Regular oblique interaction of shock waves coming from the same direction in a conducting medium with a magnetic field

Pushkar, E. A.

doi:10.1007/bf02078209

Cited by 4 publications

(5 citation statements)

References 6 publications

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“…This can be attributed to the fact that in the former case the diffusion scale length is much smaller than the distance to the TS and the ACR pressure behind the TS being comparable with the static pressure of the plasma component. In the latter case the ACR pressure is negligible as compared with the plasma component static pressure, so that the effect of the ACR on the results by Baranov and Malama (1993, 1995 can be neglected.…”

Section: Figmentioning

confidence: 96%

“…The self-consistent, kinetic-MHD approach for the solution of 2D MHD and 3D MHD problem was presented in Sect. 5.3 as a development of the kinetic-hydrodynamic model by Baranov and Malama (1993, 1995. However, numerical difficulties of the kinetic description of the H atom motion together with MHD description of the plasma component leaded to many publications where the H atom component is described in a simplified multi-fluid form.…”

Section: Mhd Models Of the Solar Wind Interaction With The Magnetizedmentioning

confidence: 99%

“…4). The instantaneous assimilation of the interstellar and solar wind proton origin with pickup protons is assumed in the model by Baranov and Malama (1993, 1995 considered above. However, experimental data (e.g., Gloeckler et al 1993;Gloeckler 1996;Gloeckler and Geiss 1998) and theoretical estimations (e.g., Isenberg 1986) clearly show that pickup ions must be considered as an individual component with the distribution function which is not coinciding with the distribution function of solar and interstellar proton origin.…”

Section: Effect Of Nonequilibrium Of Pickup and Solar Protons In The mentioning

confidence: 99%

“…However, direct (one-dimensional) collisions are not real for the problem of the TS interaction with the interplanetary discontinuities. That is why a two-dimensional MHD theory, developed by Pushkar' (1990, 1991) and Pushkar' (1995), was used to consider the problem of the termination shock interaction with the interplanetary forward (Baranov et al 1996a(Baranov et al , 1996b and reverse (Baranov and Pushkar' 2004) shocks. A result of the interaction between the TS, which is the fast S + (TS) MHD shock, and an fast MHD interplanetary shock S + (IPS) in Fig.…”

Section: On the Interaction Of The Interplanetary Strong Discontinuitmentioning

confidence: 99%

“…The distribution function f pui was determined by Malama et al (2006) solving the pickup ion kinetic equation (25) while a complete assimilation of the pickup ions into the solar wind plasma (T pui = T p ) was assumed by Baranov and Malama (1993, 1995. Malama et al (2006) used typical boundary conditions at the undisturbed LISM and at the Earth's orbit.…”

Section: Effect Of Nonequilibrium Of Pickup and Solar Protons In The mentioning

confidence: 99%

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Kinetic-Hydrodynamic Models of the Solar Wind Interaction with the Partially Ionized Supersonic Flow of the Local Interstellar Gas: Predictions and Interpretations of the Experimental Data

