Plasma structures at weakly outgassing comets—results from bi-ion fluid analysis

Bogdanov, A. T.; Sauer, K.; Baumgärtel, K.; Srivastava, Krishna M.

doi:10.1016/0032-0633(95)00153-0

Cited by 29 publications

(30 citation statements)

References 9 publications

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“…Addition of the planetary heavy ions, favorable moved in the +Z direction, might lead to a decrease of asymmetry associated with a finite proton gyroradius. The 2D bi-ion MHD modeling, which treats the protons and the heavies as separate populations and electrons as a massless fluid shows that the BS occurs at larger distances at the northern half-plane Z * > 0 (see, for example, figures 1(b)-2(b) from Bogdanov et al, 1996). In the runs by Bogdanov et al (1996) the magnetic field was perpendicular to the simulation plane, and asymmetry, related with the motional electric field, could be tested.…”

Section: Asymmetry Of the Bow Shock Predictions And Observationsmentioning

confidence: 99%

“…The 2D bi-ion MHD modeling, which treats the protons and the heavies as separate populations and electrons as a massless fluid shows that the BS occurs at larger distances at the northern half-plane Z * > 0 (see, for example, figures 1(b)-2(b) from Bogdanov et al, 1996). In the runs by Bogdanov et al (1996) the magnetic field was perpendicular to the simulation plane, and asymmetry, related with the motional electric field, could be tested. The 2D-bi-ion simulations also demonstrated that the interaction pattern changes with an increase of mass-loading.…”

Section: Asymmetry Of the Bow Shock Predictions And Observationsmentioning

confidence: 99%

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The IMF control of the Martian bow shock and plasma flow in the magnetosheath. Predictions of 3-D simulations and observations

et al. 2014

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Recent three-dimensional simulations of the Martian plasma and magnetic field environment found some unique effects-a strong asymmetry of the bow shock and the magnetic field draping, asymmetry of plasma inflow to the wake, formation of secondary shocks near the boundary of the magnetospheric cavity. The predictions of the models are testified using the Phobos-2 data. It is shown, that, although, the models reproduce some features of the bow shock and plasma flow around the planet, the real picture appears to be more variable and complicated. We suppose that addition of planetary plasma originated from the atmosphere/exosphere and effects of mass-loading is necessary modification of three-dimensional models.

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Section: Asymmetry Of the Bow Shock Predictions And Observationsmentioning

confidence: 99%

Section: Asymmetry Of the Bow Shock Predictions And Observationsmentioning

confidence: 99%

The IMF control of the Martian bow shock and plasma flow in the magnetosheath. Predictions of 3-D simulations and observations

et al. 2014

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“…(2) and (3) is mainly adopted by the code described in [22]. The main steps are briefly described here for reference.…”

Section: Time Integration Schemementioning

confidence: 99%

“…It quickly became clear in earlier simulations using the fluid model in two dimensions [2,19] that the draping of the magnetic field lines in front of the nucleus is not modeled correctly by two-dimensional models. Three-dimensional fluid simulations of this problem were done by Fischer [8] and hybrid simulations by Lipatov et al [18].…”

Section: Introductionmentioning

confidence: 98%

3D Hybrid Simulation Code Using Curvilinear Coordinates

Bagdonat¹,

Motschmann

2002

Journal of Computational Physics

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“…Magnetohydrodynamics and multi-fluid models constitute a very efficient method to study the global structure of the plasma environment of strongly outgassing comets (Wegmann et al, 1987;Bogdanov et al, 1996;Gombosi et al, 1996;Hansen et al, 2007;Benna and Mahaffy, 2006). In this regime, close to perihelion, the characteristic length scale of the solar windcomet interaction is large compared to the gyroradius of the heaviest particles and thus a fluid description is appropriate.…”

Section: Introductionmentioning

confidence: 99%

Mapping of coma anisotropies to plasma structures of weak comets: a 3-D hybrid simulation study

et al. 2009

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Abstract. The effects of coma anisotropies on the plasma environment of comets have been studied by means of a 3-D hybrid model which treats electrons as a massless, chargeneutralizing fluid, whereas ion dynamics are covered by a kinetic approach. From Earth-based observations as well as from in-situ spacecraft measurements the shape of the coma of many comets is ascertained to be anisotropic. However, most plasma simulation studies deploy a spherically symmetric activity pattern. In this paper anisotropy is studied by considering three different coma shape models. The first model is derived from the Haser model and is characterised by spherically symmetry. This reference model is then compared with two different neutral gas shape models: the dayside restricted model with no nightside activity and a cone shaped model with opening angle of π/2. In all models the integrated surface activity is kept constant. The simulations have been done for the Rosetta target comet 67P/Churyumov-Gerasimenko for two heliocentric distances, 1.30 AU and 3.25 AU. It is found that shock formation processes are modified as a result of increasing spatial confinement. Characteristic plasma structures of comets such as the bow shock, magnetic barrier region and the ion composition boundary exhibit a shift towards the sun. In addition, the cone shaped model leads to a strong increase of the mass-loaded region which in turn leads to a smooth deceleration of the solar wind flow and an increasing degree of mixture between the solar wind and cometary ion species. This creates an additional transport channel of the magnetic field from the magnetic barrier region away which in turn leads to a broadening of this region. In addition, it leads to an ion composition boundary which is only gradually developed.

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Plasma structures at weakly outgassing comets—results from bi-ion fluid analysis

Cited by 29 publications

References 9 publications

The IMF control of the Martian bow shock and plasma flow in the magnetosheath. Predictions of 3-D simulations and observations

The IMF control of the Martian bow shock and plasma flow in the magnetosheath. Predictions of 3-D simulations and observations

3D Hybrid Simulation Code Using Curvilinear Coordinates

Mapping of coma anisotropies to plasma structures of weak comets: a 3-D hybrid simulation study

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