Kinetic Physics of the Solar Corona and Solar Wind

Marsch, E.

doi:10.12942/lrsp-2006-1

Cited by 675 publications

(622 citation statements)

References 267 publications

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“…At these small scales ion temperature anisotropy instabilities can occur Marsch 2006;Matteini et al 2007), and may remove energy from, or also inject it into, the turbulence.…”

Section: Ion Scale Instabilities Driven By Solar Wind Expansion and Cmentioning

confidence: 99%

Solar Wind Turbulence and the Role of Ion Instabilities

et al. 2013

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Solar wind is probably the best laboratory to study turbulence in astrophysical plasmas. In addition to the presence of magnetic field, the differences with neutral fluid isotropic turbulence are: (i) weakness of collisional dissipation and (ii) presence of several characteristic space and time scales. In this paper we discuss observational properties of solar wind turbulence in a large range from the MHD to the electron scales. At MHD scales, within the inertial range, turbulence cascade of magnetic fluctuations develops mostly in the plane perpendicular to the mean field, with the Kolmogorov scaling k −5/3 ⊥ for the perpendicular cascade and k −2 for the parallel one. Solar wind turbulence is compressible in nature: density fluctuations at MHD scales have the Kolmogorov spectrum. Velocity fluctuations do not follow magnetic field ones: their spectrum is a power-law with a −3/2 spectral index. Probability distribution functions of different plasma parameters are not Gaussian, indicating presence of intermittency. At the moment there is no global model taking into account all these observed properties of the inertial range. At ion scales, turbulent spectra have a break, compressibility increases and the density fluctuation spectrum has a local flattening. Around ion scales, magnetic spectra are variable and ion instabilities occur as a function of the local plasma parameters. Between ion and electron scales, a small scale turbulent cascade seems to be established. It is characterized by a well defined power-law spectrum in magnetic and density fluctuations with a spectral index close to −2.8. Approaching electron scales, the fluctuations are no more self-similar: an exponential cut-off is usually observed (for time intervals without quasi-parallel whistlers) indicating an onset of dissipation. The small scale inertial range between ion and electron scales and the electron dissipation range can be together described by ∼ k −α ⊥ exp(−k ⊥ d ), with α 8/3 and the dissipation scale d close to the electron Larmor radius d ρ e . The nature of this small scale cascade and a possible dissipation mechanism are still under debate.

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“…At these small scales ion temperature anisotropy instabilities can occur Marsch 2006;Matteini et al 2007), and may remove energy from, or also inject it into, the turbulence.…”

Section: Ion Scale Instabilities Driven By Solar Wind Expansion and Cmentioning

confidence: 99%

Solar Wind Turbulence and the Role of Ion Instabilities

et al. 2013

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“…More sophisticated, collisionless kinetic models cannot be applied to model large-scale structures in the solar corona since the considered scales are several orders of magnitude larger than the relevant (microscopic) scales which have to be resolved in kinetic simulations (e.g., the gyroradius or Debye-length). This approach, however, is frequently applied to model the solar wind plasma (see review by Marsch 2006). One approach to derive plasma quantities, which can then be compared to observations, is forward modeling aided by time-dependent MHD simulations (see Peter et al 2006).…”

Section: Mhd Models Of the Coronal Magnetic Fieldmentioning

confidence: 99%

“…We also do not discuss the role of the magnetic field and related physical processes far away from the Sun (beyond the solar corona) and its transport to those places. Here, we refer the interested reader to specialized reviews on the solar wind (Marsch 2006;Ofman 2010;Bruno and Carbone 2013), space weather (Schwenn 2006), and the heliospheric magnetic field (Owens and Forsyth 2013).…”

Section: Introductionmentioning

confidence: 99%

The magnetic field in the solar atmosphere

Wiegelmann

Thalmann

Solanki

2014

Astron Astrophys Rev

176

125

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This publication provides an overview of magnetic fields in the solar atmosphere with the focus lying on the corona. The solar magnetic field couples the solar interior with the visible surface of the Sun and with its atmosphere. It is also responsible for all solar activity in its numerous manifestations. Thus, dynamic phenomena such as coronal mass ejections and flares are magnetically driven. In addition, the field also plays a crucial role in heating the solar chromosphere and corona as well as in accelerating the solar wind. Our main emphasis is the magnetic field in the upper solar atmosphere so that photospheric and chromospheric magnetic structures are mainly discussed where relevant for higher solar layers. Also, the discussion of the solar atmosphere and activity is limited to those topics of direct relevance to the magnetic field. After giving a brief overview about the solar magnetic field in general and its global structure, we discuss in more detail the magnetic field in active regions, the quiet Sun and coronal holes.

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“…1, where the v x -v y level lines of the proton distribution function, integrated over v z and averaged over x in the spatial region of trapped particles, are reported. (Valentini et al 2008) The generation of these double peaked proton velocity distributions has been recovered in many "in situ" spacecraft observations in the solar wind (Gurnett et al 1979;Marsch et al 1982a;Marsch 2006). These results show that non-Maxwellian distribution functions with multiple peaks or bumps can be spontaneously created by the wave-particle interactions in the kinetic regime.…”

Section: Wave-particle Interaction At the Kinetic Scalesmentioning

confidence: 74%

“…The interstellar medium is generally observed from spacecraft measurements (Bruno and Carbone 2005;Marsch 2006) to be in a fully turbulent regime. Along the turbulent cascade, nonlinear local couplings transfer energy from low to high frequencies.…”

Section: Vlasov Simulationsmentioning

confidence: 99%

Nonclassical Transport and Particle-Field Coupling: from Laboratory Plasmas to the Solar Wind

Perrone

Dendy

Furno

et al. 2013

Space Sciences Series of ISSI

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Understanding transport of thermal and suprathermal particles is a fundamental issue in laboratory, solar-terrestrial, and astrophysical plasmas. For laboratory fusion experiments, confinement of particles and energy is essential for sustaining the plasma long enough to reach burning conditions. For solar wind and magnetospheric plasmas, transport properties determine the spatial and temporal distribution of energetic particles, which can be harmful for spacecraft functioning, as well as the entry of solar wind plasma into the magnetosphere. For astrophysical plasmas, transport properties determine the efficiency of particle acceleration processes and affect observable radiative signatures. In all cases, transport depends on the interaction of thermal and suprathermal particles with the electric and magnetic fluctuations in the plasma. Understanding transport therefore requires us to understand these interactions, which encompass a wide range of scales, from magnetohydrodynamic to kinetic scales, with larger scale structures also having a role. The wealth of transport studies during recent decades has shown the existence of a variety of regimes that differ from the classical quasilinear regime. In this paper we give an overview of nonclassical plasma transport regimes, discussing theoretical approaches to superdiffusive and subdiffusive transport, wave-particle interactions at microscopic kinetic scales, the influence of coherent structures and of avalanching transport, and the results of numerical simulations and experimental data analyses. Applications to laboratory plasmas and space plasmas are discussed.

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Kinetic Physics of the Solar Corona and Solar Wind

Cited by 675 publications

References 267 publications

Solar Wind Turbulence and the Role of Ion Instabilities

Solar Wind Turbulence and the Role of Ion Instabilities

The magnetic field in the solar atmosphere

Nonclassical Transport and Particle-Field Coupling: from Laboratory Plasmas to the Solar Wind

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