1. Calculation of Intermittency in the Photosphere and Corona from Hinode Data Valentina I. Abramenko And Vasyl B. Yurchyshyn Big Bear Solar Observatory of NJIT

2. Spatial Domain Temporal Domain Non-intermittent NetworkIntermittent Network What is the intermittency look like? time

3. Intermittency as derived from the Structure Functions 2D: x=(x1,x2) r u(x) u(x+r) x1 x2 1D: x=t time u(t)u(t+τ) τ

4. Flatness function as an indicator of intermittency Flatness function as an indicator of intermittency power law Fatness F( r ) is a constant for a non-intermittent variable and grows as a power law when scale r vanishes for an intermittent variable: Inertial range Scale, r F( r ) ~ r -κ-κ F( r ) =S ( r ) / (S ( r ) ) 6 3 2 The intermittency index κ κ

5. NOAA 10930: sole on the solar disk 2007

6. NOAA 10930: intermittency in the corona Three subsets of Hinode XRT/Be-Thin area-integrated flux: Time Series Dec 10 Dec 13 Dec 11

7. NOAA 10930: intermittency in the corona Three subsets of Hinode XRT/Be-Thin area-integrated flux: Flatness Functions

8. NOAA 10930: intermittency in the corona Five subsets of Nobeyama Radioheliograph data: polarization at 9.4 GHz, Time Series

9. NOAA 10930: intermittency in the corona Five subsets of Nobeyama Radioheliograph data: polarization at 9.4 GHz, Time Series

10. NOAA 10930: photospheric intermittency Hinode SOT/FG magnetogram To calculate intermittency in the photosphere, we utilized 2D magnetic field images derived with Hinode SOT/FG instrument. The covered time interval: 2006 Dec 8/12:00 UT to 2006 Dec 13/18:45 UT. Advantages: high resolution, high time cadence, uninterrupted measurements for several days

11. NOAA 10930: intermittency in the photosphere and corona

12. Photospheric kinetic vorticity

14. Conclusion Highly non-Gaussian, intermittent character of the magnetic fields in the both photosphere and corona; The data allow to suggest that intermittency is preliminary stored in the photosphere and then it is transported into the chromosphere/corona.