Origin of the Solar Wind and Open Coronal Magnetic Structures

Details Origin of the Solar Wind and Open Coronal Magnetic Structures Origin of the Solar Wind and Open Coronal Magnetic Structures

Jan 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004iaus..219..587h&link_type=abstract

Stars as suns : activity, evolution and planets, Proceedings of the 219th symposium of the International Astronomical Union held

Astronomy and Astrophysics

Astronomy

Scientific paper

Following Parker's theoretical prediction in 1958 of a subsonic-supersonic solar wind outflow from the Sun space observations soon confirmed its presence at Earth's orbit. The first EUV and X-ray observations of the Sun in the early 1970's revealed the complexity of coronal structures dominated by arch-like closed magnetic structures with the exception of dim regions named coronal holes where the EUV and X-ray emissions were significantly reduced. Based originally on the chance occurrence of reduced x-ray emission at the Sun with fast solar wind streams measured at Earth's orbit coronal holes were soon associated with regions of open magnetic flux and the source of the fast solar wind despite the absence of coronal magnetic field measurements. With the advent of radio occultation and white light measurements the first coronal velocity inferences from UVCS/SOHO the over-the-poles solar wind plasma measurements by Ulysses and polarimetric coronal measurements the widely held view that coronal holes are the sole source of the fast solar wind was revisited. These observations will be highlighted and evidence for the coexistence of open and closed magnetic structures throughout the corona and the implications for the source of the fast and the slow solar wind will be discussed.

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