Venus–solar wind interaction: Asymmetries and the escape of ions

Kallio, Esa; Järvinen, R.; Janhunen, P.

doi:10.1016/j.pss.2006.04.030

Cited by 57 publications

(71 citation statements)

References 17 publications

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“…In many ways, such models are in good agreement with spacecraft observations (e.g. Kallio et al 2006;Modolo et al 2006;Dubinin et al 2008).…”

Section: Hybrid Models Of Mars' Interaction With the Solar Windmentioning

confidence: 52%

“…It emphasized the asymmetry of the O + dynamics in the direction of the motional electric field, which is in many ways similar to the Martian case. With a three-dimensional model, Kallio et al (2006) showed that asymmetry in the escape of O + was due to the motional electric field, in agreement with Moore et al (1991) . Hybrid simulations are in good agreement with Pioneer Venus Orbiter observations (Jarvinen et al 2008) and Venus-Express observations (Kallio et al 2008;Zhang et al 2010) and reproduce the main boundaries and regions.…”

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

confidence: 53%

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Modeling of Venus, Mars, and Titan

Kallio

Chaufray

Modolo

et al. 2011

Space Sciences Series of ISSI

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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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“…In many ways, such models are in good agreement with spacecraft observations (e.g. Kallio et al 2006;Modolo et al 2006;Dubinin et al 2008).…”

Section: Hybrid Models Of Mars' Interaction With the Solar Windmentioning

confidence: 52%

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

confidence: 53%

Modeling of Venus, Mars, and Titan

Kallio

Chaufray

Modolo

et al. 2011

Space Sciences Series of ISSI

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“…Having this range of simulations also has the additional advantage that one can more easily compare with simulations in the literature, e.g. Venus studies such as Martinecz et al (2009) and Kallio et al (2006). Thus, we chose to perform three simulation runs, all of them identical with the exception of the angle α sw,0 between the undisturbed stellar wind velocity and the IMF.…”

Section: Model Parametersmentioning

confidence: 99%

Interplanetary magnetic field orientation and the magnetospheres of close-in exoplanets

Johansson

Joachim

Motschmann

2010

A&A

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The abundance of exoplanets with orbits smaller than that of Mercury most likely implies that there are exoplanets exposed to a quasiparallel stellar-wind magnetic field. Many of the generic features of stellar-wind interaction depend on the existence of a nonzero perpendicular interplanetary magnetic field component. However, for closer orbits the perpendicular component becomes smaller and smaller. The resulting quasiparallel interplanetary magnetic field may imply new types of magnetospheres and interactions not seen in the solar system. We simulate the Venus-like interaction between a supersonic stellar wind and an Earth-sized, unmagnetized terrestrial planet with ionosphere, orbiting a Sun-like star at 0.2 AU. The importance of a quasiparallel stellar-wind interaction is then studied by comparing three simulation runs with different angles between stellar wind direction and interplanetary magnetic field. The plasma simulation code is a hybrid code, representing ions as particles and electrons as a massless, charge-neutralizing adiabatic fluid. Apart from being able to observe generic features of supersonic stellar-wind interaction we observe the following changes and trends when reducing the angle between stellar wind and interplanetary magnetic field 1) that a large part of the bow shock is replaced by an unstable quasiparallel bow shock; 2) weakening magnetic draping and pile-up; 3) the creation of a second, flanking current sheet due to the need for the interplanetary magnetic field lines to connect to almost antiparallel draped field lines; 4) stellar wind reaching deeper into the dayside ionosphere; and 5) a decreasing ionospheric mass loss. The speed of the last two trends seems to accelerate at low angles.

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“…See Kallio and Janhunen (2003) for the numerical details of the code. Further, Kallio et al (2006b) introduce the usage of the code in the Venus simulations.…”

Section: The Hyb Code and The Venus Express Observationsmentioning

confidence: 99%

“…23 in Brace and Kliore, 1991). Estimates of the total solar wind induced oxygen ion escape from Venus range from the order of 10 24 s −1 to 10 26 s −1 including observational and simulation studies (e.g., Brace et al, 1987;Moore and McComas, 1992;Terada et al, 2004;Lammer et al, 2006;Kallio et al, 2006b;Barabash et al, 2007a;Martinecz et al, 2009). We select to call the value 10 25 s −1 as the nominal O + escape rate.…”

Section: Introductionmentioning

confidence: 99%

Oxygen ion escape from Venus in a global hybrid simulation: role of the ionospheric O<sup>+</sup> ions

et al. 2009

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Abstract. We study the solar wind induced oxygen ion escape from Venus' upper atmosphere and the Venus Express observations of the Venus-solar wind interaction by the HYB-Venus hybrid simulation code. We compare the simulation to the magnetic field and ion observations during an orbit of nominal upstream conditions. Further, we study the response of the induced magnetosphere to the emission of planetary ions. The hybrid simulation is found to be able to reproduce the main observed regions of the Venusian plasma environment: the bow shock (both perpendicular and parallel regions), the magnetic barrier, the central tail current sheet, the magnetic tail lobes, the magnetosheath and the planetary wake. The simulation is found to best fit the observations when the planetary O + escape rate is in the range from 3×10 24 s −1 to 1.5×10 25 s −1 . This range was also found to be a limit for a test particle-like behaviour of the planetary ions: the higher escape rates manifest themselves in a different global configuration of the Venusian induced magnetosphere.

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Venus–solar wind interaction: Asymmetries and the escape of ions

Cited by 57 publications

References 17 publications

Modeling of Venus, Mars, and Titan

Modeling of Venus, Mars, and Titan

Interplanetary magnetic field orientation and the magnetospheres of close-in exoplanets

Oxygen ion escape from Venus in a global hybrid simulation: role of the ionospheric O<sup>+</sup> ions

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Venus–solar wind interaction: Asymmetries and the escape of ions

Cited by 57 publications

References 17 publications

Modeling of Venus, Mars, and Titan

Modeling of Venus, Mars, and Titan

Interplanetary magnetic field orientation and the magnetospheres of close-in exoplanets

Oxygen ion escape from Venus in a global hybrid simulation: role of the ionospheric O&lt;sup&gt;+&lt;/sup&gt; ions

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Oxygen ion escape from Venus in a global hybrid simulation: role of the ionospheric O<sup>+</sup> ions