Plasma populations in the tail of induced magnetosphere O. Vaisberg Space Research Institute (IKI), Moscow, Russia, Talk outlay Mars missions studying. - презентация

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 Первый московский симпозиум по Солнечной системе (1M-S3) 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. Первый московский симпозиум по Солнечной системе (1M-S3) Исследования системы Марса

5 Venus as another example of induced magnetosphere Первый московский симпозиум по Солнечной системе (1M-S3) Исследования системы Марса

6 Model of accretion magnetosphere Comparison of computed sizes of planetary/cometary accretional magnetotail (abscissa) and measured ones (ordinate) for Venus, Mars, and comets Giacobini-Zinner and Halley. Model of induced magnetosphere [Vaisberg and Zeleny, 1984] with mantles boundary defined by condition of replacement of the solar plasma by planetary ions. Equation of solar wind and loaded ion mass fluxes was used: N sw M sw V sw = R o N pl (r)ν m pl Первый московский симпозиум по Солнечной системе (1M-S3) Исследования системы Марса

7 Hot ions in central current sheet Первый московский симпозиум по Солнечной системе (1M-S3) Исследования системы Марса

8 Accelerated ions at the magnetopause Первый московский симпозиум по Солнечной системе (1M-S3) Исследования системы Марса

9 Accelerated ions in magnetopause current sheets Первый московский симпозиум по Солнечной системе (1M-S3) Исследования системы Марса

10 Acceleration of ions in boundary layer Первый московский симпозиум по Солнечной системе (1M-S3) Исследования системы Марса

11 Plasma structures at Venus Первый московский симпозиум по Солнечной системе (1M-S3) Исследования системы Марса

12 Tail flow - mass loss 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 10 6 ions cm -2 s x 10 7 ions cm -2 s -1 3 x 10 6 ions cm -2 s -1 < 1 x 10 6 ions cm -2 s -1 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 Первый московский симпозиум по Солнечной системе (1M-S3) Исследования системы Марса

13 Solar wind induced outflow in the tail Первый московский симпозиум по Солнечной системе (1M-S3) 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 Первый московский симпозиум по Солнечной системе (1M-S3) Исследования системы Марса