Introduction

Balogh, A.; Gosling, J. T.; Jokipii, J. R.; Kallenbach, R.; Kunow, H.

doi:10.1007/978-94-017-1179-1_1

Cited by 12 publications

(11 citation statements)

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“…The original work on CIR formation and its shocks can be found in Smith and Wolfe (1976). More recent discussion can be found in Pizzo (1985) and Balogh et al (2002).…”

Section: Historical Perspective Of Some Interplanetary Plasma Featuresmentioning

confidence: 99%

Nonlinear Alfvén waves, discontinuities, proton perpendicular acceleration, and magnetic holes/decreases in interplanetary space and the magnetosphere: intermediate shocks?

Tsurutani

Lakhina

Pickett

et al. 2005

Nonlin. Processes Geophys.

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Abstract. Alfvén waves, discontinuities, proton perpendicular acceleration and magnetic decreases (MDs) in interplanetary space are shown to be interrelated. Discontinuities are the phase-steepened edges of Alfvén waves. Magnetic decreases are caused by a diamagnetic effect from perpendicularly accelerated (to the magnetic field) protons. The ion acceleration is associated with the dissipation of phasesteepened Alfvén waves, presumably through the Ponderomotive Force. Proton perpendicular heating, through instabilities, lead to the generation of both proton cyclotron waves and mirror mode structures. Electromagnetic and electrostatic electron waves are detected as well. The Alfvén waves are thus found to be both dispersive and dissipative, conditions indicting that they may be intermediate shocks. The resultant "turbulence" created by the Alfvén wave dissipation is quite complex. There are both propagating (waves) and nonpropagating (mirror mode structures and MDs) byproducts. Arguments are presented to indicate that similar processes associated with Alfvén waves are occurring in the magnetosphere. In the magnetosphere, the "turbulence" is even further complicated by the damping of obliquely propagating proton cyclotron waves and the formation of electron holes, a form of solitary waves. Interplanetary Alfvén waves are shown to rapidly phase-steepen at a distance of 1 AU from the Sun. A steepening rate of ∼35 times per wavelength is indicated by Cluster-ACE measurements. Interplanetary (reverse) shock compression of Alfvén waves is noted to cause the rapid formation of MDs on the sunwardCorrespondence to: B. T. Tsurutani (bruce.tsurutani@jpl.nasa.gov) side of corotating interaction regions (CIRs). Although much has been learned about the Alfvén wave phase-steepening processfrom space plasma observations, many facets are still not understood. Several of these topics are discussed for the interested researcher. Computer simulations and theoretical developments will be particularly useful in making further progress in this exciting new area.

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“…The original work on CIR formation and its shocks can be found in Smith and Wolfe (1976). More recent discussion can be found in Pizzo (1985) and Balogh et al (2002).…”

Section: Historical Perspective Of Some Interplanetary Plasma Featuresmentioning

confidence: 99%

Nonlinear Alfvén waves, discontinuities, proton perpendicular acceleration, and magnetic holes/decreases in interplanetary space and the magnetosphere: intermediate shocks?

Tsurutani

Lakhina

Pickett

et al. 2005

Nonlin. Processes Geophys.

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“…Pick-up ions in the supersonic solar wind are selectively accelerated in co-rotating interaction regions (Balogh et al 1999) and at interplanetary coronal mass ejections (Bamert et al 2002). Even in the quiet solar wind, undisturbed by interplanetary shocks, ubiquitous suprathermal tails in the pick-up ion distributions are observed (Gloeckler 2003), (Fig.…”

