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Intermittency in the Photosphere and Corona as Derived from Hinode Data

This study examines the intermittent behavior of the magnetic fields in the photosphere and corona using data from the Hinode satellite. Results suggest a direct connection between the complex dynamics of the photosphere and the corona, offering new possibilities for photosphere/corona coupling.

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Intermittency in the Photosphere and Corona as Derived from Hinode Data

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  1. Intermittency in the Photosphere and Corona as Derived from Hinode Data Valentina Abramenko Vasyl Yurchyshyn Big Bear Solar Observatory of NJIT Haimin Wang CSTR/NJIT

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

  3. Magnetic field in NOAA10930 from Hinode/SOT/FG • Extended spatial/temporal intervals of low activity are intermittent • with compact intervals of enhanced activity. • Intermittency presents in both spatial and temporal domains.

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

  5. 3 F( r ) =S ( r ) / (S ( r ) ) 2 6 -κ F( r ) ~ r Flatness function as an indicator of intermittency Structure Functions Inertial range 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: κ Flatness Function The intermittency index κ Scale, r

  6. 2007 NOAA 10930:sole on the solar disk

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

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

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

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

  11. 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

  12. NOAA 10930: intermittency in the photosphere and corona

  13. 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.

  14. Conclusions • The direct connection between the complex dynamics of the photosphere and corona may be suggested, and this connection requires a new kind of linking – one associated with the transfer of information between complex systems. This standpoint offers new possibilities for the photosphere / corona coupling.

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