HR: 15:30h
AN: SH24A-01    [Abstracts]
TI: Observed and Modeled Coronal Holes
AU: * de Toma, G
EM: detoma@ucar.edu
AF: NCAR High Altitude Obs., 3450 Mitchell Lane, BOULDER, CO 80301 United States
AU: Arge, C N
EM: Nick.Arge@hanscom.af.mil
AF: AFRL/VSBXS, 29 Randolph Road, Hanscom AFB, MA 01731 United States
AU: Riley, P
EM: pete@peteriley.org
AF: SAIC, 10260 Campus Point Drive, San Diego, CA 92121 United States
AB: 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.)
DE: 2169 Sources of the solar wind
DE: 7509 Corona
DE: 7511 Coronal holes
DE: 7524 Magnetic fields
SC: SPA-Solar and Heliospheric Physics [SH]
MN: 2005 Joint Assembly