2006
DOI: 10.1086/499398
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Dissipation of the Perpendicular Turbulent Cascade in the Solar Wind

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Cited by 84 publications
(73 citation statements)
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“…These effects are associated typically with coherent structures such as magnetic structures. Indeed, intense kinetic activity is often found in the general proximity to strong gradients, including not only magnetic, but also strong density and velocity gradients [16,[55][56][57][58][59][60]. In particular, Refs.…”
Section: A Energy Conversion Related To Coherent Structuresmentioning
confidence: 99%
See 1 more Smart Citation
“…These effects are associated typically with coherent structures such as magnetic structures. Indeed, intense kinetic activity is often found in the general proximity to strong gradients, including not only magnetic, but also strong density and velocity gradients [16,[55][56][57][58][59][60]. In particular, Refs.…”
Section: A Energy Conversion Related To Coherent Structuresmentioning
confidence: 99%
“…The turbulence in most astrophysical contexts, on the other hand, is typically of weak collisionality, and frequently modeled as collisionless, and thus collisional (viscous and resistive) dissipation at small scales cannot emerge immediately. While various specific processes may contribute to conversion of energy from fields into random degrees of freedom, for example, wave-particle interactions (WPI) [16][17][18][19][20] and processes associated with coherent structures (CS) [21][22][23][24][25][26], are likely ingredients, but nevertheless an explicit dissipation function cannot at this moment be defined clearly for a collisionless system.…”
Section: Introductionmentioning
confidence: 99%
“…Since both the Kolmogorov and IK cascade timescales (∝ k −2/3 and k −1/2 , respectively) decline with increasing k (or decreasing spatial scales) more slowly than the periods of MHD waves (∝ k −1 ), the turbulence may be better described as spectra of waves at higher values of ks (smaller spatial scales), which play a critical role in the energizing of low-energy background particles. However, at such high values of ks one may be stepping beyond the MHD regime and must use more complex dispersion relations to take into account the kinetic effects and the anisotropy of the turbulence properly (Leamon et al 1998;Markovskii et al 2006).…”
Section: Introductionmentioning
confidence: 99%
“…The difficulty is to explain how the energy gets into the high-frequency waves: on small scales, the energy is known to be at lower frequencies (Howes et al 2006). Among the possible mechanisms for transferring the energy to the high frequencies (the sources of coronal heating) are reconnection (e.g., Matthaeus et al 2003), heat-flux-driven plasma instabilities (e.g., Markovskii et al 2006), and MHD turbulence (e.g., Matthaeus et al 1999;Chandran 2005). Rappazzo et al (2007) performed high-resolution simulations of MHD turbulence in a coronal loop described by reduced MHD equations.…”
mentioning
confidence: 99%