calculation of the linear growth rate of Rayleigh-Taylor instability

Details calculation of the linear growth rate of Rayleigh-Taylor instability calculation of the linear growth rate of Rayleigh-Taylor instability

Dec 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005agufmsa23a0302p&link_type=abstract

American Geophysical Union, Fall Meeting 2005, abstract #SA23A-0302

Physics

2411 Electric Fields (2712), 2415 Equatorial Ionosphere, 2437 Ionospheric Dynamics, 2439 Ionospheric Irregularities, 2467 Plasma Temperature And Density

Scientific paper

For solar maximum conditions, we have computed the linear growth rate of Rayleigh-Taylor instability in each season in every longitude sector with a cell size of 30 degrees. The electric field data in Scherliess and Fejer [1999], Mass Spectrometer Incoherent Scatter (MSIS) Model and International Reference Ionosphere (IRI) Model were used for the calculation, but the vertical wind term was omitted due to its large variability. First, the computed growth rate was compared with the topside bubble encounter of KOrea Multi-Purpose SATellite-1 (KOMPSAT-1) at the altitude of 680 km at 2230 LT. Second, the calculated Pedersen conductivity and the conductivity ratio were contrasted with the observed ambient density that had been averaged for a given location and season. The calculated results showed considerable departure from the topside observation of KOMPSAT-1. Third, relative importance was examined for each term that constitutes the linear growth rate. Among those terms the ambient electric field manifested the largest variation, while the vertical density gradient and the Pedersen conductivity ratio also had considerble importance in making the variation of the linear growth rate.

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