On electron and ion components of plasma in the antisolar part of near-Martian space

Gringauz, K. I.; Безруких, В. В.; Веригин, М. И.; Remizov, A. P.

doi:10.1029/ja081i019p03349

Cited by 44 publications

(29 citation statements)

References 10 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…However, the discoveries from the very first Mars-and Venus missions, such as Mars-2, -3, and -5 (e.g. Gringauz et al 1976aGringauz et al , 1976bVaisberg 1976), Venera-9, and -10 (Vaisberg et al 1976;Gringauz et al 1976a), and Pioneer Venus Orbiter, PVO, (e.g. Intriligator et al 1979;Mihalov and Barnes 1981;Russell et al 1985;Brace et al 1987) paved the way for the new discoveries.…”

Section: Introductionmentioning

confidence: 97%

Ion Acceleration and Outflow from Mars and Venus: An Overview

Lundin

2011

Space Sci Rev

View full text Add to dashboard Cite

Solar wind forcing of Mars and Venus results in outflow and escape of ionospheric ions. Observations show that the replenishment of ionospheric ions starts in the dayside at low altitudes (≈300-800 km), ions moving at a low velocity (5-10 km/s) in the direction of the external/ magnetosheath flow. At high altitudes, in the inner magnetosheath and in the central tail, ions may be accelerated up to keV energies. However, the dominating energization and outflow process, applicable for the inner magnetosphere of Mars and Venus, leads to outflow at energies ≈5-20 eV.The aim of this overview is to analyze ion acceleration processes associated with the outflow and escape of ionospheric ions from Mars and Venus. Qualitatively, ion acceleration may be divided in two categories:(a) Modest ion acceleration, leading to bulk outflow and/or return flow (circulation). (b) Acceleration to well over escape velocity, up into the keV range.In the first category we find a processes denoted "planetary wind", the result of e.g. ambipolar diffusion, wave enhanced planetary wind, and mass-loaded ion pickup. In the second category we find ion pickup, current sheet acceleration, wave acceleration, and parallel electric fields, the latter above Martian crustal magnetic field regions. Both categories involve mass loading. Highly mass-loaded ion energization may lead to a low-velocity bulk flow-A consequence of energy and momentum conservation. It is therefore not self-evident what group, or what processes are connected with the low-energy outflow of ionospheric ions from Mars.Experimental and theoretical findings on ionospheric ion acceleration and outflow from Mars and Venus are discussed in this report.

show abstract

Section: Introductionmentioning

confidence: 97%

Ion Acceleration and Outflow from Mars and Venus: An Overview

Lundin

2011

Space Sci Rev

View full text Add to dashboard Cite

show abstract

“…The Martian bowshock (Gringauz et al, 1976a) has turned out to be more complex than anticipated (e.g. Dubinin et al, 1993).…”

Section: Dayside and Magnetotail Boundariesmentioning

confidence: 97%

The wakes and magnetotails of Mars and Venus

Lundin

Barabash

2004

Advances in Space Research

View full text Add to dashboard Cite

“…The magnetic fields and plasma were measured on the planet's night side with the threeaxial orientation of the satellite (Dolginov et al, 1974;Gringauz et al, 1975). The magnetic fields and plasma were measured on the planet's night side with the threeaxial orientation of the satellite (Dolginov et al, 1974;Gringauz et al, 1975).…”

Section: The Mars-5 Orbiter and Latermentioning

confidence: 99%

“…The magnetic field and plasma data were obtained during nine communication periods (Dolginov et al, 1974(Dolginov et al, , 1976aGringauz et al, 1975). The magnetic field and plasma data were obtained during nine communication periods (Dolginov et al, 1974(Dolginov et al, , 1976aGringauz et al, 1975).…”

Section: Mars-~• Rbitermentioning

confidence: 99%

What we have learned about the Martian magnetic field

Dolginov

1987

Earth Moon Planet

View full text Add to dashboard Cite

The evidence is presented for the existence of the magnetic field of the planet Mars and for the effectiveness of the dipolar part of the field as an obstacle to the solar wind at the most frequent parameters of the latter. The dipolar magnetic moment of Mars is (1.5-2.20 x 102* G cm3. The dipole axis makes an angle i < 15" with the rotation axis of the panet. The magnetic north pole of Mars is located in its southern hemisphere.In terms of the precession dynamo model, the magnetic fields of the Earth and Mars are similar. This indicates that the Martian magnetic field is associated with the present-day dynamo-process in the Martian liquid core. MAGNETIC FIELD 43

show abstract

On electron and ion components of plasma in the antisolar part of near-Martian space

Cited by 44 publications

References 10 publications

Ion Acceleration and Outflow from Mars and Venus: An Overview

Ion Acceleration and Outflow from Mars and Venus: An Overview

The wakes and magnetotails of Mars and Venus

What we have learned about the Martian magnetic field

Contact Info

Product

Resources

About