1. Magnetic Field and Heating of the Corona Valentyna Abramenko and Vasyl Yurchyshyn Big Bear Solar Observatory

2. Soft X-ray luminosity of the corona

3. Active Regions: Total unsigned magnetic flux versus Soft X-ray flux Abramenko, Pevtsov, Romano 2006

4. Structural parameters of the magnetic field versus the area-averaged X-ray flux in the Al1.1 channel Abramenko, 2007

5. Time variations of the power index and flatness index from SOT/FG/Hinode magnetograms for NOAA 10930 Abramenko & Yurchyshyn, 2007

6. Poynting Flux vs X-ray Flux: area-averaged values Follow-up study: Tan, Jing, Abramenko, Pevtsov, Song, Park, Wang, 2007 ApJ Poynting Flux ~ B h B z V h B z B z V h

7. Total unsigned magnetic flux versus X-ray luminosity for different objects Pevtsov et al. 2003

8. Coronal Holes: Magnetic flux versus the corresponding solar wind speed Abramenko & Yurchyshyn 2007

9. ConclusionsConclusions Energy input due to the random motions strongly correlates with brightness, temperature and emission measure of the corona. Energy input due to the random motions strongly correlates with brightness, temperature and emission measure of the corona. Energy flux is (1 ÷ 14)×10 6 erg cm -2 s -1, which is quite sufficient to heat the corona above ARs. Energy flux is (1 ÷ 14)×10 6 erg cm -2 s -1, which is quite sufficient to heat the corona above ARs. Magnetic diffusivity in ARs is, which is twice lower than in QS areas. Magnetic diffusivity in ARs is (150 ÷ 300) km 2 /s, which is twice lower than in QS areas.

10. Magnetic dissipation versus temperature and emission measure

11. Magnetic dissipation versus averaged flux in Al.1 and AlMgMn channels Flux density (Al.1) Flux density (AlMgMn)