Scale invariance of normalized cross-helicity throughout the inertial range of solar wind turbulence

Journal Article · Mon Nov 15 00:00:00 EST 2010 · Physics of Plasmas

DOI:https://doi.org/10.1063/1.3505092· OSTI ID:21532004

Podesta, J J; Borovsky, J E ^[1]

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1. Los Alamos National Laboratory, Los Alamos, New Mexico 87545 (United States)

Solar wind measurements over the period from 1995 through 2006 are used to study fluctuations in the plasma bulk velocity and magnetic field over the range of magnetohydrodynamic (MHD) scales commonly referred to as the inertial range. Power spectra of the solar wind velocity, magnetic field, proton density, total energy (kinetic plus magnetic), and cross-helicity are analyzed for 176 time intervals in which the interplanetary magnetic field is restricted to a single magnetic sector. The data yield measurements of the normalized cross-helicity {sigma}{sub c}, the ratio of the cross-helicity spectrum to the energy spectrum, that span the entire inertial range at 1 AU and extend previous measurements by more than one decade in wavenumber. The results show that {sigma}{sub c} is approximately constant throughout the inertial range, independent of wavenumber, consistent with existing theoretical ideas. At the highest frequencies measured, |{sigma}{sub c}| is observed to decrease toward zero, however, this decrease is caused by measurement noise and is not a real physical effect. Other new results obtained in this study are (1) the average spectral index for the total energy--kinetic plus magnetic--is found to be closer to 3/2 than 5/3 with an average value 1.540{+-}0.033 for highly Alfvenic wind, in agreement with simulations of incompressible MHD turbulence with a strong ambient magnetic field; (2) the spectral index for the total energy is a function of |{sigma}{sub c}| that varies from roughly 5/3 when {sigma}{sub c}{approx_equal}0 to approximately 3/2 when |{sigma}{sub c}|{approx_equal}1; (3) the spectral index for the total energy exhibits a solar cycle dependence during solar cycle 23 with above average values (steeper spectra) in the early rising phase of the cycle and below average values (shallower spectra) during the declining phase of the cycle--the controlling parameter for this solar cycle dependence appears to be |{sigma}{sub c}|.

• OSTI ID: 21532004
• Journal Information: Physics of Plasmas, Vol. 17, Issue 11; Other Information: DOI: 10.1063/1.3505092; (c) 2010 American Institute of Physics; ISSN 1070-664X
• Country of Publication: United States
• Language: English

Related Subjects

70 PLASMA PHYSICS AND FUSION TECHNOLOGY
72 PHYSICS OF ELEMENTARY PARTICLES AND FIELDS
ENERGY SPECTRA
FLUCTUATIONS
HELICITY
INTERPLANETARY MAGNETIC FIELDS
MAGNETOHYDRODYNAMICS
PLASMA SIMULATION
PROTON DENSITY
SCALE INVARIANCE
SOLAR WIND
TURBULENCE
VELOCITY
FLUID MECHANICS
HYDRODYNAMICS
INVARIANCE PRINCIPLES
MAGNETIC FIELDS
MECHANICS
PARTICLE PROPERTIES
SIMULATION
SOLAR ACTIVITY
SPECTRA
STELLAR ACTIVITY
STELLAR WINDS
VARIATIONS