% 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{Simon:824031,
      author       = {Simon, Sven and Kriegel, Hendrik and Saur, Joachim and
                      Wennmacher, Alexandre and Neubauer, Fritz M. and Roussos,
                      Elias and Motschmann, Uwe and Dougherty, Michele K.},
      title        = {{A}nalysis of {C}assini magnetic field observations over
                      the poles of {R}hea},
      journal      = {Journal of geophysical research},
      volume       = {117},
      number       = {A7},
      issn         = {0148-0227},
      address      = {Washington, DC},
      publisher    = {Union91972},
      reportid     = {FZJ-2016-06657},
      pages        = {A07211},
      year         = {2012},
      abstract     = {We analyze Cassini magnetic field observations from the
                      only two polar flybys of Saturn's largest icy satellite Rhea
                      (R2 on 02 March 2010 and R3 on 11 January 2011) which are
                      scheduled between Saturn Orbit Insertion and the end of the
                      mission in 2017. For the interpretation of these data, we
                      apply estimations from simple analytical models as well as
                      results from numerical hybrid simulations (kinetic ions,
                      fluid electrons) of Rhea's interaction with the incident
                      magnetospheric plasma. In-situ observations of exospheric
                      neutral gas and pick-up ions suggest Rhea to be embedded in
                      a tenuous gas envelope. However, the interaction of this gas
                      with the magnetospheric flow does not make any measurable
                      contributions to the magnetic field perturbations detected
                      above the poles of the moon. Instead, the field
                      perturbations observed in these regions mainly arise from
                      the absorption of magnetospheric particles with large
                      field-aligned velocities, impinging on the north and south
                      polar surface of Rhea. In addition to numerous interaction
                      features known from preceding Cassini flybys of Saturn's
                      plasma-absorbing moons, the magnetic field data acquired
                      above Rhea's poles reveal perturbations of the flow-aligned
                      field component, corresponding to a draping/Alfvén wing
                      pattern. Based on our hybrid simulations, we suggest that
                      these signatures arise from the finite extension of Rhea's
                      wakeside plasma void along the corotational flow direction,
                      yielding a density gradient in corotation direction, and
                      thereby generating a diamagnetic current from the
                      Saturn-facing into the Saturn-averted hemisphere of the
                      moon. This transverse current is responsible for generating
                      a weak Alfvén wing pattern at Rhea which has been detected
                      by the Cassini spacecraft during the R2 and R3 flybys. Due
                      to the large gyroradii of the incident magnetospheric ions,
                      this structure features a pronounced asymmetry with respect
                      to the direction of the convective electric field. Results
                      of our simulation, considering only plasma absorption on the
                      moon, are in good agreement with Cassini magnetometer data
                      from both flybys. At Saturn's icy satellites Tethys and
                      Dione, the low value of the magnetospheric plasma beta most
                      likely prevents the formation of similar currents and
                      measurable flow-aligned magnetic field distortions.},
      cin          = {NIC},
      ddc          = {550},
      cid          = {I:(DE-Juel1)NIC-20090406},
      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},
      UT           = {WOS:000306701600005},
      doi          = {10.1029/2012JA017747},
      url          = {https://juser.fz-juelich.de/record/824031},
}