Magnetic and Optical Signatures of Pc 3-4 Waves in Relation to Wave Transmission at South Pole, Antarctica

Details Magnetic and Optical Signatures of Pc 3-4 Waves in Relation to Wave Transmission at South Pole, Antarctica Magnetic and Optical Signatures of Pc 3-4 Waves in Relation to Wave Transmission at South Pole, Antarctica

Dec 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005agufmsm43c1242q&link_type=abstract

American Geophysical Union, Fall Meeting 2005, abstract #SM43C-1242

Physics

2407 Auroral Ionosphere (2704), 2483 Wave/Particle Interactions (7867), 2706 Cusp, 2752 Mhd Waves And Instabilities (2149, 6050, 7836)

Scientific paper

A significant unresolved question in regard to Pc 3-4 (7-100 mHz) waves is the means by which such waves propagate to the high-latitude dayside ionosphere from their presumed origin upstream of the Earth's bow shock. Suggested mechanisms include equatorial entry via compressional waves, direct wave entry through the cusp, and indirect near-cusp entry via modulated precipitation of energetic particles. To further examine the latter mechanism, a correlation study was performed using data from search coil magnetometers, zenith-viewing photometers (427.8 and 630.0 nm), and an all-sky camera located at South Pole, Antarctica over a 153 day span in the Austral Winter of 2003. A statistical study was conducted in which the number of occurrences of Pc 3-4 waves seen in the x and y magnetic field components as well as in the two photometer signals was plotted as a function of local time. This showed a broad peak around 10:30 MLT for the magnetometer data and a sharper peak at the same time for the optical data. We found that when magnetic and optical signatures of Pc 3-4 pulsations were present at the same frequency and time, a brightened band in the poleward portion of the all-sky imager was present, most prominently at 630.0 nm. Such brightening was not seen when magnetic signatures of Pc 3-4 were present without corresponding optical pulsations. Selected events will be studied further to determine characteristic energy of precipitating particles and test whether their modulations are sufficient to produce the observed magnetic pulsations.

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