Astronomy and Astrophysics – Astrophysics
Scientific paper
Nov 2006
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006ihy..worke..43p&link_type=abstract
2nd UN/NASA Workshop on International Heliophysical Year and Basic Space Science. Proceedings of the conference held 27 Novembe
Astronomy and Astrophysics
Astrophysics
Scientific paper
It is well known that the fast solar wind originates from coronal holes, but its source close to the solar 'surface' has been a matter of debate even in today's era of modern solar observations. Recently, it has been suggested that the fast solar wind outflow starts at about 10 kilometers per second in coronal funnels, which are located at the edges of the chromospheric magnetic network inside coronal holes. We present further evidence that the outflow might also originate from above 'explosive event' sites. These jets have a lifetime of about 5 minutes and are often seen reoccurring at the same location over intervals of typically 20-30 minutes. Although the expelled jets might actually extend high in the Sun's atmosphere, they are not seen in the intensity on the disk. Some of the transparent features might nevertheless appear as macrospicules at the Sun's edge. This observation itself is shedding new light onto another long- standing question regarding the nature of macrospicules. These results about the small-scale structures of coronal holes and their consequence on explaining the nature of the fast solar wind have been derived due to an innovative way of extracting information from the spectral data offered by SOHO’s highest resolution detector, SUMER. The 'secret' of our technique lies in understanding plasma properties from the signature it leaves in the shape and widths of the spectral lines.
Banerjee Dipti
Doyle Gerry J.
Popescu Miruna-Daniela
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