Observed and Modeled Coronal Holes

Details Observed and Modeled Coronal Holes Observed and Modeled Coronal Holes

May 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005agusmsh24a..01d&link_type=abstract

American Geophysical Union, Spring Meeting 2005, abstract #SH24A-01

Physics

2169 Sources Of The Solar Wind, 7509 Corona, 7511 Coronal Holes, 7524 Magnetic Fields

Scientific paper

We combine relative intensity images of the solar chromosphere and corona with magnetograms to identify coronal hole regions on the Sun. We compare them with the coronal holes - defined as the foot-points of magnetically open field lines - derived with two different coronal models: a PFSS model (Arge and Pizzo, 2000) and a 3D MHD model (Riley, Linker, and Mikic, 2001) that use the same magnetic field maps as photospheric boundary. The fraction of the observed coronal holes found by coronal models gives us a means to validate how well models reproduce observations. Cases for different level of solar activity during solar cycle 23 are presented and discussed. (This work is supported by CISM, which is funded by the STC program of the National Science Foundation under Agreement Number ATM-0120950.)

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