The Structure of the Solar Corona 1999-2002

Details The Structure of the Solar Corona 1999-2002 The Structure of the Solar Corona 1999-2002

Apr 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003eaeja.....1183a&link_type=abstract

EGS - AGU - EUG Joint Assembly, Abstracts from the meeting held in Nice, France, 6 - 11 April 2003, abstract #1183

Physics

Scientific paper

The LASCO C2 and C3 coronagraphs have been recording a regular sequence of images of the solar corona at height range of 2.5 to greater than 30 Rs. Since the middle of 1999, the typical cadence has been 3 C2 and 2 C3 images per hour. This sequence of images clearly shows the changes in coronal structure during the approach to solar maximum, at the maximum of solar activity, and during the decline form solar maximum. There is a striking asymmetry in coronal brightness beginning in early 2000 and continuing till mid 2002. The corona above the North Pole brightens rapidly during 1999 with peak brightness observed in early 2000. The southern coronal brightness does not peak until late 2000. This asymmetry has continued with the corona above the South Pole being much brighter than observed in the north.

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