Acceleration of the Solar Wind as a Result of the Reconnection of Open Magnetic Flux with Coronal Loops

Details Acceleration of the Solar Wind as a Result of the Reconnection of Open Magnetic Flux with Coronal Loops Acceleration of the Solar Wind as a Result of the Reconnection of Open Magnetic Flux with Coronal Loops

Sep 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003aipc..679..287f&link_type=abstract

SOLAR WIND TEN: Proceedings of the Tenth International Solar Wind Conference. AIP Conference Proceedings, Volume 679, pp. 287-2

Computer Science

1

Particle Emission, Solar Wind, Interplanetary Magnetic Fields, Solar Wind Plasma, Sources Of Solar Wind

Scientific paper

There are compelling observations of a clear anti-correlation between solar wind flow speed and coronal electron temperature, as determined from solar wind ionic charge states. A simple theory is presented which can account for these observations, including the functional form of the correlation: Solar wind flow speed squared varies essentially linearly as the inverse of the coronal electron temperature. In this theory, magnetic field lines in the corona that open into the heliosphere reconnect with coronal loops near their base. This process displaces the open field line, and disturbs and imparts energy into the overlying corona, thereby determining the Poynting vector into the corona. This process releases mass from the loop into the corona, and determines the mass flux of the solar wind. The Poynting and mass flux into the corona determine the final speed of the solar wind, and yield a relationship that provides an excellent fit to observations.

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