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Lundstedt (IRF-Lund)

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Narayan (Stockholm-U)

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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 E up hemisphere E is northern direction Crustal magnetic field is in E down hemisphere 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 Only In the case when the crustal magnetic field is in the E up hemisphere, the proton number density increases.

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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 of Saturn’s magnetosphere M. Morooka et al. (IRFU) Morooka (IRF-Uppsala)

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Dusty plasma of E-ring and Enceladus M. Morooka et al. (IRFU) Ni ≈ Ne Enceladus E-ring Ni ≠ Ne

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IMAGE (FUV) E Aurora equatorial plane Yamauchi (IRF-Kiruna)

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Liléo (KTH)

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Arvelius (IRF-Kiruna)

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