Numerical modeling of the solar wind interaction with Venus

Murawski, K.; Steinolfson, R. S.

doi:10.1016/0032-0633(95)00108-5

Cited by 21 publications

(19 citation statements)

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“…The solar wind is flowing from the left-hand side to the righthand side. A bow shock is formed at about 1.4 R M , which is roughly the same as the observed values (Slavin and Holzer, 1982;Schwingenschuh et al, 1990), although the 2D model is not capable of accurately reproducing the position and shape of the bow shock. The ionosphere is very thin, and cannot be seen in Fig.…”

Section: Case 1 (High P Sw )supporting

confidence: 66%

A two-dimensional MHD model of the solar wind interaction with Mars

Shinagawa

Bougher

2014

Earth Planet Sp

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The ionosphere of Mars is expected to be significantly affected by the solar wind because Mars does not possess a significant intrinsic magnetic field which deflects the solar wind. Despite a number of plasma measurements made near Mars, the nature of the solar wind-Mars interaction has not yet been fully understood. In order to self-consistently study the solar wind interaction with the ionosphere of Mars, a two-dimensional MHD model has been developed with an emphasis placed on the structure of the ionosphere of Mars. It is found that the modeled electron density profile in the upper ionosphere strongly depends on the solar wind dynamic pressure as well as the solar zenith angle. The ionosphere in the model tends to have an ionopause-like sharp drop of the electron density at some altitude for realistic solar wind dynamic pressures. Such behavior is not consistent with most of the observed electron density profiles, which exhibit relatively large and constant scale height in most of the dayside region. While the observed electron density profiles of the Venus ionosphere have been reproduced reasonably well by ionospheric models as well as recent three-dimensional MHD models, the electron density profiles of the Martian ionosphere have not been successfully reproduced by theoretical models including this study. This fact implies that processes not present in the Venus ionosphere, such as crustal magnetic fields and the rotation of the planet, may have significant effects on the structure and the dynamics of the ionosphere of Mars.

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Section: Case 1 (High P Sw )supporting

confidence: 66%

A two-dimensional MHD model of the solar wind interaction with Mars

Shinagawa

Bougher

2014

Earth Planet Sp

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“…For a long time most numerical schemes were based on methods dependent on artificial viscosity to represent adequately shocks [4]. Although these schemes were successfully applied in the past [5], recent experience with fully conservative, high-order upwind hydrodynamic codes found latter to be superior in many applications [6]. It is therefore natural to extend such schemes to solve the MHD equations.…”

Section: Introductionmentioning

confidence: 99%

Numerical solutions of magnetohydrodynamic equations

Murawski¹

2011

Bulletin of the Polish Academy of Sciences: Technical Sciences

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Abstract. In this paper we review several mathematical aspects in numerical methods for magnetohydrodynamic equations. The intrinsic complexity and the requirements of the selenoidity condition make numerical solutions of these equations a formidable task. We present results of advanced numerical simulations for a complex system, which reveal that the numerical methods cope very well with this task.

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“…Results of numerical simulations of waves in a strongly stratified atmosphere are presented in Sec. 4. This paper is completed by summary of the main results.…”

Section: Introductionmentioning

confidence: 99%

“…We pay particular attention to those methods which were recently implemented in the code FLASH [6], described briefly in Sec. 4. HD equations are presented in Sec.…”

Section: Introductionmentioning

confidence: 99%

“…They are simple to implement, easily adaptable to complex geometries, and well suited to handle nonlinear terms and large gradients. To represent adequately these gradients most numerical schemes were based on artificial viscosity which was originally introduced by Neumann and Richtmeyer [2], and later used by a number of authors [3,4]. The use of standard numerical schemes of second-order accuracy or higher (e.g., the Lax-Wendroff method) generates spurious oscillations which destroy monotonicity of the solution.…”

Section: Introductionmentioning

confidence: 99%

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