Electromagnetic proton/proton instabilities in the solar wind: Simulations

Daughton, W.; Gary, S. Peter; Winske, D.

doi:10.1029/1998ja900105

Cited by 93 publications

(101 citation statements)

References 32 publications

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“…To eliminate the beam influence on our analysis we just used the beta of the core here. This restriction is also suggested by the theoretical stability analyses (Daughton and Gary, 1998;Daughton et al, 1999).…”

Section: Data Analysis Proceduresmentioning

confidence: 97%

“…A general account of space-plasma microinstabilities was given in the book by Gary (1993). Furthermore, Daughton and Gary (1998) and Daughton et al (1999) provided arguments from analytic instability calculations and from direct numerical simulations, which indicated that the beam velocity is regulated by electromagnetic instabilities driven by the beam kinetic energy, a process in which the core β is a key parameter. Dum et al (1980) found evidence for wave growth from the detailed measured VDFs, and so did Leubner and Viñas (1986) for double-peaked proton VDFs.…”

Section: Temperature Anisotropy Driven Instabilitiesmentioning

confidence: 99%

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Limits on the core temperature anisotropy of solar wind protons

Marsch

Zhao

2006

Ann. Geophys.

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Abstract.We analyse the temperature anisotropy of the protons in the solar wind and thereby concentrate on plasma data obtained in the year 1976 of the Helios 1 and Helios 2 missions. We derive the core proton temperatures T ⊥ and T , in the directions perpendicular and parallel to the magnetic field, as well as the core parallel plasma beta, β . The data are separately analysed for two distance ranges, R≤0.4 AU and R>0.4 AU, and divided into 24 bins for the plasma beta, in the range from β =0.1 to β =10, and into 72 bins for the total temperature anisotropy, A=1−T ⊥ /T , which is here considered in the range from −0.9 to 0.9. The number of spectra in each bin is determined to obtain distributions. The statistical results are presented in two-dimensional histograms. For each column we define a critical upper and lower limit of the anisotropy. The resulting empirical points are compared with the known theoretical instability thresholds. The protons are found to come with increasing radial distance closer to the fire-hose instability threshold.

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Section: Data Analysis Proceduresmentioning

confidence: 97%

Section: Temperature Anisotropy Driven Instabilitiesmentioning

confidence: 99%

Limits on the core temperature anisotropy of solar wind protons

Marsch

Zhao

2006

Ann. Geophys.

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“…These results may have important applications. For example, [17] using hybrid simulations for a solar wind type plasma showed that the ion beam instability leads to a proton beam anisotropy Figs. 2a and 4a].…”

Section: Discussionmentioning

confidence: 99%

“…Studies have been carried out by [14,15,16], including the effects of dissipation and of the beam drift speed. The effect and the evolution of the beam for right and left handed polarized waves, have also been studied by using simulation experiments [17]. These studies have considered linearly stable systems [9,10,14,15,16].…”

Section: Introductionmentioning

confidence: 99%

Behavior of linear beam-plasma instabilities in the presence of finite amplitude circularly polarized waves

Gomberoff¹,

Hoyos²,

Brinca³

2004

Braz. J. Phys.

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We review the effect of finite amplitude circularly polarized waves on the behavior of linear ion-beam plasma instabilities. It has been shown that left-hand polarized waves can stabilize linear right-handed instabilities [1]. It has also been shown that for beam velocities capable of destabilizing left-handed waves, left-hand polarized large amplitude waves can also stabilize these waves. On the other hand, when the large amplitude wave is right-hand polarized, they can either stabilize or destabilize right-handed instabilities depending on the wave frequency and beam speed [2]. Finally, we show that the presence of large amplitude left-hand polarized waves can also trigger electrostatic ion-acoustic instabilities by forcing the phase velocities of two ion acoutic waves to become equal, above a threshold amplitude value.

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“…The hybrid code is a robust, well-documented simulation tool which has been used to study various electromagnetic ion instabilities (McKean et al, 1994;Gary et al, 1997;Daughton et al, 1999;Gary et al, 2000Gary et al, , 2001Gary et al, , 2003Ofman et al, 2001;Xie et al, 2004;Ofman and Viñas, 2007;Ofman, 2010a). Both 1-D and 2-D hybrid codes solve for the full three components of velocity for the ions; the critical difference between the two types of codes is in the dimensionality of the magnetic field fluctuation solver.…”

Section: Hybrid Model Of Solar Wind Plasmamentioning

confidence: 99%

Hybrid models of solar wind plasma heating

2011

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Abstract. Remote sensing and in-situ observations show that solar wind ions are often hotter than electrons, and the heavy ions flow faster than the protons by up to an Alfvén speed. Turbulent spectrum of Alfvénic fluctuations and shocks were detected in solar wind plasma. Cross-field inhomogeneities in the corona were observed to extend to several tens of solar radii from the Sun. The acceleration and heating of solar wind plasma is studied via 1-D and 2-D hybrid simulations. The models describe the kinetics of protons and heavy ions, and electrons are treated as neutralizing fluid.The expansion of the solar wind is considered in 1-D hybrid model. A spectrum of Alfvénic fluctuations is injected at the computational boundary, produced by differential streaming instability, or initial ion temperature anisotropy, and the parametric dependence of the perpendicular heating of H + -He ++ solar wind plasma is studied. It is found that He ++ ions are heated efficiently by the Alfvénic wave spectrum below the proton gyroperiod.

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Electromagnetic proton/proton instabilities in the solar wind: Simulations

Cited by 93 publications

References 32 publications

Limits on the core temperature anisotropy of solar wind protons

Limits on the core temperature anisotropy of solar wind protons

Behavior of linear beam-plasma instabilities in the presence of finite amplitude circularly polarized waves

Hybrid models of solar wind plasma heating

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