Two-Dimensional Kinetic Turbulence in the Solar Wind

Journal Article · Fri May 21 00:00:00 EDT 2010 · Physical Review Letters

DOI:https://doi.org/10.1103/PHYSREVLETT.104.205002· OSTI ID:21410687

Valentini, F ^[1]; Califano, F ^[1]; Veltri, P ^[2]

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1. Dipartimento di Fisica and CNISM, Universita di Pisa, 56127 Pisa (Italy)
2. Dipartimento di Fisica and CNISM, Universita della Calabria, 87036 Rende (Italy)

We present the first 2D hybrid-Vlasov simulations of turbulence in the solar wind that describe the evolution of the energy spectra in a range of two decades of wavelengths around the ion inertial scale. Several previous magnetohydrodynamics and particle-in-cell simulations in the range of large (fluid) wavelengths showed a marked anisotropy of the energy spectra in the direction perpendicular to the mean magnetic field. Here we give evidence that the parallel direction can also be a privileged way for turbulence to develop towards short scales, where kinetic effects govern the plasma dynamics.

• OSTI ID: 21410687
• Journal Information: Physical Review Letters, Vol. 104, Issue 20; Other Information: DOI: 10.1103/PhysRevLett.104.205002; (c) 2010 The American Physical Society; ISSN 0031-9007
• Country of Publication: United States
• Language: English

Related Subjects

70 PLASMA PHYSICS AND FUSION TECHNOLOGY
71 CLASSICAL AND QUANTUM MECHANICS
GENERAL PHYSICS
ANISOTROPY
BOLTZMANN-VLASOV EQUATION
ENERGY SPECTRA
IONS
MAGNETIC FIELDS
MAGNETOHYDRODYNAMICS
PLASMA
SOLAR WIND
TURBULENCE
TWO-DIMENSIONAL CALCULATIONS
WAVELENGTHS
CHARGED PARTICLES
DIFFERENTIAL EQUATIONS
EQUATIONS
FLUID MECHANICS
HYDRODYNAMICS
MECHANICS
PARTIAL DIFFERENTIAL EQUATIONS
SOLAR ACTIVITY
SPECTRA
STELLAR ACTIVITY
STELLAR WINDS