Radial Dependence of the Frequency Break Between Fluid and Kinetic Scales in the Solar Wind Fluctuations

Bruno, R.; Trenchi, Lorenzo

doi:10.1088/2041-8205/787/2/l24

Cited by 124 publications

(118 citation statements)

References 32 publications

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“…Bourouaine et al (2012), while taking into account the two-dimensional nature of the turbulent fluctuations and their Doppler shifts in the solar wind, concluded from an analysis of the spectral break in turbulence spectra that the proton inertial length d p is the most relevant microscopic scale (and not the proton gyroradius) at which turbulence dissipation appears to take place. In a recent observational attempt to better identify the turbulence dissipation scale, it was found that the dependence on the radial distance r of the wavenumber corresponding to the break in the observed frequency spectra is of the kind k~-r 1.08 (Bruno & Trenchi 2014). This behavior was judged to be in good agreement with that of the wavenumber derived from the linear resonance condition for proton-cyclotron damping, which can be written as…”

Section: Revisiting Slow Modementioning

confidence: 64%

Kinetic Slow Mode in the Solar Wind and Its Possible Role in Turbulence Dissipation and Ion Heating

Narita

Marsch

2015

ApJ

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The solar wind is permeated by various kinds of fluctuations ranging broadly in scales from those of the solar corona and inner heliosphere down to the local ion and electron plasma kinetic scales. The question of what rules the dissipation of magnetohydrodynamic (MHD) turbulence in the solar wind has not conclusively been answered, but remains a key research topic of space plasma physics. Here we propose a new dissipation mechanism, the proton Landau damping of the quasi-perpendicular kinetic slow mode. This mode is linked to the oblique MHD slow mode, yet has shorter wavelengths going down to the proton inertial length. The kinetic slow mode can be separated from the kinetic Alfvén mode by the Alfvén resonance parameter, the proton Landau resonance parameter, the magnetic compressibility, and the electric field polarization. Numerical simulations and in situ observations indicate that the MHD turbulent cascade preferably transfers energy in the direction perpendicular to the background magnetic field. If the kinetic slow mode is also generated and replenished by the energy cascade, this mode can lead to both perpendicular and parallel heating of the protons.

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Section: Revisiting Slow Modementioning

confidence: 64%

Kinetic Slow Mode in the Solar Wind and Its Possible Role in Turbulence Dissipation and Ion Heating

Narita

Marsch

2015

ApJ

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“…On the other hand, Bruno & Trenchi [42], using a combination of MESSENGER, Wind and Ulysses data during radial alignments of the satellites, concluded that there was a clear radial dependence, i.e. f b ∼ R −1.09 , and showed good agreement between the scaling of the observed break wavenumber and the scaling of the wavenumber corresponding to the resonance condition for parallel-propagating Alfvén waves [40], a result consistent neither with the damping of kinetic Alfvén waves [76] nor with Hall MHD effects [84,85].…”

Section: (B) Dissipationmentioning

confidence: 99%

Kinetic scale turbulence and dissipation in the solar wind: key observational results and future outlook

Goldstein

Wicks

Perri

et al. 2015

Phil. Trans. R. Soc. A.

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One contribution of 11 to a theme issue 'Dissipation and heating in solar wind turbulence' . Turbulence is ubiquitous in the solar wind. Turbulence causes kinetic and magnetic energy to cascade to small scales where they are eventually dissipated, adding heat to the plasma. The details of how this occurs are not well understood. This article reviews the evidence for turbulent dissipation and examines various diagnostics for identifying solar wind regions where dissipation is occurring. We also discuss how future missions will further enhance our understanding of the importance of turbulence to solar wind dynamics.

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“…We assume that the inner scale l i is given by the proton inertial length (Verma et al 1996;Leamon et al 1999Leamon et al , 2000Smith et al 2001;Chen et al 2014;Bruno & Trenchi 2014), which is related to the background electron density by…”

Section: Background Electron Density and The Inner Scalementioning

confidence: 99%

Turbulent Density Fluctuations and Proton Heating Rate in the Solar Wind from 9–20 R_⊙

Raja

Subramanian

Ramesh

et al. 2017

ApJ

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We obtain scatter-broadened images of the Crab nebula at 80 MHz as it transits through the inner solar wind in June 2016 and 2017. These images are anisotropic, with the major axis oriented perpendicular to the radially outward coronal magnetic field. Using these data, we deduce that the density modulation index (δN e /N e ) caused by turbulent density fluctuations in the solar wind ranges from 1.9 ×10 −3 to 7.7 ×10 −3 between 9 -20 R ⊙ . We also find that the heating rate of solar wind protons at these distances ranges from 2.2 × 10 −13 to 1.0 × 10 −11 erg cm −3 s −1 . On two occasions, the line of sight intercepted a coronal streamer. We find that the presence of the streamer approximately doubles the thickness of the scattering screen.

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Radial Dependence of the Frequency Break Between Fluid and Kinetic Scales in the Solar Wind Fluctuations

Cited by 124 publications

References 32 publications

Kinetic Slow Mode in the Solar Wind and Its Possible Role in Turbulence Dissipation and Ion Heating

Kinetic Slow Mode in the Solar Wind and Its Possible Role in Turbulence Dissipation and Ion Heating

Kinetic scale turbulence and dissipation in the solar wind: key observational results and future outlook

Turbulent Density Fluctuations and Proton Heating Rate in the Solar Wind from 9–20 R_⊙

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Radial Dependence of the Frequency Break Between Fluid and Kinetic Scales in the Solar Wind Fluctuations

Cited by 124 publications

References 32 publications

Kinetic Slow Mode in the Solar Wind and Its Possible Role in Turbulence Dissipation and Ion Heating

Kinetic Slow Mode in the Solar Wind and Its Possible Role in Turbulence Dissipation and Ion Heating

Kinetic scale turbulence and dissipation in the solar wind: key observational results and future outlook

Turbulent Density Fluctuations and Proton Heating Rate in the Solar Wind from 9–20 R⊙

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Turbulent Density Fluctuations and Proton Heating Rate in the Solar Wind from 9–20 R_⊙