Radial evolution of power spectra of interplanetary Alfvénic turbulence

Bavassano, B.; Dobrowolny, M.; Mariani, F.; Ness, N. F.

doi:10.1029/ja087ia05p03617

Cited by 326 publications

(259 citation statements)

References 16 publications

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“…However, this is not the case in the Alfv6nic fluctuations in the inner heliosphere. As mentioned above, in the observed Alfv6nic turbulence the lowfrequency (around 10 -4 Hz) fluctuations do not decay, whereas the high-frequency (around 10 -3 Hz) fluctuations radially decay [Bavassano et al, 1982]. The heating rate or the cascading rate is associated with the decrease offc (see equation (1)).…”

Section: Discussion Of the Solar Wind Model Of Tumentioning

confidence: 96%

Comment on “Evolution of energy‐containing turbulent eddies in the solar wind” by W. H. Matthaeus, S. Oughton, D. H. Pontius Jr., and Y. Zhou

Tu¹,

Marsch²

1995

J. Geophys. Res.

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IntroductionIn a recent paper (hereinafter referred to as paper 1), Matthaeus et al. [1994, p. 19,268] argued that the lowfrequency fluctuations in the solar wind should be identified with the energy-containing turbulent eddies as described in normal HD turbulence theory [Batchelor, 1953]. According to this idea they claimed that it is necessary to consider the energy supplied by these eddies (resulting from their decay) in wave-driven models of the solar wind. They concluded that "the Tu

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Section: Discussion Of the Solar Wind Model Of Tumentioning

confidence: 96%

Comment on “Evolution of energy‐containing turbulent eddies in the solar wind” by W. H. Matthaeus, S. Oughton, D. H. Pontius Jr., and Y. Zhou

Tu¹,

Marsch²

1995

J. Geophys. Res.

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“…[36] Helios data are used as a guide for the range of reasonable values for the total fluctuation energy and cross helicity [e.g., Bavassano et al, 1982;Bruno and Dobrowolny, 1986] from 0.3 to 1 AU. Observational studies at 1 AU suggest that the quasi-2-D energy is ∼80% of the total fluctuation energy [Bieber et al, 1996;Horbury et al, 2008;Osman and Horbury, 2009;MacBride et al, 2010], and we use a similar partitioning to set Z 2 and W 2 here.…”

Section: Solutions With a Single Set Of Boundary Conditionsmentioning

confidence: 99%

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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“…Later, we shall provide evidence to support the association between doublepeaked proton velocity distributions and sunward propagating waves when we briefly discuss the effect on the solar wind due to a different e − /e + ratio. The power of the waves in the solar wind decreases with frequency, as indicated by the Helios measurements of the magnetic field spectra (Bavassano et al 1982;Denskat & Neubauer 1982). The dependence of the wave power on frequency can generally be described by a power law.…”

Section: Ion Cyclotron Resonant Heatingmentioning

confidence: 99%

“…The dependence of the wave power on frequency can generally be described by a power law. It was also found that the wave power decreases with radial distance, and the dependence can also be described by a power law, at least in the observed regime (Bavassano et al 1982). In our model, we assume a magnetic field power spectrum based on these experimental results.…”

Section: Ion Cyclotron Resonant Heatingmentioning

confidence: 99%

“…Recently, Chang (2002) has suggested that such type of intermittent turbulence may be associated with the "complexity" generated by the sporadic localized mergings and interactions of the coherent magnetic structures near the coronal holes. Measurements of the power spectra of these waves by the Helios spacecraft indicated that the wave power decreases with frequency (Bavassano et al 1982;Denskat & Neubauer 1982). Note that the alpha particles have a lower gyrofrequency than the protons.…”

Section: Introductionmentioning

confidence: 99%

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Comparison of the effects of wave-particle interactions and the kinetic suprathermal electron population on the acceleration of the solar wind

Tam

Chang

2002

A&A

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Abstract. Kinetic effects due to wave-particle interactions and suprathermal electrons have been suggested in the literature as possible solar wind acceleration mechanisms. Ion cyclotron resonant heating, in particular, has been associated with some qualitative features observed in the solar wind. In terms of solar wind acceleration, however, it is interesting to compare the kinetic effects of suprathermal electrons with those due to the wave-particle interactions. The combined effects of the two acceleration mechanisms on the fast solar wind have been studied by Tam & Chang (1999a,b). In this study, we investigate the role of the suprathermal electron population in the acceleration of the solar wind. Our model follows the global kinetic evolution of the fast solar wind under the influence of ion cyclotron resonant heating, while taking into account Coulomb collisions, and the ambipolar electric field that is consistent with the particle distributions themselves. The kinetic effects due to the suprathermal electrons, which we define to be the tail of the electron distributions, can be included in the model as an option. By comparing the results with and without the inclusion of the suprathermal electron effects, we determine the relative importance of suprathermal electrons and wave-particle interactions in driving the solar wind. We find that although suprathermal electrons enhance the ambipolar electric potential in the solar wind considerably, their overall influence as an acceleration mechanism is relatively insignificant in a wave-driven solar wind.

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Radial evolution of power spectra of interplanetary Alfvénic turbulence

Cited by 326 publications

References 16 publications

Comment on “Evolution of energy‐containing turbulent eddies in the solar wind” by W. H. Matthaeus, S. Oughton, D. H. Pontius Jr., and Y. Zhou

Comment on “Evolution of energy‐containing turbulent eddies in the solar wind” by W. H. Matthaeus, S. Oughton, D. H. Pontius Jr., and Y. Zhou

Transport of solar wind fluctuations: A two-component model

Comparison of the effects of wave-particle interactions and the kinetic suprathermal electron population on the acceleration of the solar wind

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