Physics
Scientific paper
May 2002
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002agusmsm32a..10c&link_type=abstract
American Geophysical Union, Spring Meeting 2002, abstract #SM32A-10
Physics
2740 Magnetospheric Configuration And Dynamics, 2752 Mhd Waves And Instabilities, 2764 Plasma Sheet, 2788 Storms And Substorms, 7827 Kinetic And Mhd Theory
Scientific paper
Ballooning modes and field line resonances are critical issues in understanding substorm onset and auroral arc formation. Based on the AMPTE/CCE observations [Cheng and Lui, GRL, 1998], a low frequency instability with period on the order of 1 min is identified as a kinetic ballooning instability near the end of the late growth phase before the substorm onset. Although kinetic effects are essential for ballooning modes, it is important to first understand the stability property and mode structure of ideal MHD ballooning modes. Moreover, auroral substorm breakup starts usually from a localized location in a pre-existing arc. Field line resonance has been considered as a primary mechanism for the auroral arc formation. The theoretical formation and numerical solutions of ballooning modes and field line resonances for 3D magnetospheric magnetic fields are still being actively pursued. Here, we present analytical formulation and numerical solutions of MHD ballooning modes and field line resonances in 3D magnetic fields including the coupling effects between perpendicular and parallel (compressional) perturbed magnetic fields. The numerical calculations make use of numerical 3D magnetospheric equilibria including thin current sheet by assuming pressure to be constant along a field line. Ideas on the relationship between the ballooning instability and field line resonances will be discussed.
Cheng C. Z.
Zaharia Sorin
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