The nature of convectively unstable waveguide mode disturbances on the magnetospheric flanks

Details The nature of convectively unstable waveguide mode disturbances on the magnetospheric flanks The nature of convectively unstable waveguide mode disturbances on the magnetospheric flanks

Sep 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002jgra..107.1242w&link_type=abstract

Journal of Geophysical Research (Space Physics), Volume 107, Issue A9, pp. SMP 14-1, CiteID 1242, DOI 10.1029/2001JA005091

Physics

Plasma Physics

4

Magnetospheric Physics: Mhd Waves And Instabilities, Magnetospheric Physics: Solar Wind/Magnetosphere Interactions, Space Plasma Physics: Kinetic And Mhd Theory, Space Plasma Physics: Waves And Instabilities

Scientific paper

Convectively unstable disturbances are often described in terms of propagating wave packets that grow and broaden. We extend such a description here and show how it recovers previous results and agrees with simulations. Applying these ideas to the magnetospheric flanks, we find that such wave packets will often not provide a driver of long enough duration for establishing a fully formed field line resonance (FLR). This suggest that the alternative description of the convective instability as a steady wave train radiated by a fixed source may be more appropriate for the flanks on some occasions. Whether the unstable waveguide modes prefer to exist as steady wave trains or convecting wave packets can have important implications for identifying the mechanisms through which the magnetosheath is coupled to the magnetosphere.

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