Lundstedt (IRF-Lund)

1
Lundstedt (IRF-Lund)
2
Narayan (Stockholm-U)
3
Kanao (ISAS, Japan)
The effect of the crustal magnetic field on the
distribution of the ion number density around Mars
The distribution of the Martian proton number
density at the dayside
M. Kanao, A. Yamazaki, Y. Futaana, T. Abe, M.
Nakamua, S. Barabash,A. Fedorov, M. Franz, and
ASPERA-3 Team
E is northern direction Crustal magnetic field
is in Edown hemisphere
E is southern direction.Crustal magnetic field
is in Eup hemisphere
Only In the case when the crustal magnetic field
is in the Eup hemisphere, the proton number
density increases.
4
Morooka (IRF-Uppsala)
Co-rotating dynamics of Saturns magnetosphere M.
Morooka et al. (IRFU)
The electron density model obtained by
Cassini/LP (nightside of Saturns magnetosphere)

• Statistics of the electron density show the
  importance of both
• External condition
• (solar wind)
• Internal condition
• (centrifugal force, plasma source from moons and
  rings)

Solar Wind
5
Dusty plasma of E-ring and EnceladusM. Morooka
et al. (IRFU)
E-ring
Ni ? Ne
Ni Ne
Ni Ne
Enceladus
6
Yamauchi (IRF-Kiruna)
equatorial plane
E
IMAGE (FUV)
Aurora
7
Liléo (KTH)
8
Arvelius (IRF-Kiruna)