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

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Presentation transcript:

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

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

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

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

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 ) ) The intermittency index κ κ Structure Functions Flatness Function

NOAA 10930: sole on the solar disk 2007

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

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

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

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

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

NOAA 10930: intermittency in the photosphere and corona

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.

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.