Post on 21-Dec-2015
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.