Field Line Resonance conjugate studies in the dayside inner magnetosphere using SAMBA antarctic magnetometers and THEMIS mission probes

Details Field Line Resonance conjugate studies in the dayside inner magnetosphere using SAMBA antarctic magnetometers and THEMIS mission probes Field Line Resonance conjugate studies in the dayside inner magnetosphere using SAMBA antarctic magnetometers and THEMIS mission probes

Dec 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011agufmsa51d1975p&link_type=abstract

American Geophysical Union, Fall Meeting 2011, abstract #SA51D-1975

Physics

[2700] Magnetospheric Physics, [2730] Magnetospheric Physics / Magnetosphere: Inner, [2752] Magnetospheric Physics / Mhd Waves And Instabilities

Scientific paper

To test the robustness of the automated Field Line Resonance (FLR) technique described by [Boudouridis and Zesta 2007], and commonly used for the estimation of the plasma density in the inner magnetosphere, conjugate studies between the SAMBA magnetometer array and the THEMIS satellite were performed. An excellent conjunction, with a duration of nearly 40 minutes, between Escudero (ESC) and O'Higgins (OHI) antarctic fluxgate magnetometers from SAMBA and three probes from THEMIS was found on June 16, 2007. It is shown that the amplitude ratio method for the estimation of the frequency of resonance is more reliable than the phase difference method. For the amplitude ratio method we found time intervals in which we have the same resonance frequency in both ground and space measurements. We also compared this estimation with the in-situ ion number density measurements from the THEMIS satellites. It was found that the plasma density obtained from the FLR frequency is more fluctuating than the ion number density observed by THEMIS ESA and SST instruments. The time intervals for wich the plasma density and the number density are strongly correlated are much shorter than the intervals of high correlation between ground and space field line resonance frequencies. We investigate if the difference can be attributed to the orbital and/or ion composition effects.

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