A model of solar wind and corona driven by high-frequency Alfvén waves

Details A model of solar wind and corona driven by high-frequency Alfvén waves A model of solar wind and corona driven by high-frequency Alfvén waves

Feb 1998

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998cha%26a..22...76z&link_type=abstract

Chinese Astronomy and Astrophysics, Volume 22, Issue 1, p. 76-82.

Astronomy and Astrophysics

Astrophysics

1

Scientific paper

The small-scale ejection events in the solar atmosphere detected in recent space observations have been regarded as manifestations of small-scale magnetic reconnection. But such reconnections generate high-frequency Alfvén waves. Based on this idea we set up a time-dependent, two-fluid model of coronal heating and solar wind acceleration. Numerical solutions are made, showing the time evolution, and including a discussion of their convergence and conservation properties. Under suitable assumptions regarding the generation of the waves in the transition zone, the numerical solution can explain a number of observations including coronal heating, the radial density profile of coronal holes, the acceleration of the wind near the bottom of the corona and the high-velocity streams observed at 0.3 au.

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