Magnetic field evolution in a coronal hole

Details Magnetic field evolution in a coronal hole Magnetic field evolution in a coronal hole

Aug 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006iaujd...3e..41z&link_type=abstract

Solar Active Regions and 3D Magnetic Structure, 26th meeting of the IAU, Joint Discussion 3, 16-17 August, 2006, Prague, Czech R

Physics

Scientific paper

Using Big Bear Solar Observatory (BBSO) and SOHO observations, we explore the magnetic evolution and temperature variation in a coronal hole during its appearing and disappearing phases. The following results are obtained: (1) In the early phase of the coronal hole formation, more than 65 % of the magnetic flux is negative, and coronal temperature, estimated from the ratio of EIT 195 and 171 Å images, is 1.05×10^6 K in the hole. (2) In the end phase of the hole, about 55% of the magnetic flux is negative, and the temperature increases to 1.10×10^6 K. Our results display that in a coronal hole, there is a connection between magnetic evolution and coronal temperature, the coronal temperature increases while the magnetic imbalance of the both polarities decreases.

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