1. Plasma populations in the tail of induced magnetosphere
O. Vaisberg
Space Research Institute (IKI), Moscow, Russia,
Talk outlay
Mars missions studying Martian magnetosphere
Four plasma populations in the accretion tail
Solar wind induced planetary ions flow
Hot ions in the central current sheet
Accelerated ions at the tail boundary
Ionospheric outflow
Venus is used as a proxy for some topics
Conclusion
Первый московский симпозиум по Солнечной системе (1M-S3)
Исследования системы Марса

2. Mars probes in solar activity cycles
Sputnik launch
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Исследования системы Марса

3. First observations of hot planetary ions outflow on Mars orbiters
The region of low-energy ions ( eV) on the dayside and in the tail was found on Mars-2 and Mars-3 indication that the tail flow is a continuation of the dayside ion cusion [Vaisberg and Bogdanov, 1974].
Первый московский симпозиум по Солнечной системе (1M-S3)
Исследования системы Марса

4. Heavy planetary ions in ionosheath and tail
Dynamics of light and heavy ions in magnetosheath and in tail obtained by channel multipliers’ “mass-spectrometry” [Vaisberg, 1976]. Note the termination of light ions with transition to cometary ions flow at magnetic tail boundary.
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Исследования системы Марса

5. Venus as another example of induced magnetosphere
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6. Model of accretion magnetosphere
Model of induced magnetosphere [Vaisberg and Zeleny, 1984] with mantle’s boundary defined by condition of replacement of the solar plasma by planetary ions. Equation of solar wind and loaded ion mass fluxes was used:
NswMswVsw= RoNpl (r)ν mpl
Comparison of computed sizes of planetary/cometary accretional magnetotail (abscissa) and measured ones (ordinate) for Venus, Mars, and comets Giacobini-Zinner and Halley.
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Исследования системы Марса

7. Hot ions in central current sheet
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Исследования системы Марса

8. Accelerated ions at the magnetopause
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Исследования системы Марса

9. Accelerated ions in magnetopause current sheets
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Исследования системы Марса

10. Acceleration of ions in boundary layer
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Исследования системы Марса

11. Plasma structures at Venus
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Исследования системы Марса

12. Tail flow - mass loss Barabash et al., ME/Aspera-3
Vaisberg et al., Mars-5
Verigin et al., 1991
Phobos-2/TAUS
Lundin et al., 1989
Phobos-2/Aspera
Barabash et al., ME/Aspera-3
Measured flux in the tail
average 3 x 106
ions cm-2 s-1
2.5 x 107
3 x 106
< 1 x 106
Calculated mass loss
1 x s–1
~ 250 g s–1
5 x s–1
150 g s–1
2 x s–1
500 g s–1
3.9 x s–1
18 g s–1
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Исследования системы Марса

13. Solar wind induced outflow in the tail
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Исследования системы Марса

14. Conclusion • New picture of accretion magnetosphere of Mars/Venus
• Four populations of plasma in accretion tail:
Solar wind induced planetary ions flow
Hot ions in the central current sheet
Accelerated ions at the tail boundary
Ionospheric outflow
• There is basic understanding of their origin
• The role of different mechanisms in atmospheric losses and their quantitative characteristics is not well established
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Исследования системы Марса