Physics
Scientific paper
Dec 2009
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009agufm.p21a1207k&link_type=abstract
American Geophysical Union, Fall Meeting 2009, abstract #P21A-1207
Physics
[2756] Magnetospheric Physics / Planetary Magnetospheres, [2772] Magnetospheric Physics / Plasma Waves And Instabilities, [5440] Planetary Sciences: Solid Surface Planets / Magnetic Fields And Magnetism, [6235] Planetary Sciences: Solar System Objects / Mercury
Scientific paper
When an incident compressional wave propagates across an Alfven velocity gradient in multi-fluid plasmas, the compressional wave can couple with the Alfven resonance for lower frequency (below the heavy ion gyrofrequency) and/or the ion-ion hybrid (IIH) resonance for higher frequency (between ion gyrofrequencies). Recently, a wave simulation in electron-hydrogen-sodium plasmas suggested that the field line resonance at Mercury is expected to occur when the IIH and/or Alfven resonance conditions are satisfied [Kim et al., 2008]. However, the relative efficiency of wave energy absorption at these resonances and eigenmodes of the field line resonance have not been studied in the context of Mercury's magnetosphere. To understand the efficiency of wave absorption, we evaluate absorption coefficients at the IIH and Alfven resonances for variable concentrations of sodium, ηNa = NNa / Ne, where Nj is number density for particle species j, and azimuthal wave number, ky. By adopting Mercury’s realistic magnetosphere model, eigenmodes of field line resonance are calculated for variable ηNa in radial and/or field aligned directions. We also discuss applications of our results to MESSENGER observations.
Johnson Jesse
Kim Erik
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