Active Region and Coronal Holes Sources of Solar Wind at Solar Activity Maximum

Details Active Region and Coronal Holes Sources of Solar Wind at Solar Activity Maximum Active Region and Coronal Holes Sources of Solar Wind at Solar Activity Maximum

Dec 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002agufmsh52a0459l&link_type=abstract

American Geophysical Union, Fall Meeting 2002, abstract #SH52A-0459

Physics

2164 Solar Wind Plasma, 2169 Sources Of The Solar Wind, 7509 Corona, 7511 Coronal Holes, 7536 Solar Activity Cycle (2162)

Scientific paper

Previous studies of the photospheric source regions of solar wind near solar maximum showed that solar wind comes from open flux in active regions as well as from the familiar coronal hole sources. To understand the relationship between solar wind sources and coronal magnetic structure, we compare the coronal hole and active regions solar wind sources as imaged in various wavelengths: He 10830 Å (the traditional coronal hole diagnostic), EUV (SOHO EIT lines) and soft X- rays (Yohkoh). The various wavelengths presumably show closed loops of different temperatures and/or heights and we will compare the images with the coronal magnetic structure predicted by potential source surface models. The determination of the solar wind source regions were made using a two-step magnetic mapping of solar wind sampled at ACE and Ulysses to the photosphere (1). A solar wind source was labeled an active region source when there was no corresponding coronal hole in the He 10830 Å synoptic maps. Using ACE data, we also found that the solar wind from these active region sources generally has a higher Oxygen charge state than wind from the Helium-10830\x8F coronal hole sources, indicating a hotter source region, consistent with the active region source interpretation. Further investigation of active region sources in the four Carrington rotations analyzed showed that, although no coronal hole is identified in the 10830 Å synoptic maps, often a dark lane or hole is seen in SOHO EIT or YOHKOH SXT images near the location of the active region source. We address the question of which wavelength synoptic maps are the best indicator of solar wind source regions. (1) Neugebauer, M. et al. ``Sources of the Solar Wind at Solar Activity Maximum," (JGR, in press, 2002)

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