Section: Pre-acceleration Of Suprathermal Ions In the Supersonic Solamentioning

confidence: 99%

On the “injection problem” at the solar wind termination shock

Kallenbach

Hilchenbach

Chalov

et al. 2005

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Abstract. This article presents an integrated analytical model on the injection efficiencies of the different ion species of the Anomalous component of the Cosmic Rays (ACRs) at the solar wind termination shock. We find that the injection into diffusive (first-order Fermi) acceleration is dominated by parallel ion diffusion and not by perpendicular diffusion unless the angle Ψ between the shock normal and the heliospheric magnetic field is almost exactly 90 • (89.3 • < Ψ ≈ 90 • ). In steady state the threshold speed for injection into first-order Fermi acceleration at a not exactly perpendicular solar wind termination shock -with the Parker shock angle Ψ ≈ 89.3 • -adjusts itself self-consistently. Increased anisotropic ACR flux amplifies Alfvénic turbulence which in turn suppresses parallel diffusion. It therefore increases the injection threshold and decreases the ACR flux until equilibrium is reached. For this equilibrium situation, we estimate the injection efficiencies of different species of suprathermal ions at the termination shock. We consider the following pre-acceleration processes: 1) momentum diffusion in compressional (ion-acoustic and magnetosonic) turbulence in the upstream supersonic solar wind and adiabatic cooling during convection to the termination shock; 2) reflection, transmission, and acceleration in the electric potential of the termination shock; and 3) momentum diffusion (stochastic or second-order Fermi acceleration) in the subsonic solar wind downstream of the termination shock in the inner heliosheath region. Our model results are compared to data from instruments on board the SOHO, ACE, Ulysses, and Voyager spacecraft.

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“…Much work has been done on Corotating Interaction Regions (CIRs), see e.g. Balogh et al (1999). Apart from the actual impact of CIRs on the solar wind plasma environment, the influence of CIRs on energetic particle populations has been of special interest.…”

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The influence of CIRs on the energetic electron flux at 1 AU

Kissmann

Fichtner

Ferreira

2004

A&A

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Abstract. Much work has been done on Corotating Interaction Regions (CIRs), see e.g. Balogh et al. (1999). Apart from the actual impact of CIRs on the solar wind plasma environment, the influence of CIRs on energetic particle populations has been of special interest. In this paper we study the influence of a CIR on the propagation of Jovian electrons to a spacecraft located at 1 AU. Recent modelling in this field has been concentrated on the local influence of CIRs on the electron flux at distances greater than 1 AU. This is due to the fact that modelling on larger spatial scales thus reaching closer to the Sun requires a 3D numerical model which also includes an energy and time dependence of the intensities. With our recently developed numerical model we were able to fulfil these requirements. We show the results of the calculated influence of CIRs on the Jovian and Galactic electron intensity at 1 AU, compared to data taken by the IMP 8 spacecraft, and discuss the implications for the CIR effects on the transport of energetic electrons.Key words. cosmic rays -turbulence -shock waves -convection -diffusion -methods: numerical MotivationThe research concerned with the influence of Corotating Interaction Regions (CIRs) on the continuous flux of energetic electrons, i.e. of Jovian and Galactic origin can formally be split into two fields. First, very interesting results can be obtained by a direct analysis of the data recorded by various spacecraft. Since, usually, only the data recorded on one spacecraft is available, such analysis is confined to the space regions close to the spacecraft. For an analysis of a non-local effect of CIRs one has to apply models to take into account the transport of the particles. These models constitute the second of these fields. According to the region of interest, models considering the transport of Jovian electrons are applicable to different spatial regions. For example the analytical model by Chenette et al. (1974) is only applicable in the vicinity of the Jovian source.In contrast, considering the huge database provided by many spacecraft at 1 AU as well as in the outer heliospheree.g. the IMP 8 probe recorded data throughout more than two solar cycles without major data gaps -a model for the influence of CIRs on large-scale electron transport would be desirable. For this, one needs to solve the Parker equation (Parker 1965) considering three spatial dimensions:Here f (r, P, t) is the electron distribution function depending on rigidity P (this is defined as P = pc |q| with p the momentum, c the speed of light and q the charge of the particle. This is for Send offprint requests to: R. Kissmann, e-mail: rk@tp4.rub.de electrons with energies above 6 MeV, as under consideration here, nearly equivalent to the energy of the particle), position r and time t. Additionally, u represents the solar wind velocity,κ is the diffusion tensor and Q represents any sources. Now, the first term on the right-hand side represents the diffusion of the particles, followed by the term representing c...

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Introduction

Cited by 12 publications

References 0 publications

Nonlinear Alfvén waves, discontinuities, proton perpendicular acceleration, and magnetic holes/decreases in interplanetary space and the magnetosphere: intermediate shocks?

Nonlinear Alfvén waves, discontinuities, proton perpendicular acceleration, and magnetic holes/decreases in interplanetary space and the magnetosphere: intermediate shocks?

On the “injection problem” at the solar wind termination shock

The influence of CIRs on the energetic electron flux at 1 AU

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