Sorriso-Valvo<i>et al.</i>Reply:

Sorriso‐Valvo, L.; Carbone, V.; Marino, Raffaele; Noullez, A.; Bruno, R.; Veltri, P.

doi:10.1103/physrevlett.104.189002

Cited by 73 publications

(93 citation statements)

References 8 publications

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“…Relation (2) was already ob-‫ע‬ e served in the inertial range of two-dimensional numerical simulations of MHD equations (Sorriso-Valvo et al 2002), but has been verified only recently in solar wind turbulence (MacBride et al 2005;Sorriso-Valvo et al 2007). In order to find the scaling relation (2), it was necessary to avoid, as far as possible, variations of the solar activity and ecliptic disturbances (slow wind sources, coronal mass ejections, ecliptic current sheet, etc.…”

Section: ϫ1 ϫ1mentioning

confidence: 95%

Heating the Solar Wind by a Magnetohydrodynamic Turbulent Energy Cascade

Marino

Sorriso‐Valvo²,

Carbone

et al. 2008

ApJ

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139

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Section: ϫ1 ϫ1mentioning

confidence: 95%

Heating the Solar Wind by a Magnetohydrodynamic Turbulent Energy Cascade

Marino

Sorriso‐Valvo²,

Carbone

et al. 2008

ApJ

Self Cite

139

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“…Of course, the presence of Yaglom's law generates some controversial questions about data selection, reliability and a brief discussion on the extension of the inertial range. The interested reader can find some questions and relative answers in Physical Review Letters (Forman et al, 2010;Sorriso-Valvo et al, 2010a). In this section, we present a reasoned look at the main aspect of what has been reported in literature about the problem of intermittency in the solar wind turbulence.…”

Section: Living Reviews In Solar Physicsmentioning

confidence: 98%

The Solar Wind as a Turbulence Laboratory

Bruno

Carbone

2013

Living Rev. Solar Phys.

951

957

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In this review we will focus on a topic of fundamental importance for both astrophysics and plasma physics, namely the occurrence of large-amplitude low-frequency fluctuations of the fields that describe the plasma state. This subject will be treated within the context of the expanding solar wind and the most meaningful advances in this research field will be reported emphasizing the results obtained in the past decade or so. As a matter of fact, Helios inner heliosphere and Ulysses' high latitude observations, recent multi-spacecrafts measurements in the solar wind (Cluster four satellites) and new numerical approaches to the problem, based on the dynamics of complex systems, brought new important insights which helped to better understand how turbulent fluctuations behave in the solar wind. In particular, numerical simulations within the realm of magnetohydrodynamic (MHD) turbulence theory unraveled what kind of physical mechanisms are at the basis of turbulence generation and energy transfer across the spectral domain of the fluctuations. In other words, the advances reached in these past years in the investigation of solar wind turbulence now offer a rather complete picture of the phenomenological aspect of the problem to be tentatively presented in a rather organic way.

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“…The drawback of this approach is that, since the sign of ε can vary within the inertial range as can be seen in Figure 17 and in e.g. in Sorriso-Valvo et al (2007), the choice of the value of τ may influence the conclusion regarding the nature (direct versus inverse) of the turbulent cascade. Figure 18 shows the histogram of ε I computed using PP98 at different values of τ .…”

Section: Mean Value Of Cascade Rate and Sign Changementioning

confidence: 99%

Energy Cascade Rate in Compressible Fast and Slow Solar Wind Turbulence

Hadid

Sahraoui

Galtier

2017

ApJ

102

142

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Estimation of the energy cascade rate in the inertial range of solar wind turbulence has been done so far mostly within the incompressible magnetohydrodynamics (MHD) theory. Here, we go beyond that approximation to include plasma compressibility using a reduced form of a recently derived exact law for compressible, isothermal MHD turbulence. Using in-situ data from the THEMIS/ARTEMIS spacecraft in the fast and slow solar wind, we investigate in detail the role of the compressible fluctuations in modifying the energy cascade rate with respect to the prediction of the incompressible MHD model. In particular, we found that the energy cascade rate: i) is amplified particularly in the slow solar wind; ii) exhibits weaker fluctuations in spatial scales, which leads to a broader inertial range than the previous reported ones; iii) has a power law scaling with the turbulent Mach number; iv) has a lower level of spatial anisotropy. Other features of solar wind turbulence are discussed along with their comparison with previous studies that used incompressible or heuristic (non exact) compressible MHD models.

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Sorriso-Valvoet al.Reply:

Cited by 73 publications

References 8 publications

Heating the Solar Wind by a Magnetohydrodynamic Turbulent Energy Cascade

Heating the Solar Wind by a Magnetohydrodynamic Turbulent Energy Cascade

The Solar Wind as a Turbulence Laboratory

Energy Cascade Rate in Compressible Fast and Slow Solar Wind Turbulence

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