Solar Wind Scaling Law

Details Solar Wind Scaling Law Solar Wind Scaling Law

Dec 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003apj...599.1395s&link_type=abstract

The Astrophysical Journal, Volume 599, Issue 2, pp. 1395-1403.

Astronomy and Astrophysics

Astronomy

45

Sun: Solar Wind, Sun: Corona

Scientific paper

We derive a simple, robust scaling law, which explains naturally how the well-known anticorrelation between final solar wind speed and freezing-in temperature results from the loss of radiated energy in the corona. Furthermore, 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 paper reveals an underlying connection between the solar wind and its coronal source.

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