The Turbulent Cascade and Proton Heating in the Solar Wind at 1 Au

Stawarz, J. E.; Smith, Charles W.; Vasquez, Bernard J.; Forman, M. A.; MacBride, Benjamin T.

doi:10.1088/0004-637x/697/2/1119

Cited by 140 publications

(146 citation statements)

References 46 publications

Supporting

Mentioning

131

Contrasting

Order By: Relevance

“…As before [20,23,30,126], the average over many samples produces a net forward transfer of both pseudo-energies consistent with the observed solar wind heating. The estimates derived from individual 1 h samples show evidence of intermittent dynamics with a high degree of variability relative to the mean cascade rates.…”

Section: Discussionsupporting

confidence: 80%

“…The comparison is strongly favourable in both solar maximum and solar minimum. At the present time, 20-40% of the energy cascade is available to heat heavy ions and electrons when the cascade is strong (wind speed and proton temperature are both high) and less when the cascade is weak [23], which is in agreement with empirical constraints [111].…”

Section: Third Moment Theorysupporting

confidence: 85%

See 1 more Smart Citation

Third-moment descriptions of the interplanetary turbulent cascade, intermittency and back transfer

Coburn

Forman

Smith

et al. 2015

Phil. Trans. R. Soc. A.

Self Cite

View full text Add to dashboard Cite

One contribution of 11 to a theme issue 'Dissipation and heating in solar wind turbulence' . We review some aspects of solar wind turbulence with an emphasis on the ability of the turbulence to account for the observed heating of the solar wind. Particular attention is paid to the use of structure functions in computing energy cascade rates and their general agreement with the measured thermal proton heating. We then examine the use of 1 h data samples that are comparable in length to the correlation length for the fluctuations to obtain insights into local inertial range dynamics and find evidence for intermittency in the computed energy cascade rates. When the magnetic energy dominates the kinetic energy, there is evidence of anti-correlation in the cascade of energy associated with the outward-and inward-propagating components that we can only partially explain.

show abstract

Section: Discussionsupporting

confidence: 80%

Section: Third Moment Theorysupporting

confidence: 85%

Third-moment descriptions of the interplanetary turbulent cascade, intermittency and back transfer

Coburn

Forman

Smith

et al. 2015

Phil. Trans. R. Soc. A.

Self Cite

View full text Add to dashboard Cite

show abstract

“…Some linear scaling of third-order structure functions is observed, 6 even though isotropy is not fully satisfied in the solar wind, [26][27][28] due to the presence of a strong large-scale magnetic field. 23,24 Other recent studies 7,29 have also extended the treatment of the third-order MHD laws to a form in which spectral anisotropy can be accommodated. In particular, MacBride et al 7 model the solar wind magnetic fluctuations as either an isotropic or a nonisotropic model ͑a mixture of one-dimensional and 2D fluctuations͒ when they evaluate heating rates using the homogeneous third-order law.…”

Section: Summary and Discussionmentioning

confidence: 99%

The third-order law for magnetohydrodynamic turbulence with shear: Numerical investigation

et al. 2010

View full text Add to dashboard Cite

The scaling laws of third-order structure functions for isotropic, homogeneous, and incompressible magnetohydrodynamic ͑MHD͒ turbulence relate the observable structure function with the energy dissipation rate. Recently ͓Wan et al. Phys. Plasmas 16, 090703 ͑2009͔͒, the theory was extended to the case in which a constant velocity shear is present, motivated by the application of the third-order law to the solar wind. We use direct numerical simulations of two-dimensional MHD with shear to confirm this new generalization of the theory. The presence of the shear effect broadens the circumstances in which the law can be applied. Important implications for laboratory and space plasmas are discussed.

show abstract

“…A turbulent energy cascade is believed to operate in the solar wind (Coleman 1968;Matthaeus et al 1982Matthaeus et al , 1998Zank et al 1996;Smith et al 2001Smith et al , 2006MacBride et al 2008;Breech et al 2009;Stawarz et al 2009Stawarz et al , 2011Coburn et al 2012Coburn et al , 2013Coburn et al , 2014Coburn et al , 2015Bruno & Carbone 2013). Spacecraft observations (Smith 2003a;Hamilton et al 2008;Horbury et al 2008;MacBride et al 2008;Chen et al 2010;Forman et al 2011;He et al 2011;Podesta & Gary 2011) and numerical simulations (Shebalin et al 1983;Goldstein et al 1995;Matthaeus et al 1996;Cho & Vishniac 2000;Müller & Grappin 2005;Boldyrev et al 2009;Beresnyak 2011) indicate that the turbulent cascade is preferentially perpendicular to the ambient magnetic field.…”

Section: Introductionmentioning

confidence: 99%

Statistical Analysis of the Magnetic Helicity Signature of the Solar Wind Turbulence at 1 Au

Markovskii

Vasquez

Smith

2015

ApJ

Self Cite

View full text Add to dashboard Cite

The absolute value of the magnetic helicity spectrum of the solar wind turbulence often has a peak at kinetic scales. This helicity signature is important for understanding the mechanism of the turbulent cascade. In this paper, a statistical analysis of the magnetic helicity is performed. For this purpose, a database of the solar wind intervals with the helicity signature was assembled using Wind spacecraft magnetic and plasma data. New statistically significant correlations between the magnetic helicity and the properties of the background plasma are found. The position of the signature within the spectrum depends on the proton gyroscale and the proton inertial scale. Possible mechanisms responsible for the observed trends are discussed. The helicity peak is interpreted as a result of two competing processes, one of which generates the helicity and the other one eliminates it.

show abstract

The Turbulent Cascade and Proton Heating in the Solar Wind at 1 Au

Cited by 140 publications

References 46 publications

Third-moment descriptions of the interplanetary turbulent cascade, intermittency and back transfer

Third-moment descriptions of the interplanetary turbulent cascade, intermittency and back transfer

The third-order law for magnetohydrodynamic turbulence with shear: Numerical investigation

Statistical Analysis of the Magnetic Helicity Signature of the Solar Wind Turbulence at 1 Au

Contact Info

Product

Resources

About