Fluid/Kinetic: Investigations of the Dynamic Solar Wind

Details Fluid/Kinetic: Investigations of the Dynamic Solar Wind Fluid/Kinetic: Investigations of the Dynamic Solar Wind

May 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010aas...21611401k&link_type=abstract

American Astronomical Society, AAS Meeting #216, #114.01; Bulletin of the American Astronomical Society, Vol. 41, p.906

Physics

Scientific paper

The supersonic solar wind originates in the hot solar corona and expands through interplanetary space, interacting with planets and carving the heliospheric bubble out of the interstellar medium. We can use direct exploration of the solar wind with instrumented spacecraft to understand the solar wind and as a laboratory for investigating the physics of magnetized astrophysical plasmas. Many of our open questions about fundamental physical processes such as heating, particle acceleration, angular momentum transport, and the production of magnetic fields require an understanding of the kinetic physics of non-Maxwellian plasmas in regimes where fluid physics breaks down. This talk will review current research at this fluid/kinetic interface, including joint measurements of particles and electromagnetic waves in the solar wind and what we have learned about heating, instabilities, and energy flow. Examples of the application of these results to more distant objects such as jets, accretion disks, and galactic dynamos will be presented. Some potential future work will be discussed, including understanding energy flow between ions and electrons and the exciting potential for direct measurements of the solar corona with the proposed NASA Solar Probe Plus mission.

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