Numerical simulations of mass loading in the solar wind interaction with Venus

Murawski, K.; Steinolfson, R. S.

doi:10.1029/95ja02433

Cited by 26 publications

(15 citation statements)

References 28 publications

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“…Therefore, the global scale solar wind interaction with Mars is with the ionosphere‐atmosphere system, but the presence of this remnant magnetization can have an important impact on some aspects of the interaction processes. Studies of the solar wind interaction with unmagnetized bodies (e.g., Venus, Mars, Titan) have been carried out in the past using semikinetic [e.g., Brecht , 1997], single and multispecies MHD [e.g., Murawski and Steinolfson , 1996; Tanaka and Murawski , 1997; Tanaka , 1998; Bauske et al , 1998; Shinagawa and Bougher , 1999; Liu et al , 1999, 2001] and two‐ion [ Sauer et al , 1994, 1996] MHD model calculations.…”

Section: Introductionmentioning

confidence: 99%

Three‐dimensional multispecies MHD studies of the solar wind interaction with Mars in the presence of crustal fields

et al. 2002

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[1] We present the results of model calculations using a multispecies MHD model of the interaction of the solar wind with Mars. The three ions considered are H + , O 2 + , and O + , representing the solar wind and the two major ionospheric ion species, respectively. The calculations indicate that the presence of a hot oxygen corona does not, within the resolution and accuracy of the model, lead to any significant effect on the dayside bow shock and ionopause positions. Next the trans-terminator fluxes and escape fluxes down the tail were calculated neglecting the effects of the crustal magnetic field. The calculated flux values are consistent with the measured escape fluxes and the calculated limiting fluxes from the dayside ionosphere. Finally, a 60-order harmonic expansion model of the measured magnetic field was incorporated into the model. The crustal magnetic field did not cause major distortions in the bow shock but certainly had an important effect within the magnetosheath and on the apparent altitude of the ionopause. The model results also indicated the presence of ''minimagnetocylinders,'' consistent with the MGS observations. We also recalculated the trans-terminator and escape fluxes, for the nominal solar wind case, in the presence of the crustal magnetic field and found, as expected, that there is a decrease in the calculated escape flux; however, it is still reasonably close to the value estimated from the Phobos-2 observations.

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Section: Introductionmentioning

confidence: 99%

Three‐dimensional multispecies MHD studies of the solar wind interaction with Mars in the presence of crustal fields

et al. 2002

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“…Observations showed that the bow shock and MPB were located further from Venus during solar maximum than solar minimum. It was hypothesized that mass loading from higher EUV ionization caused the bow shock to move out during solar maximum, however previous 3D MHD models (Murawski and Steinolfson 1996) had not been able to show this effect. However, the simulation by Murawski and Steinolfson (1996) used an unrealistic IMF direction.…”

Section: Mhd Models Of Venus' Interaction With the Solar Windmentioning

confidence: 91%

“…It was hypothesized that mass loading from higher EUV ionization caused the bow shock to move out during solar maximum, however previous 3D MHD models (Murawski and Steinolfson 1996) had not been able to show this effect. However, the simulation by Murawski and Steinolfson (1996) used an unrealistic IMF direction. Kallio et al (1998) used an ideal MHD model with a source term included in the continuity equation to determine if mass loading from photoionization, charge exchange, and electron impact ionization could account for the bow shock distances.…”

Section: Mhd Models Of Venus' Interaction With the Solar Windmentioning

confidence: 91%

Modeling of Venus, Mars, and Titan

et al. 2011

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Increased computer capacity has made it possible to model the global plasma and neutral dynamics near Venus, Mars and Saturn's moon Titan. The plasma interactions at Venus, Mars, and Titan are similar because each possess a substantial atmosphere but lacks a global internally generated magnetic field. In this article three self-consistent plasma models are described: the magnetohydrodynamic (MHD) model, the hybrid model and the fully kinetic plasma model. are also described. In particular, we describe the pros and cons of each model approach. Results from simulations are presented to demonstrate the ability of the models to capture the known plasma and neutral dynamics near the three objects.

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“…1-16͒. In several studies, planets are modeled as the simple perfect-conducting sphere and numerical simulations have been conducted to investigate the flow field and magnetic field around planets in detail. [2][3][4][5]15 These include the following: ͑1͒ a magnetic pile-up region, where magnetic pressure is dominant, exists in front of the planet; ͑2͒ density buildup and depletion occurs in the magnetosheath; ͑3͒ flow near the planet is accelerated in the polar regions and decelerated in the equatorial plane because of the Lorentz force; and ͑4͒ an induced magnetotail from highly draped interplanetary flux tubes forms in the wake. In those past studies, steady flow fields in which the magnetic field slips from obstacles were analyzed.…”

Section: Introductionmentioning

confidence: 99%

Magnetohydrodynamic analysis of the interaction of magnetized plasma flow with a perfect-conducting object

Nishida

Abe

2010

Physics of Plasmas

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In this study, a supersonic and super-Alfvénic magnetized plasma flow past a perfect-conducting cylinder was simulated based on single-fluid ideal magnetohydrodynamics to clarify the piling-up process of the magnetic field frozen in the plasma flow. Therefore, the magnetic field is assumed to be perpendicular to both the cylinder axis and the flow direction. Simulation results indicated that the cylinder continuously traps the magnetic field and an unsteady flow field is generated. Even though the drag force exerting on the cylinder is expected to continuously increase with the continuous increase in the trapped magnetic field and the shock layer, the intensity of magnetic flux density at the cylinder surface is saturated at a certain value and the drag force is also saturated. The saturated values are characterized by the Alfvén Mach number of the mainstream. Furthermore, on this flow structure the wake flow in which magnetic reconnection plays an important role was found to have a strong influence by using the pseudomagnetic reconnection in the ideal magnetohydrodynamic flow.

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Numerical simulations of mass loading in the solar wind interaction with Venus

Cited by 26 publications

References 28 publications

Three‐dimensional multispecies MHD studies of the solar wind interaction with Mars in the presence of crustal fields

Three‐dimensional multispecies MHD studies of the solar wind interaction with Mars in the presence of crustal fields

Modeling of Venus, Mars, and Titan

Magnetohydrodynamic analysis of the interaction of magnetized plasma flow with a perfect-conducting object

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