Numerical simulation of the viscous interaction of the
solar wind with the magnetic polar regions of Venus

Reyes-Ruiz, M.; Díaz-Méndez, E.; Pérez‐de‐Tejada, H.

doi:10.1051/0004-6361:20079265

Cited by 2 publications

References 18 publications

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Numerical simulation of viscous-like flow in and around the plasma tail of a comet

Reyes-Ruiz

Pérez‐de‐Tejada

Aceves

et al. 2010

A&A

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Aims. We model the interaction of the solar wind with the plasma tail of a comet using numerical simulations, taking into account the effects of viscous-like forces. Methods. We developed a 2D hydrodynamical, two species, finite difference code to solve the time-dependent continuity, momentum, and energy conservation equations, and model the interaction of the solar wind with a cometary plasma tail. We compute the evolution of the plasma of cometary origin in the tail as well as the properties of the shocked solar wind plasma around it, as it transfers momentum on its passage by the tail. Velocity, density and temperature profiles across the tail are obtained. Several models with different flow parameters are considered to study the relative importance of viscous-like effects and the coupling between species on the flow dynamics.Results. Assuming a Mach number equal to 2 for the incident solar wind as it flows past the comet's nucleus, the flow exhibits three transitions with location and properties depending on the Reynolds number of each species and on the ratio of the timescale for interspecies coupling to the crossing time of the free-flowing solar wind. By comparing our results with the measurements taken in situ by the Giotto spacecraft during its flyby of comet Halley, we constrain the flow parameters for both plasmas. Conclusions. In the context of our approximations, we find that our model is qualitatively consistent with the in situ measurements as long as the Reynolds number of both solar wind protons and cometary H 2 O+ ions is low, less than 100, suggesting that viscous-like momentum transport processes may play an important role in the interaction of the solar wind and the plasma environment of comets.

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Numerical simulation of viscous-like flow in and around the plasma tail of a comet

Reyes-Ruiz

Pérez‐de‐Tejada

Aceves

et al. 2010

A&A

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Solar Cycle Variations in the Position of Vortex Structures in the Venus Wake

Pérez‐de‐Tejada¹,

Lundin²

2021

Solar System Planets and Exoplanets

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Measurements conducted with the Venus Express (VEX) spacecraft at its entry and exit through vortex structures in the Venus wake reveal that their position varies with the solar cycle. Both crossings are consistently measured closer to Venus during minimum solar cycle conditions and are gradually encountered at larger distances downstream from the planet along the solar cycle. At the same time their width along the VEX trajectory on the plane transverse to the solar wind direction is larger during minimum solar cycle conditions and show a gradual decrease along the solar cycle. As a result the vortex structures are envisioned as features that gradually become thinner as they extend along the Venus wake and agree with the geometry of a vortex flow in fluid dynamics whose thickness decreases with the downstream distance from an obstacle. Similar conditions should also be applicable to Mars and other bodies within the solar system and also possibly to exo-planets in external stellar systems.

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Numerical simulation of the viscous interaction of the solar wind with the magnetic polar regions of Venus

Cited by 2 publications

References 18 publications

Numerical simulation of viscous-like flow in and around the plasma tail of a comet

Numerical simulation of viscous-like flow in and around the plasma tail of a comet

Solar Cycle Variations in the Position of Vortex Structures in the Venus Wake

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