Alfvén waves in the solar corona, the solar wind, and the magnetosphere

Details Alfvén waves in the solar corona, the solar wind, and the magnetosphere Alfvén waves in the solar corona, the solar wind, and the magnetosphere

Dec 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004agufmsm44a..02o&link_type=abstract

American Geophysical Union, Fall Meeting 2004, abstract #SM44A-02

Physics

7509 Corona, 7511 Coronal Holes, 7807 Charged Particle Motion And Acceleration, 7827 Kinetic And Mhd Theory, 7839 Nonlinear Phenomena

Scientific paper

Observations and theoretical models show that Alfvén waves play an important role in many physical processes taking place in the plasma of the "local cosmos." For example, Alfvén waves are still the major candidates for the acceleration and heating of the fast solar wind, since they were proposed nearly 4 decades ago. Recently, MHD waves were observed in coronal loops in the EUV with the TRACE satellite. The SOHO, and TRACE instrument provide evidence for slow magnetosonic waves in coronal plumes. In-situ Helios and Ulysses spacecraft find ample evidence for the presence of propagating Alfvén waves in the solar wind. The CLUSTER mission provides for the first time multi-point view of the magnetospheric and solar wind plasma environment, and in particular high cadence magnetic field measurements with the Fluxgate Magnetometer (FGM), that enables to study the properties of Alfvén waves in various parts of the magnetosphere simultaneously. I will discuss the observations and modeling of Alfvén waves starting from the low corona (loops), continuing into the solar wind, the magnetosphere, and to the auroral ionosphere. I will present the results of MHD, multifluid, and hybrid models of low-frequency (MHD), as well as kinetic Alfvén waves in the plasma in various parts of the "local cosmos", and I will discuss the role Alfvén waves play in the energization of the plasma, and as a diagnostic tool of the plasma physical processes.

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