Lundstedt (IRF-Lund)

Narayan (Stockholm-U)

Kanao (ISAS, Japan)The effect of the crustal magnetic field on the distribution of the ion number density around Mars

E is southern direction.Crustal magnetic field is in Eup hemisphere

E is northern direction Crustal magnetic field is in Edown hemisphere

The distribution of the Martian proton number density at the daysideM. Kanao, A. Yamazaki, Y. Futaana, T. Abe, M. Nakamua, S. Barabash,A. Fedorov, M. Franz, and ASPERA-3 Team

Only In the case when the crustal magnetic field is in the Eup hemisphere, the proton number density increases.

Statistics of the electron density show the importance of both

• External condition (solar wind)

• Internal condition(centrifugal force, plasma source from moons and rings)

The electron density model obtained by Cassini/LP

(nightside of Saturn’s magnetosphere)

Solar Wind

Co-rotating dynamics ofSaturn’s magnetosphere

M. Morooka et al. (IRFU)

Morooka (IRF-Uppsala)

Dusty plasma of E-ring and Enceladus

M. Morooka et al. (IRFU)

Ni ≈ Ne Ni ≈ Ne

Enceladus

E-ring

Ni ≠ Ne

IMAGE(FUV)

E

Aurora

equatorial plane

Yamauchi (IRF-Kiruna)

Liléo (KTH)

Arvelius (IRF-Kiruna)