Баранов

2008

Space Sci Rev

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At present there is no doubt that the local interstellar medium (LISM) is mainly partially ionized hydrogen gas moving with a supersonic flow relative to the solar system. The bulk velocity of this flow is approximately equal ∼ 26 km/s. Although the interaction of the solar wind with the charged component (below plasma component) of the LISM can be described in the framework of hydrodynamic approach, the interaction of H atoms with the plasma component can be correctly described only in the framework of kinetic theory because the mean free path of H atoms in the main process of the resonance charge exchange is comparable with a characteristic length of the problem considered. Results of selfconsistent, kinetic-hydrodynamic models are considered in this review paper. First, such the model was constructed by Baranov and Malama (J. Geophys. Res. 98(A9): 15,163, 1993). Up to now it is mainly developed by Moscow group taking into account new experimental data obtained onboard spacecraft studying outer regions of the solar system (Voyager 1 and 2, Pioneer 10 and 11, Hubble Space Telescope, Ulysses, SOHO and so on). Predictions and interpretations of experimental data obtained on the basis of these models are presented. Kinetic models for describing H atom motion were later suggested by Fahr et al. (Astron. Astrophys 298:587-600, 1995) and Lipatov et al. (J. Geophys. Res. 103(A9):20,631-20,642, 1998). However they were not self-consistent and did not incorporate sources to the plasma component. A self-consistent kinetic-hydrodynamic model suggested by Heerikhuisen et al. (J. Geophys. Res. 111:A06110, 2006, Astrophys. J. 655:L53-L56, 2007) was not tested on the results by Baranov and Malama (J. Geophys. Res. 111:A06110, 1993) although it was suggested much later. Besides authors did not describe in details their Monte Carlo method for a solution of the H atom Boltzmann equation and did not inform about an accuracy of this method. Therefore the results of Heerikhuisen et al. (J . Geophys. Res. 111:A06110, 2006) are in open to question and will not be considered in this review paper. That is why below we will mainly consider a progress of the Moscow group on heliospheric modelling endeavours in the kinetic-hydrodynamic approach. Criticism of the models that treat interstellar hydrogen in the heliosphere as several fluids is given. It is shown that the multi-fluid 24 V.B. Baranov models give rise to unreal results especially for distributions of neutral component parameters. Magnetohydrodynamic (MHD) modelling of the solar wind interaction with the LISM gas is also reviewed.

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Section: Figmentioning

confidence: 96%

Section: Mhd Models Of the Solar Wind Interaction With The Magnetizedmentioning

confidence: 99%

Section: Effect Of Nonequilibrium Of Pickup and Solar Protons In The mentioning

confidence: 99%

Section: On the Interaction Of The Interplanetary Strong Discontinuitmentioning

confidence: 99%

Section: Effect Of Nonequilibrium Of Pickup and Solar Protons In The mentioning

confidence: 99%

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Kinetic-Hydrodynamic Models of the Solar Wind Interaction with the Partially Ionized Supersonic Flow of the Local Interstellar Gas: Predictions and Interpretations of the Experimental Data

Баранов

2008

Space Sci Rev

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Pushkar

Бармин

2000

Astrophysics and Space Science

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Interaction of interplanetary shocks with the heliospheric termination shock: Two‐dimensional magnetohydrodynamic model

Баранов¹,

Barmin²,

Pushkar³

1996

J. Geophys. Res.

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The two‐dimensional problem of the oblique interaction between an interplanetary shock (IPS) and the termination shock (TS) with allowance for the effect of the interplanetary magnetic field is studied within the framework of the ideal magnetohydrodynamic model and a steady model of the solar wind interaction with the local interstellar medium. The self‐consistent axisymmetric model proposed by Baranov and Malama, which takes into account the processes of resonant charge exchange between H atoms and protons, is used. The electron number density and the solar wind velocity VSW ahead of TS depends on the parameters of this model. The postinteraction configuration consists of a new moving TS′, a transmitted IPS′, a set of Alfvén and slow magnetohydrodynamic waves, and a contact discontinuity which can change as functions of five dimensionless governing parameters and the specific heat ratio γ. The maximum electron number density ne is usually reached behind the new termination shock TS′ for an oblique (θ ≠ 0) impingement of IPS on TS rather than for the head‐on collision (θ = 0). Nevertheless, the maximum calculated values of ne are lower than those corresponding to plasma frequencies ωp ≅ 2 kHz observed by the Voyager spacecraft. It is found that all the quantities considered depends radically on the angle ψTS between the front of TS and the vector of the interplanetary magnetic field strength BSW.

show abstract

Regular oblique interaction of shock waves coming from the same direction in a conducting medium with a magnetic field

Cited by 4 publications

References 6 publications

Kinetic-Hydrodynamic Models of the Solar Wind Interaction with the Partially Ionized Supersonic Flow of the Local Interstellar Gas: Predictions and Interpretations of the Experimental Data

Kinetic-Hydrodynamic Models of the Solar Wind Interaction with the Partially Ionized Supersonic Flow of the Local Interstellar Gas: Predictions and Interpretations of the Experimental Data

Untitled

Interaction of interplanetary shocks with the heliospheric termination shock: Two‐dimensional magnetohydrodynamic model

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