Solar Wind Scaling Law

Details Solar Wind Scaling Law Solar Wind Scaling Law

Dec 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003agufmsh11d1134s&link_type=abstract

American Geophysical Union, Fall Meeting 2003, abstract #SH11D-1134

Physics

2164 Solar Wind Plasma, 2169 Sources Of The Solar Wind, 7509 Corona, 7511 Coronal Holes, 7847 Radiation Processes

Scientific paper

We discuss a simple, robust scaling law, which explains naturally how the well-known anti-correlation between final solar wind speed and freezing-in temperature results from loss of radiated energy in the corona. Further, if the Sun injects roughly fixed electromagnetic energy per particle, this law provides a unified theory for the source of solar wind: fast tenuous solar wind from dark coronal holes; slow dense wind from hotter, brighter regions; and bound but unstable plasma in extremely hot regions, which may be related to solar transients. The scaling law is not an extension, or a new variant of previous solar wind models, but rather, a requirement on all solar wind models, which should apply quite generally to magnetically driven winds. Thus, this presentation reveals an underlying connection between the solar wind and its coronal source.

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