Electron and proton heating by solar wind turbulence

Breech, B.; Matthaeus, W. H.; Cranmer, Steven R.; Kasper, J. C.; Oughton, Sean

doi:10.1029/2009ja014354

Cited by 99 publications

(107 citation statements)

References 47 publications

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“…Assuming that there is scale separation between the fluctuations and the large-scale fields, transport equations for general incompressible fluctuations can be readily derived [Zhou and Matthaeus, 1990;Zank et al, 1996;Matthaeus et al, 1996;Tu and Marsch, 1993]. A comprehensive derivation and discussion of the approximations used is given by Breech et al [2008].…”

Section: Transport Modelmentioning

confidence: 99%

“…Since much of this development parallels that of the single-component models, we refer readers desiring more details to a study by Breech et al [2008], which contains a thorough account of the derivation of (singlecomponent) transport equations for incompressible solar wind fluctuations. It is, however, helpful to list some key approximations used in developing the model: (1) scale separation between the fluctuations and the background fields, (2) locally incompressible fluctuations, (3) large-scale fields specified and time steady (density r, wind speed U, Alfvén speed V A ), with U ) V A , (4) assumption that largescale gradients are in the radial direction, and (5) assumption that turbulent decay leads to proton heating.…”

Section: Modelmentioning

confidence: 99%

“…It is, however, helpful to list some key approximations used in developing the model: (1) scale separation between the fluctuations and the background fields, (2) locally incompressible fluctuations, (3) large-scale fields specified and time steady (density r, wind speed U, Alfvén speed V A ), with U ) V A , (4) assumption that largescale gradients are in the radial direction, and (5) assumption that turbulent decay leads to proton heating. See the work of Breech et al [2008] for detailed discussion of the approximations and simplifications used.…”

Section: Modelmentioning

confidence: 99%

“…Subsequent observational studies indicated that at magnetohydrodynamic (MHD) scales there are at least two distinct types of fluctuation and that the wave-like energy may be a minor component Bieber et al, 1996;Milano et al, 2004;Dasso et al, 2005;Horbury et al, 2005Horbury et al, , 2008Podesta, 2009;Osman and Horbury, 2009;Narita et al, 2010]. This encouraged development of more complete transport theories for the energy-containing range quantities [e.g., Tu and Marsch, 1993;Matthaeus et al, 1994Matthaeus et al, , 1996Matthaeus et al, , 1999Matthaeus et al, , 2004Zank et al, 1996;Smith et al, 2001Smith et al, , 2006Isenberg et al, 2003Isenberg et al, , 2010aIsenberg, 2005;Breech et al, 2005Breech et al, , 2008Yokoi and Hamba, 2007;Usmanov and Goldstein, 2010;Ng et al, 2010], in which turbulence properties are built in, contrasting with WKB theory, in which the waves are noninteracting at leading order. The agreement between observations made from 0.3 to 80 AU and numerical solutions to these models has also improved, with reasonable accord achieved for the radial evolution of the energy, cross helicity (H c ), and correlation length of the fluctuations and also for the proton temperature.…”

Section: Introductionmentioning

confidence: 99%

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Transport of solar wind fluctuations: A two-component model

et al. 2011

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[1] We present a new model for the transport of solar wind fluctuations which treats them as two interacting incompressible components: quasi-two-dimensional turbulence and a wave-like piece. Quantities solved for include the energy, cross helicity, and characteristic transverse length scale of each component, plus the proton temperature. The development of the model is outlined and numerical solutions are compared with spacecraft observations. Compared to previous single-component models, this new model incorporates a more physically realistic treatment of fluctuations induced by pickup ions and yields improved agreement with observed values of the correlation length, while maintaining good observational accord with the energy, cross helicity, and temperature.

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Section: Transport Modelmentioning

confidence: 99%

Section: Modelmentioning

confidence: 99%

Section: Modelmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Transport of solar wind fluctuations: A two-component model

et al. 2011

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“…Breech et al 2009). The nonlinear dynamics of the the CR-driven magnetic fluctuations in the shock precursor deserves thorough modeling.…”

Section: Collisionless Heating Of Ions and Electrons By Magnetic Turbmentioning

confidence: 99%

Collisionless Shocks in Partly Ionized Plasma with Cosmic Rays: Microphysics of Non-thermal Components

Bykov

Malkov

Raymond

et al. 2013

Microphysics of Cosmic Plasmas

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In this review we discuss some observational aspects and theoretical models of astrophysical collisionless shocks in partly ionized plasma with the presence of nonthermal components. A specific feature of fast strong collisionless shocks is their ability to accelerate energetic particles that can modify the shock upstream flow and form the shock precursors. We discuss the effects of energetic particle acceleration and associated magnetic field amplification and decay in the extended shock precursors on the line and continuum multi-wavelength emission spectra of the shocks. Both Balmer-type and radiative astrophysical shocks are discussed in connection to supernova remnants interacting with partially neutral clouds. Quantitative models described in the review predict a number of observable line-like emission features that can be used to reveal the physical state of the matter in the shock precursors and the character of nonthermal processes in the shocks. Implications of recent progress of gamma-ray observations of supernova remnants in molecular clouds are highlighted.

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A new stationary analytical model of the heliospheric current sheet and the plasma sheet

2015

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We develop a single‐fluid 2‐D analytical model of the axially symmetric thin heliospheric current sheet (HCS) embedded into the heliospheric plasma sheet (HPS). A HCS‐HPS system has a shape of a relatively thin plasma disk limited by separatrices that also represent current sheets, which is in agreement with Ulysses observations in the aphelion, when it crossed the HCS perpendicular to its plane. Our model employs a differential rotation of the solar photosphere that leads to unipolar induction in the corona. Three components of the interplanetary magnetic field (IMF), the solar wind speed, and the thermal pressure are taken into account. Solar corona conditions and a HCS‐HPS system state are tied by boundary conditions and the “frozen‐in” equation. The model allows finding spatial distributions of the magnetic field, the speed within the HPS, and electric currents within the HCS. An angular plasma speed is low within the HPS due to the angular momentum conservation (there is no significant corotation with the Sun), which is consistent with observations. We found that the HPS thickness L decreases with distance r, becoming a constant far from the Sun (L ~2.5 solar radii (R0) at 1 AU). Above the separatrices and at large heliocentric distances, the solar wind behavior obeys Parker's model, but the magnetic field spiral form may be different from Parker's one inside the HPS. At r ≤ 245 R0, the IMF spiral may undergo a turn simultaneously with a change of the poloidal current direction (from sunward to antisunward).

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Electron and proton heating by solar wind turbulence

Cited by 99 publications

References 47 publications

Transport of solar wind fluctuations: A two-component model

Transport of solar wind fluctuations: A two-component model

Collisionless Shocks in Partly Ionized Plasma with Cosmic Rays: Microphysics of Non-thermal Components

A new stationary analytical model of the heliospheric current sheet and the plasma sheet

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