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@ARTICLE{Meier:824035,
      author       = {Meier, Patrick and Kriegel, Hendrik and Motschmann, Uwe and
                      Schmidt, Jürgen and Spahn, Frank and Hill, Thomas W. and
                      Dong, Yaxue and Jones, Geraint H.},
      title        = {{A} model of the spatial and size distribution of
                      {E}nceladus׳ dust plume},
      journal      = {Planetary and space science},
      volume       = {104},
      issn         = {0032-0633},
      address      = {Kidlington [u.a.]},
      publisher    = {Elsevier Science},
      reportid     = {FZJ-2016-06661},
      pages        = {216 - 233},
      year         = {2014},
      abstract     = {The structure of Enceladus׳ south polar plume of charged
                      dust is studied by simulations of the dust grain dynamics.
                      The model considers the Lorentz force and charging of the
                      grains by the plasma environment within the plume. Simulated
                      dust plumes are investigated by applying 10 selected sets of
                      dust parameters that include variations of the grain
                      production rate, the slope of the grain size distribution
                      and the start conditions (velocity, direction) of the
                      grains. The modeled dust plume profiles are in good
                      agreement with nanograin data of Cassini Plasma Spectrometer
                      (CAPS). Major results are (1) due to the local plasma
                      environment the nanograins are accelerated by the Lorentz
                      force and form a structured tail; (2) due to the finite
                      charging time the peak dust charge density is located about
                      0.3–0.6rE0.3–0.6rE below Enceladus׳ south pole; (3)
                      nanograins smaller than 10 nm are more than $99\%$ of the
                      produced dust; (4) CAPS data are best matched if the
                      nanograins are launched with high, collimated start
                      velocities; (5) the grain charging time is crucially
                      affected by inhomogeneities in the local plasma
                      environment.},
      ddc          = {620},
      pnm          = {899 - ohne Topic (POF3-899) / Plasma and Dust Simulations
                      on the Saturnian Rings $(hbs06_20111101)$},
      pid          = {G:(DE-HGF)POF3-899 / $G:(DE-Juel1)hbs06_20111101$},
      typ          = {PUB:(DE-HGF)16},
      doi          = {10.1016/j.pss.2014.09.016},
      url          = {https://juser.fz-juelich.de/record/824035},
}