Monte Carlo study of interaction between solar wind plasma and Venusian upper atmosphere

Shematovich, V. I.; Bisikalo, D. V.; Barabash, S.; Stenberg, G.

doi:10.1134/s0038094614050049

Cited by 9 publications

(3 citation statements)

References 22 publications

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“…Taking into account the flow lines would only decrease the overall energy deposition by ENAs and, therefore, not change the main conclusion. Although we studied the conditions of a young Sun (assuming the Sun being a slow and a moderate rotator), this results is similar to the one obtained for modern Venus [ Shematovich et al, ], where also the effects of the induced magnetic field on the proton flux have been taken into account. Our results also suggest that most of the initial CO 2 inventory cannot be removed by the XUV fluxes less than 100 times the present solar value, while hydrogen originating from H 2 O may escape efficiently.…”

Section: Resultssupporting

confidence: 70%

Solar XUV and ENA‐driven water loss from early Venus' steam atmosphere

et al. 2016

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We present a study on the influence of the upper atmosphere hydrodynamic escape of hydrogen, driven by the solar soft X‐ray and extreme ultraviolet radiation (XUV), on an expected outgassed steam atmosphere of early Venus. By assuming that the young Sun was either a weak or moderately active young G star, we estimated the water loss from a hydrogen dominated thermosphere due to the absorption of the solar XUV flux and the precipitation of solar wind produced energetic hydrogen atoms (ENAs). The production of ENAs and their interaction with the hydrodynamic extended upper atmosphere, including collision‐related feedback processes, have been calculated by means of Monte Carlo models. ENAs that collide in the upper atmosphere deposit their energy and heat the surrounding atmosphere mainly above the main XUV energy deposition layer. It is shown that precipitating ENAs modify the thermal structure of the upper atmosphere, but the enhancement of the thermal escape rates caused by these energetic hydrogen atoms is negligible. Our results also indicate that the majority of oxygen arising from dissociated H2O molecules is left behind during the first 100 Myr. It is thus suggested that the main part of the remaining oxygen has been absorbed by crustal oxidation.

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Section: Resultssupporting

confidence: 70%

Solar XUV and ENA‐driven water loss from early Venus' steam atmosphere

et al. 2016

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“…Shematovich et al (2014) considered the effects of an induced ionospheric magnetic field on the ability of solar wind ions to penetrate into the Venus atmosphere with a Monte-Carlo simulation of the interaction between the two. They found that such penetration helps to reflect the solar wind ions, results suggesting that absorption would be minimized with the ionosphere is magnetized due to the condition of either low solar EUV fluxes or high solar wind dynamic pressures.…”

Section: Monte Carlo Modelsmentioning

confidence: 99%

Solar Wind Interaction and Impact on the Venus Atmosphere

et al. 2017

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Venus has intrigued planetary scientists for decades because of its huge contrasts to Earth, in spite of its nickname of "Earth's Twin". Its invisible upper atmosphere and space environment are also part of the larger story of Venus and its evolution. In 60s to 70s, several missions (Venera and Mariner series) explored Venus-solar wind interaction regions. They identified the basic structure of the near-Venus space environment, for example, existence of the bow shock, magnetotail, ionosphere, as well as the lack of the intrinsic magnetic field. A huge leap in knowledge about the solar wind interaction with Venus was made possible by the 14-year long mission, Pioneer Venus Orbiter (PVO), launched in 1978. More recently, ESA's probe, Venus Express (VEX), was inserted into orbit in 2006, operated for 8 years.Owing to its different orbit from that of PVO, VEX made unique measurements in the polar and terminator regions, and probed the near-Venus tail for the first time. The near-tail hosts dynamic processes that lead to plasma energization. These processes in turn lead to the loss of ionospheric ions to space, slowly eroding the Venusian atmosphere. VEX carried an ion spectrometer with a moderate mass-separation capability and the observed ratio of the escaping hydrogen and oxygen ions in the wake indicates the stoichiometric loss of water from Venus. The structure and dynamics of the induced magnetosphere depends on the prevailing solar wind conditions. VEX studied the response of the magnetospheric system on different time scales. A plethora of waves was identified by the magnetometer on VEX; some of them were not previously observed by PVO. Proton cyclotron waves were seen far upstream of the bow shock, mirror mode waves were observed in magnetosheath and whistler mode waves, possibly generated by lightning discharges were frequently seen. VEX also encouraged renewed numerical modeling efforts, including fluid-type of models and particle-fluid hybrid type of models, describing the plasma interaction on scales ranging from ion gyro radius to the entire induced magnetosphere. In this review article, we review what has been found from space physics measurements around Venus (from the solar wind down to the ionopause), with a particular emphasis on updated results since the Venus Express mission. We conclude the article by a short discussion on the remaining open scientific questions and the future of this field.

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“…In the problems connected with the stellar wind, the MHD simulation is necessary too. Thus, the turbulence in stellar wind was investigated (Galtier & Buchlin 2007), one-dimensional MHD model of interaction of stellar wind with 67P/Churyumov-Gerasimenko comet (Mendis & Horanyi 2014), Halley comet (Ogino et al 1988), and also gas planet (Johnstone et al 2015 Shematovich et al 2014) was built. In addition, the similar problems of interaction between stellar wind and stars (Villaver et al 2012) are worth noting.…”

Section: Introductionmentioning

confidence: 99%

The numerical modelling of MHD astrophysical flows with chemistry

Kulikov

Chernykh

Protasov

2017

J. Phys.: Conf. Ser.

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The new code for numerical simulation of magnetic hydrodynamical astrophysical flows with consideration of chemical reactions is given in the paper. At the heart of the code -the new original low-dissipation numerical method based on a combination of operator splitting approach and piecewise-parabolic method on the local stencil. The details of the numerical method are described; the main tests and the scheme of parallel implementation are shown. The chemodynamics of the hydrogen while the turbulent formation of molecular clouds is modeled.

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Monte Carlo study of interaction between solar wind plasma and Venusian upper atmosphere

Cited by 9 publications

References 22 publications

Solar XUV and ENA‐driven water loss from early Venus' steam atmosphere

Solar XUV and ENA‐driven water loss from early Venus' steam atmosphere

Solar Wind Interaction and Impact on the Venus Atmosphere

The numerical modelling of MHD astrophysical flows with chemistry

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