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Session 7 - Corona II.
Oral session, Saturday, June 28
Ballroom A, Chair: Fran Bagenal
Observations at 1.15 R_\sun of the forebidden coronal lines Fe XIV 530.3 nm and Fe X 637.4 nm obtained at the National Solar Observatory at Sacramento Peak are used to determine the variation of coronal temperature at high latitudes during Cycle 22. An unexpected pattern, symmetric about solar maximum and consistent between the northern and southern hemisphere, is seen. Beginning near solar minimum in 1985, the temperature above 60\deg latitude is seen to be at a minimum value, varying from about 1.3 MK near the poles to about 1.5 MK near 60\deg. Near the time that the "Rush-to-the-Poles" begins in 1987, the high-latitude temperature increases abruptly, reaching values of 1.7 MK at the North pole and 1.6 MK at the South pole in 1989. After 1990, the process reverses, and temperatures at the poles are below 1.3 MK by 1995. This pattern may be consistent with the latitude variations of polar-crown prominences. The author was supported by the Air Force Office of Scientific Research.
The author(s) of this abstract have provided an email address for comments about the abstract: altrock@sunspot.noao.edu
