Formation of the plasma mantle in the Venusian magnetosphere

Вайсберг, О. Л.; Zeleny, L. M.

doi:10.1016/0019-1035(84)90087-3

Cited by 65 publications

(29 citation statements)

References 29 publications

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“…A coupling occurs via the normal and tangential magnetic field stresses and (or) anomalous processes of plasma transport (anomalous diffusion and viscosity). The existence of boundary layers on Mars and Venus was already observed in the first space missions (Vaisberg et al 1976;Taylor et al 1981;Kaspzak et al 1982;Vaisberg and Zelenyi 1984;Vaisberg et al 1995). These observations have identified slow and heavy planetary plasma moving tailward in the intermediate transition between the magnetosheath and the ionosphere.…”

Section: Boundary Layer/mantlementioning

confidence: 82%

Ion Energization and Escape on Mars and Venus

Dubinin

Fräenz

Fedorov³

et al. 2011

Space Sci Rev

167

174

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Mars and Venus do not have a global magnetic field and as a result solar wind interacts directly with their ionospheres and upper atmospheres. Neutral atoms ionized by solar UV, charge exchange and electron impact, are extracted and scavenged by solar wind providing a significant loss of planetary volatiles. There are different channels and routes through which the ionized planetary matter escapes from the planets. Processes of ion energization driven by direct solar wind forcing and their escape are intimately related. Forces responsible for ion energization in different channels are different and, correspondingly, the effectiveness of escape is also different. Classification of the energization processes and escape channels on Mars and Venus and also their variability with solar wind parameters is the main topic of our review. We will distinguish between classical pickup and 'massloaded' pickup processes, energization in boundary layer and plasma sheet, polar winds on unmagnetized planets with magnetized ionospheres and enhanced escape flows from localized auroral regions in the regions filled by strong crustal magnetic fields.

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Section: Boundary Layer/mantlementioning

confidence: 82%

Ion Energization and Escape on Mars and Venus

Dubinin

Fräenz

Fedorov³

et al. 2011

Space Sci Rev

167

174

View full text Add to dashboard Cite

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“…However at the time of PVO it was unclear weather the magnetic tail boundary had a dayside counterpartalthough certain works like Vaisberg and Zeleny (1984) postulated it. More recently, and following the identification criteria of the Martian IMB by MGS (Bertucci et al 2003a), Bertucci et al (2003b) found that the dayside Venusian IMB could be detected from the enhancement of the IMF draping.…”

Section: Identification and Structurementioning

confidence: 97%

The Induced Magnetospheres of Mars, Venus, and Titan

et al. 2011

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This article summarizes and aims at comparing the main features of the induced magnetospheres of Mars, Venus and Titan. All three objects form a well-defined induced magnetosphere (IM) and magnetotail as a consequence of the interaction of an external wind of plasma with the ionosphere and the exosphere of these objects. In all three, photoionization seems to be the most important ionization process. In all three, the IM displays a clear outer boundary characterized by an enhancement of magnetic field draping and massloading, along with a change in the plasma composition, a decrease in the plasma temperature, a deflection of the external flow, and, at least for Mars and Titan, an increase of the total density. Also, their magnetotail geometries follow the orientation of the upstream magnetic field and flow velocity under quasi-steady conditions. Exceptions to this are fossil fields observed at Titan and the near Mars regions where crustal fields dominate the magnetic topology. Magnetotails also concentrate the escaping plasma flux from these three objects and similar acceleration mechanisms are thought to be at work. In the case of Mars and Titan, global reconfiguration of the magnetic field topology (reconnection with the crustal sources and exits into Saturn's magnetosheath, respectively) may lead to important losses of C. Bertucci ( )

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“…In the same way that currents on the surface of a spherical conductor in a time-varying uniform magnetic field produce an opposing induced dipole field preventing penetration of the external field, currents generated in Venus' ionosphere produce fields that to first order exclude the IMF (e.g. Vaisberg and Zeleny 1984;Dubinin et al 2013a). The fields of these ionospheric currents combine with the external magnetic field to produce the piled-up and draped magnetosheath-like fields that deflect the solar wind plasma around the 'obstacle': the main ionosphere and body of Venus.…”

Section: Differences From Comets and Marsmentioning

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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Formation of the plasma mantle in the Venusian magnetosphere

Cited by 65 publications

References 29 publications

Ion Energization and Escape on Mars and Venus

Ion Energization and Escape on Mars and Venus

The Induced Magnetospheres of Mars, Venus, and Titan

Solar Wind Interaction and Impact on the Venus Atmosphere

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