Calculation of Intermittency in the Photosphere and Corona from

Hinode DataValentina I. Abramenko

And

Vasyl B. YurchyshynBig Bear Solar Observatory of NJIT

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Non-intermittent Network Intermittent Network

What is the intermittency look like?

time time

Intermittency as derived from the Structure Functions

2D: x=(x1,x2)

ru(x)

u(x+r)

x1

x2

1D: x=t

time

u(t) u(t+τ)

τ

Flatness function as an indicator of intermittencyFlatness function as an indicator of intermittency

Fatness F( r ) is a constant for a non-intermittent variable and grows as a power lawpower law when scale r vanishes for an intermittent variable:

Inertial range

Scale, r

F( r ) ~ r-κ

F( r ) =S ( r ) / (S ( r ) )6

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The intermittency index κ

κ

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

Photospheric kinetic vorticity

Photospheric kinetic vorticity

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.