Calculation of Intermittency in the Photosphere and Corona from Hinode Data

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

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What is the intermittency look like?
Non-intermittent Network
Intermittent Network
Spatial Domain
Temporal Domain
time
time
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Intermittency as derived from the Structure
Functions
2D x(x1,x2)
1D xt
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Flatness function as an indicator of
intermittency
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

?
The intermittency index ?
Scale, r
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NOAA 10930sole on the solar disk
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NOAA 10930intermittency in the corona
Three subsets of Hinode XRT/Be-Thin
area-integrated flux Time Series
Dec 13
Dec 11
Dec 10
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NOAA 10930intermittency in the corona
Three subsets of Hinode XRT/Be-Thin
area-integrated flux Flatness Functions
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NOAA 10930intermittency in the corona
Five subsets of Nobeyama Radioheliograph data
polarization at 9.4 GHz, Time Series
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NOAA 10930intermittency in the corona
Five subsets of Nobeyama Radioheliograph data
polarization at 9.4 GHz, Time Series
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NOAA 10930photospheric 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 8/1200 UT to 2006 Dec
13/1845 UT.
Advantages high resolution,
high time cadence,
uninterrupted measurements for several days
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NOAA 10930 intermittency in the photosphere and
corona
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Photospheric kinetic vorticity
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Photospheric kinetic vorticity
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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.