Transport of Transient Solar Wind Particles in Earth's Cusps

Details Transport of Transient Solar Wind Particles in Earth's Cusps Transport of Transient Solar Wind Particles in Earth's Cusps

Dec 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008agufmsm44a..06p&link_type=abstract

American Geophysical Union, Fall Meeting 2008, abstract #SM44A-06

Physics

7513 Coronal Mass Ejections (2101), 7829 Kinetic Waves And Instabilities, 7839 Nonlinear Phenomena (4400, 6944)

Scientific paper

Where does the solar wind enter the Earth's magnetosphere? We report first observations of transient solar wind particles produced by solar disturbances (CMEs, for example) in the Earth's mid-altitude cusps (~5 RE) with densities nearly equal to those in the magnetosheath. The nearly equal density observed at mid- altitude cusps compared to those in the magnetosheath suggests the particles may be free streaming along B. An estimate of the number of particles entering the cusp for a one-hour transient using a typical RExRE cusp area yields ~1030 particles. An important question not answered by observations is what fraction remains in the magnetosphere or mirrors back to the magneto sheath. Modeling could tell us if any of these particles directly contribute to the ring current. The transient ions are moving parallel to the magnetic field (B) toward Earth and often coexist with ionospheric particles that are flowing out. Phase space distributions show a mixture of hot and cold electrons and multiple ion species including energetic O+ and ionospheric cold O+ beams accompanied by electromagnetic and broadband electrostatic emissions and Bernstein mode waves. These observations are not explained by any existing models and would require inductive effects induced by the solar wind interaction with the magnetosphere.

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