Induced magnetospheres

Luhmann, J. G.; Ledvina, S. A.; Russell, C. T.

doi:10.1016/j.asr.2003.03.031

Cited by 79 publications

(48 citation statements)

References 28 publications

(28 reference statements)

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“…It was based on the theory of fluid flow around the obstacle, which was assumed to have the shape of the ionopause derived from PVO plasma data [Theis et al, 1980]. Zhang et al [1991] realized that the effective obstacle was not the ionopause, but the magnetic barrier above it in the inner magnetosheath, which was also considered as an induced magnetosphere in analogy to the Earth's magnetosphere [Luhmann et al, 2004;Kallio et al, 2008;Zhang et al, 2008a]. At solar minimum, the magnetopause location is at an altitude of about 1000 km at the terminator and 300 km at the subsolar point [Zhang et al, 2008b].…”

Section: Discussionmentioning

confidence: 99%

Magnetosheath fluctuations at Venus for two extreme orientations of the interplanetary magnetic field

Zhang

Wang

et al. 2009

Geophysical Research Letters

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[1] Using the magnetosheath crossings of Venus Express on two consecutive days, we investigate magnetic fluctuations in the same locations for two extreme interplanetary magnetic field orientations, i.e., nearly along and nearly perpendicular to the solar wind flow. It is shown that the properties of the fluctuations are drastically different at basically the same location of the spacecraft in the magnetosheath. The strength and properties of the fluctuations are strongly controlled by the types of the upstream bow shock. The magnetic fluctuations behind a quasi-parallel bow shock are quite strong and turbulent, having a strongly variable angle a eB between maximum variance direction of the fluctuations and the direction of the magnetic field, which may be convected from the upstream waves in the foreshock. The magnetic fluctuations behind a quasi-perpendicular bow shock are less intensive and wave-like, showing a less perturbed angle a eB , which are probably generated locally.

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Section: Discussionmentioning

confidence: 99%

Magnetosheath fluctuations at Venus for two extreme orientations of the interplanetary magnetic field

Zhang

Wang

et al. 2009

Geophysical Research Letters

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“…The magnetosphere of Venus provided us with the first example of an induced magnetosphere (see more about this type of magnetospheres in Podgorny et al 1982;Vaisberg et al 1990;Russell 1991;Luhmann et al 2004). Ionospheric ions and neutral atoms ionized by solar UV, charge exchange and electron impact gain momentum and energy from solar wind and escape to space or impact the atmosphere and sputter heavy atoms and molecules off the exosphere which then can also leave the planets.…”

Section: General Features Of Ion Energizationmentioning

confidence: 98%

Ion Energization and Escape on Mars and Venus

Dubinin

Fräenz

Fedorov³

et al. 2011

Space Sci Rev

162

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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“…(From Ma et al 2007a) in front of Titan. A pair of Alfven wings forms along the magnetic field lines due to perturbations of field-aligned currents (Ness et al 1982;Luhmann et al 2004). On the upstream side, Saturn's magnetospheric plasma flow starts to slow down from about 8 R T (Titan radius) due to mass loading with Titan's extended atmosphere (Hartle et al 2006a(Hartle et al , 2006b, while significant pile-up and strong draping of the magnetic field lines begins around 2 to 3 R T in front of the satellite.…”

Section: General Interaction Featuresmentioning

confidence: 99%

Plasma Flow and Related Phenomena in Planetary Aeronomy

Ma¹,

Altwegg

Бреус

et al. 2008

Space Sci Rev

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Understanding the processes involved in the interaction of solar system bodies with plasma flows is fundamental to the entire field of space physics. The features of the interaction can be very different, depending upon the properties of the incident plasma as well as the nature of the obstacle. The properties of the atmosphere/ionosphere associated with the obstacle are of particular importance into understanding the plasma interaction process, especially for non-magnetized obstacle. This paper discusses in detail the roles of the atmosphere and ionosphere systems of plasma interaction around Venus, Mars, comets Y.-J. Ma ( ) IGPP, UCLA, 312 Y.-J. Ma et al.and some particular satellites. The coupling between magnetosphere and ionosphere is also discussed for Earth and Giant planets.

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Induced magnetospheres

Cited by 79 publications

References 28 publications

Magnetosheath fluctuations at Venus for two extreme orientations of the interplanetary magnetic field

Magnetosheath fluctuations at Venus for two extreme orientations of the interplanetary magnetic field

Ion Energization and Escape on Mars and Venus

Plasma Flow and Related Phenomena in Planetary Aeronomy

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