Solar Wind Excitation of Magnetospheric ULF Waves

Details Solar Wind Excitation of Magnetospheric ULF Waves Solar Wind Excitation of Magnetospheric ULF Waves

May 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005agusmsa11a..03r&link_type=abstract

American Geophysical Union, Spring Meeting 2005, abstract #SA11A-03

Other

2736 Magnetosphere/Ionosphere Interactions, 2784 Solar Wind/Magnetosphere Interactions

Scientific paper

We use global simulations of the magnetosphere-ionosphere system to investigate how the solar wind and the interplanetary magnetic field couple ULF wave energy into the magnetosphere, how the energy is converted and travels into the ionosphere, and how these processes depend on parameters like the wave frequency and the dipole tilt. We find that (i) SW density fluctutions couple more efficiently to the magnetosphere than IMF fluctuations, (ii) fluctuations are more effectively coupled to the magnetosphere during northward IMF, (iii) fluctuations are are more effectively coupled to the magnetosphere during solstice compared to equinox, (iv) the primary entry channels for the wave energy are the cusps, but there can also be other hot spots in the ionosphere that receive disproportionate amounts of wave power, and (v) there is a distinct difference between the small amplitude regime which causes a linear response, and the large amplitude regime which leads to non-linear phenomena such as line broadening and harmonics.

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