Ion Cyclotron Instabilities in Multicomponent Coronal Hole Plasma with Cross-Field Streaming Species

Details Ion Cyclotron Instabilities in Multicomponent Coronal Hole Plasma with Cross-Field Streaming Species Ion Cyclotron Instabilities in Multicomponent Coronal Hole Plasma with Cross-Field Streaming Species

May 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001agusm..sh22e10m&link_type=abstract

American Geophysical Union, Spring Meeting 2001, abstract #SH22E-10

Other

2164 Solar Wind Plasma, 7511 Coronal Holes, 7867 Wave/Particle Interactions, 7871 Waves And Instabilities

Scientific paper

It is well known that ion cyclotron instability driven by cross-field streaming of the plasma components, with zero or nonzero net current, can be excited at relative velocities of the species much smaller than the ion thermal velocity. We use this instability as a mechanism of generation of ion cyclotron waves in coronal holes. In previous work, we have demonstrated that, given the scales of spatial inhomogeneity suggested by observations and reasonably large magnetic field fluctuations, the instability can be excited by the cross-field current in an electron-proton plasma. We now extend our work to include other ion species. We show that the abundance of helium is large enough for the generation of helium cyclotron waves, while the excitation of minor-ion cyclotron waves would require unrealistically large streaming velocities. Nevertheless, the minor ions can resonantly interact with the waves existing in the electron-hydrogen-helium plasma. The important property of the waves induced by the cross-field streaming is that they propagate almost perpendicular to the background magnetic field. One of the consequences of this fact is a considerable Doppler shift of the wave frequency in the frames of reference connected with different plasma components. We will discuss how the resonant wave particle interaction is modified in this case compared to the case of parallel-propagating waves with no streaming of the species.

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