity spectrum to the energy spectrum, is approximately constant, independent of wavenumber, throughout the inertial range. This means that the correlation between velocity and magnetic field fluctuations is the same at every scale, that the ratio of the two Elsasser energies (w{sup +}/w{sup }){sup 2} is the same at every scale, and that the ratio of the energy cascade times of the two Elsasser energies {tau}{sup +}/{tau}{sup } is the same at every scale. In the case when the magnetic Prandtl number is unity, it can be shown from the equations of incompressible MHD that if {sigma}{sub c} is a constant, then the cascade times of the two Elsasser energies are equal so that {tau}{sup +}/{tau}{sup } = 1. This is an important constraint for turbulence theories. Using this result, the Goldreich and Sridhar theory and the Boldyrev theory are generalized to MHD turbulence with nonvanishing crosshelicity in such a way that the scaling laws of the original two theories are unchanged. The derivation and some of the important properties of these more general theories shall be presented. Solar wind measurements in support of these theoretical models will also be discussed. For example, new solar wind measurements of the total energy spectrum (kinetic plus magnetic) show that the powerlaw exponent is closer to 3/2 than 5/3, consistent with simulations of 3D incompressible MHD turbulence with a strong mean meagnetic field that show a 3/2 scaling. For highly Alfvenic, high crosshelicity solar wind turbulence, new measurements presented her show that the average spectral index is 1.540 {+} 0.033.},
doi = {},
url = {https://www.osti.gov/biblio/1043539},
journal = {},
number = ,
volume = ,
place = {United States},
year = {2010},
month = {12}
}