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Lundstedt (IRF-Lund)

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. The distribution of the Martian proton number density at the dayside.

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Lundstedt (IRF-Lund)

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  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 Saturn’s magnetosphere M. Morooka et al. (IRFU) The electron density model obtained by Cassini/LP (nightside of Saturn’s 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)

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