% IMPORTANT: The following is UTF-8 encoded.  This means that in the presence
% of non-ASCII characters, it will not work with BibTeX 0.99 or older.
% Instead, you should use an up-to-date BibTeX implementation like “bibtex8” or
% “biber”.

@ARTICLE{Roussos:824034,
      author       = {Roussos, E. and Kollmann, P. and Krupp, N. and Paranicas,
                      C. and Krimigis, S. M. and Mitchell, D. G. and Persoon, A.
                      M. and Gurnett, D. A. and Kurth, W. S. and Kriegel, H. and
                      Simon, S. and Khurana, K. K. and Jones, G. H. and Wahlund,
                      J.-E. and Holmberg, M. K. G.},
      title        = {{E}nergetic electron observations of {R}hea’s
                      magnetospheric interaction},
      journal      = {Icarus},
      volume       = {221},
      number       = {1},
      issn         = {0019-1035},
      address      = {Orlando, Fla.},
      publisher    = {Academ. Press},
      reportid     = {FZJ-2016-06660},
      pages        = {116 - 134},
      year         = {2012},
      note         = {Welcher Autor ist denn vom Forschungszentrum?},
      abstract     = {Saturn’s moon Rhea is thought to be a simple plasma
                      absorber, however,energetic particle observations in its
                      vicinity show a variety ofunexpected and complex interaction
                      features that do not conform withour current understanding
                      about plasma absorbinginteractions. Energetic electron data
                      are especially interesting, asthey contain a series of broad
                      and narrow flux depletions on eitherside of the moon’s
                      wake. The association of these dropouts withabsorption by
                      dust and boulders orbiting within Rhea’s Hill sphere
                      wassuggested but subsequently not confirmed, so in this
                      study we reviewdata from all four Cassini flybys of Rhea to
                      date seeking evidence foralternative processes operating
                      within the moon’s interactionregion. We focus on energetic
                      electron observations, which we put incontext with
                      magnetometer, cold plasma density and energetic iondata. All
                      flybys have unique features, but here we only focus
                      onseveral structures that are consistently observed. The
                      mostinteresting common feature is that of narrow dropouts in
                      energeticelectron fluxes, visible near the wake flanks.
                      These are typicallyseen together with narrow flux
                      enhancements inside the wake. Aphase-space-density analysis
                      for these structures from the first Rheaflyby (R1) shows
                      that Liouville’s theorem holds, suggesting that theymay be
                      forming due to rapid transport of energetic electrons from
                      themagnetosphere to the wake, through narrow channels. A
                      series ofpossibilities are considered to explain this
                      transport process. Weexamined whether complex energetic
                      electron drifts in the interactionregion of a plasma
                      absorbing moon (modeled through a hybrid simulationcode) may
                      allow such a transport. With the exception of
                      severalfeatures (e.g. broadening of the central wake with
                      increasing electronenergy), most of the commonly observed
                      interaction signatures inenergetic electrons (including the
                      narrow structures) were notreproduced. Additional dynamical
                      processes, not simulated by thehybrid code, should be
                      considered in order to explain the data. Forthe small scale
                      features, the possibility that a flute
                      (interchange)instability acts on the electrons is discussed.
                      This instability isprobably driven by strong gradients in
                      the plasma pressure and themagnetic field magnitude:
                      magnetometer observations show clearlysignatures consistent
                      with the (expected) plasma pressure loss due toion
                      absorption at Rhea. Another potential driver of the
                      instabilitycould have been gradients in the cold plasma
                      density, which are,however, surprisingly absent from most
                      crossings of Rhea’s plasmawake. The lack of a density
                      depletion in Rhea’s wake suggests thepresence of a local
                      cold plasma source region. Hybrid plasmasimulations show
                      that this source cannot be the ionized component ofRhea’s
                      weak exosphere. It is probably related to
                      acceleratedphotoelectrons from the moon’s negatively
                      charged surface, indicatingthat surface charging may play a
                      very important role in shaping Rhea’smagnetospheric
                      interaction region.},
      ddc          = {520},
      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.icarus.2012.07.006},
      url          = {https://juser.fz-juelich.de/record/824034},
}